Résumé 0.1 Introduction 0.1.1 La Matière Noire dans l'Univers v reherhe de wtière xoire @wxA dns l9nivers fit prtit des domines de iene ponE dmentle les plus tifs du PI ème sièleD u roisement de l hysique des rtiulesD des estroprtiules et de l gosmologieF h9une prt les mesures de vitesses rdiles des étoiles dns les qlxiesD de l dispersion des vitesses des qlxies les unes pr rpport ux utres dns les ms et utres e'ets de lentilles grvittionnelles @pigure 1A ont permit de révéler l9existene d9une mtière invisile présente en très grnde quntité utour de es ojetsD néesE sire pour pouvoir expliquer les érts oservés entre es mesures et les préditions issues de l ménique lssiqueF h9utre prt le wodèle tndrd de l gosmologieD le modèle ΛEghwD Figure I ! smge de l9ms de l flleD en fusses ouleursF v mtière visile @en rougeA montre l ollision de deux ms de qlxiesF veurs hlos de wtière xoire respetifs @en leuA sont révélés pr e'et de lentille grvittionnelle et sont délés pr rpport à l mtière visileD e qui suggère qu9ils se soient roisés sns intergir ve l mtièreD une propriété intrinsèque à l prtiule de wtière xoire reherhéeF entreprend d9expliquer e phénomène en introduisnt les fondements théorique de e onept de wx X l9nivers serit insi dominé pr des omposntes 4somres4D l wx onstitunt environ PT7 de son iln msseEénergieF rès de TW7 orrespond à l9inergie xoireD responE sle de l9élértion de l9expnsion de l9niversD non étudiée dns e trvilF in(n les S7 restnt représentent notre onnissne tuelle de l9niversD 9estEàEdire l mtière visileD omposée essentiellement des ryons mis ussi de ryonnement @photonsA et de neutrinosF ii eussiD l9intégrtion des prmètres osmologiques du modèle ΛEghw @et en prtiulier l quntité ttendue de wxA dns les simultions réentes à xEorps permettent de omprer l formtion des strutures réées spontnément dns es simultions ve les strutures de mtière visiles oservées dns l9niversF ves résultts supposent une formtion hiérrhique des strutures de wx u ÷ur desquelles l mtière ryonique est pturée grvittionnelE lementD les qlxies étnt inluses dns des hlos de wx à l9éhelle qltiqueD les ms de qlxies inlus euxEmêmes dns des hlos à plus grnde éhelleD et insi de suiteF ges résults permettent églement de ontrindre les propriétés intrinsèques de l9hypothétique prtiule de wxD dont l nture reste à l9heure tuelle l9un des plus grnds mystères de l hysique moderne Y l wx doit insi être nonEryoniqueD neutreD stleD mssiveD intergissnt fileE ment ve l mtière et omptile ve s densité relique dns l9nivers orrespondnt ux PT7 dérits préédemmentF ves sws @ekly snterting wssive rtilesA sont dns e ontexte un sénrio privilégiéD véri(nt toutes les onditions énumérées iEdessus et dont le ndidt le plus prometteur est le neutrlino χD une prtiule uniquement dé(nit dns le dre d9extensions upersymmétriques @A du wodèle tndrd de l hysique des rtiules @wAD tel que le wodèle uperymmétrique winiml @wwAF ve neutrlino est l prtiule stle l plus légère du ww et est s propre ntiprtiuleD pr onséquent son nnihiltion ve un utre neutrlino pourrit produire des prtiules du wD détetles ve les expérienes sienti(ques tuelles u sol ou dns l9espeF 0.1.2 Détection indirecte de la Matière Noire en rayons γ gette thèse se folise sur l reherhe de wx supersymmétrique sous forme de swsD dont le ndidt prometteur est le neutrlino χD et dont le dre théorique est le modèle ΛEghw de l gosmologieF sl est possile que l9nnihiltion des neutrlinos puisse produire des prtiules du wD essentiellement des pires de fermions lourds @χχ → b b, t t, τ + τ -A et des osons de guge et de riggs @χχ → ZZ, W + W -, HA, hA, ...AF ges produits primires d9nnihiltions suissent ensuite des proessus d9hdronistion ou d9émissionD produisnt insi des prtiules seondires telles que des prtiules hrgées que l9on retrouve dns les ryons osmiques @e + , e -, p, pD deutéronsAD des neutrinos et des ryons gmm @γAF ves neutrinos et ryons γ peuvent ussi être réés diretement omme produit primire d9nnihiltionF v détetion d9un exès de es prtiules dns le )ux ttriué ourmment à des proessus strophysiques stndrds permettrit de mettre en évidene l9existene de l wx et de déterminer les propriétés intrinsèques du neutrlinoD en prtiulier s msseF gette méthode de détetion indirete de l wx est u ÷ur du trvil présenté dns ette thèseD entrée sur l reherhe d9un exès de ryons γ de très hutes énergies @∼ IHH qe E IHH eA ve l9expériene rFiFFFD en provenne de régions supposées de forte densité en wx telles que le gentre qltique @gqA et les qlxies xines phéroïdes @dphsAF lusieurs signtures spetrles rtéristiques en γ permettent d9identi(er un signl de wx u milieu des di'érents ruits de fond initiés pr les ryons osmiques et les soures strophysiques stndrdD qui suivent générlement une loi de puissneF illes sont représentées sur l pigure 2F ve nl d9nnihiltion χχ → π 0 → γγ génère un spetre ontinu de γ 4seondires4 ve une oupure à l msse du neutrlino m χ F h9utre prtD les 0.1. Introduction iii nnihiltions χχ → γγ, γZ réent des ries spetrles @monohromtiquesAD dont l9énergie est égle à m χ pour l9nnihiltion en γγF gependnt le rpport d9emrnhement orrespondnt à l prodution de γ monohromtiques est réduit pr un à trois ordres de grndeur ompré à l prodution de γ seondiresF in(n des proessus d9émission fremsstrhlung internes χχ → X Xγ peuvent églement produire des pis dns les spetres de γ à une énergie prohe de m χ D mis plus étendus que les ries spetrlesF e e jour uun de es signux en γ n9 été lirement déteté et dé(nitivement ttriué à de l wxD ien que de nomreux rtiles font étt d9une potentielle détetionD priniplement dns les données de l9expériene sptile permiEveF Figure P ! ves proessus prinipux d9émission de ryons γ lors de l9nnihiltion des prtiE ules de wtière xoireD et leurs signtures spetrles respetivesF ves ries spetrles χχ → γγ seront reherhées dns l région du gentre qltique dns le dernier hpitre @0.6A hns ette thèse l wx est reherhée ve rFiFFF dns l qlxie xine du gitE tire @0.4.3AD sns hypothèse initile sur l forme spetrle du signl reherhé @des limites seront ependnt lulées pour l9émission ontinue de γAF insuite l prtie mjeure du trvil e'etué onsiste en l reherhe de ries spetrles en γ dns l région du gqD détillée en 0.6F iv 0.2 L'expérience H.E.S.S. rFiFFF @righ inergy tereosopi ystemA est un réseu de S télesopes à imgerie gherenE kov tmosphérique @segA situé en xmiieD dédié à l détetion de ryons γ de très hute énergieF ves télesopes fontionnent en stéréosopie pour reonstruire l diretion et l9énergie des ryons γ en provenne de l diretion de pointé des télesopesF ges ryons γ intergissent ve l9tmosphèreD produisent une sde de prtiules seondires @des életronsD positrons et photonsA dont les prtiules hrgées émettent de l lumière dns le prohe ultrEviolet pr e'et gherenkovF gette lumière est détetée pr les mérs des télesopes de rFiFFF onstituées de entines de photoEmultipliteursD puis onvertie en signux életriquesF v9enE registrement d9un événement est délenhé lorsqu9une imge d9intensité su0snte est oservée dns plusieurs pixels onséutifs et e dns u moins P des S télesopesF ve ruit de fond de l9expériene onsiste essentiellement en l détetion de geres hdroniques initiées pr les ryons osmiques @et produisnt églement de l lumière gherenkovAD essentiellement des protons et des noyux d9héliumD et qui tivent le système de délenhement des mérsF v pluprt de es événements sont ensuite rejetés en omprnt l forme des imges otenues dns les mérs ve des imges simuléesD les geres hdroniques produisnt générlement des imges plus étlées et désorgnisées ompré ux geres életromgnétiques initiées pr les ryons γ dont les imges gherenkov sont de forme elliptiqueF v première phse de l9expériene @rFiFFFsAD entre PHHQ et PHIPD onsistit en un premier réseu rré de R télesopes de IPm de dimètre @gIERAD ve un hmp de vue de ∼S • et un seuil en énergie d9environ IHH qeF in PHIP l mise en servie d9un inquième télesopeD le plus grnd seg dns le monde ve un dimètre de PVm @gSAD permit d9ugmenter l sensiilité de rFiFFF à sse énergieD qui entre lors dns s seonde phse @rFiFFFssAF ve seuil est à l9heure tuelle issé à ∼VH qeD et devrit tteindre ∼ SH qe prohinementF 0.3. Amélioration du logiciel de sélection de qualité des runs de H.E.S.S. v yutre l9étude des soures strophysiquesD rFiFFF est en très onne position prmi les exE périenes tuelles en γ pour déteter l wx ou pour ontrindre les modèles d9nnihiltion ssoiésD plus préisément l setion e0e d9nnihiltion des neutrlinos pondérée pr leurs vitesses reltives < σv >D en fontion de leur msse dns les divers nux d9nnihiltions présentés en 0.1.2F he plus s lolistion dns l9hémisphère ud permet l9oservtion du gentre qltique sous de files ngles zénithuxD e qui n9est ps le s des expérienes onurrentes weqsg et eritsF in prtiulierD les ontrintes produites pr rFiFFF sur l msse du neutrlino sont omplémentiresD à plus hute énergieD ve elles de l9expériene permiEveF 0.3 Amélioration du logiciel de sélection de qualité des runs de H.E.S.S.

Figure R ! v9interfe grphique du logiiel de séletion de qulité des runs de rFiFFFD risunulityD dptée pour une utilistion ve le inquième télesope gS v séletion des runs d9oservtions de rFiFFF est une étpe essentielle vnt l9nlyse des données et l prodution de résultts physiquesD et sert à limiter l9impt des éventuels prolèmes de hrdwre lors de l prise de données et des fteurs externes omme l météo et l9étt générl de l9tmosphère sur l reonstrution des ryons γ primiresF in e'et es divers prolèmes iisent les vleurs des énergies et diretions reonstruites des γ et fussent leur identi(tion ve les hdrons du ryonnement osmiqueF ve logiiel de séletion de qulité des runs utilisé dns rFiFFFD risunulityD permettit jusque là d9e'etuer vi des séletions sées sur les runs d9oservtion pris dns l première phse de l9expériene @`PHIPAD en ppliqunt des oupures sur des prmètres omme le nomre de télesopes opértionnels pendnt l prise de donnéeD l durée du runD le tux de pixels défetueux dns hque mérD ou le tux de délenhement des événements @qui dépend fortement de l qulité de l9tmosphèreAF n trvil de mise à jour de e logiiel été rélisé pendnt l thèseD dns le ut d9dpter son interfe grphiqueD ses fontionnlités et les oupures proposées pr défut à une utilistion ve rFiFFFssD 9estEàEdire ve les S télesopes du réseu opérnt ensemle depuis PHIPF he plusD gS est struturellement et tehniquement di'érent de gIER @en prtiulier l9életronique des mérs été revue et méliorée pour de meilleures perforE mnesA et requiert don des ritères de qulité indépendntsF ge trvil est onsidéré omme étnt une the de hute priorité et d9intérêt générl pour l gollortionF ves oupures préédemment dé(nies sur les prmètres de gIER ont été restreintes à es R télesopesD tndis que de nouvelles oupures indépendntes font leur pprition spéi(quement pour gSD telles que le tux de pixels défetueuxD le tux de délenhement des événementsD le temps mort @dé(nit omme étnt le temps d9oservtion totl perdu lors d9un runD dû u temps de suvegrde des informtions des événements délenhésAD et les réglges de l9eutofous @le système d9justement de l position du pln des mérs pr rpport u pln fol des miroirs des télesopesAF eussi de nouvelles oupures générles ont été joutées dns risunulityD sur le gin de l9életronique d9quisition des photoEmultipliteurs insi que sur le oe0ient de trnsprene de l9tmosphèreF in(nD des pro(les pr défut sont désormis disponiles dns l9interfe grphique du logiielD (n d9éder u plus vite à l liste des oupures stndrd sur les ritères de qulité des runs pour une on(gurtion donnée des télesopes @gIERD gIESD gS seulAF v9interfe grphique de risunulity modi(ée est représentée en pigure 4F gertines des oupures stndrd sur gIERD dé(nies dns l9nienne version du logiielD ont ussi été réjustées pour les runs d9oservtions pris à prtir de PHIP ve les S télesopesD dns lesquels une ugmenttion de S7 du temps mort des télesopes été oservée @l présene de gS dns le système de délenhement en est l useA insi qu9une ugmenttion inttendue du tux de pixels défetueux dns les mérs de gIERD de S7 églementF ves oupures orrespondntes ont été relâhées en onséquene de S7 pour éviter l9exlusion d9un trop grnd nomre de runs lors de l séletionF eu (nl sur l totlité des runs d9oservtion pris depuis tnvier PHIR ve rFiFFFssD environ PS7 sont rejetés pr les séletions stndrd ppliquées à gSD du même ordre de grndeur que e qui étit otenu ve les oupures stndrd sur gIER dns l version préédente du logiielF ges nouvelles oupures sont tuellement utilisées dns rFiFFF pour produire les listes de runs pour les nlyses de hysique en on(gurtion monosopique @gS seulAF in prtiulier les premiers résultts de rFiFFFss sont puliés dns ette on(gurtion 4wono4F h9utre prt les oupures stndrd pour les nlyses stéréosopiques @téréoAD 9estEàEdire l9pplition de ritères de qulité sur les inq télesopes de rFiFFFssD néessitent enore de futures optimistions pour éviter l9élimintion d9un trop grnd nomre de runsF 0.4. La méthode standard d'analyse ON-OFF pour la détection de sources astrophysiques et de Matière Noire vii 0.4 La méthode standard d'analyse ON-OFF pour la détection de sources astrophysiques et de Matière Noire 0.4.1 La méthode ON-OFF v méthode stndrd d9nlyse de données dns rFiFFF est sée sur l dé(nition d9une région yx dns le hmp de vue des mérsD 9estEàEdire l région soure @ou région d9nE lyseGd9intérêtAD insi qu9une ou plusieurs régions ypp générlement dé(nies dns le même hmp de vue pour estimer le ruit de fond présent dns l région yxF n délge @o'E setA est introduit entre l position de l soure étudiée et le entre des mérs pour que les vleurs de l9eptne de l9instrument dns les régions yx et ypp soient similiresF eussi l diretion ngulire de et o'set vrie d9un run d9oservtion à un utre permettnt insi d9homogénéiser les positions des régions ypp tout utour de l région yxF e el peut s9jouter l dé(nition de régions d9exlusion utour de soures strophysiques onnues @où le ruit de fond ne peut ps être estimé orretementA et utour de l région yx @pour éviter le possile déordement du signl yx dns les régions ypp en s de soure étendueAF ve prinipe de l méthode est présenté plus expliitement sur l pigure 5F représentent les positions de pointé suessives des télesopes utour de l région soure @yxA pour des runs d9oservtion di'érentsF ves régions ypp sont dé(nies utour de es positions de pointéD les onditions d9eptne de l9instrument étnt insi les mêmes pour les régions yx et ypp pour un run donnéF ve nomre totl d9événements dns les régions ypp est ensuite renormlisé et soustrit u nomre d9événements dns l région yx pour otenir l9exès de signl en γ reherhé viii v soustrtion des nomres d9événements N ON -N OF F /α permet d9éliminer en grnde prtie le ruit de fond hdronique résiduel restnt près l reonstrution des γ @voir 0.2A et d9otenir insi l9exès de signl en γ produit pr l soure étudiéeD où α est le fteur de normlistion entre les régions ypp et yxD égl u rpport de leurs surfes respetives dns l on(gurtion présentée sur l (gure 5F v signi(tivité de et exès en γ et le spetre ssoié peuvent ensuite être déterminésF 0.4.2 Analyse de sources astrophysiques HESS J1741-302 v méthode yxEypp été ppliquée sur l soure strophysique étendue et nonEidenti(ée ri tIURIEQHPF gette soure prohe du gq est située à l même position qu9un exès à ∼Sσ oservé dns les données de permiEve en PHIP et qui ser étudié dns le dernier hpitre @0.6AD d9où l9intérêt préliminire de l9étude de ette soure strophysiqueF n exès est lirement oservé à 7.9σ ve ∼IVTh de données prises ve rFiFFFsD et le spetre est justé pr une loi de puissne d9indie spetrl Γ = 2.18 ± 0.15D omptile ve les préédentes mesures e'etuées sur ette soureF eussi l présene d9une possile oupure en énergie dns le spetre uEdelà de ∼ 10T eV est reherhéeD mis n9 ps outit pr mnque de sttistique à es hutes énergiesF PKS 2155-304 v méthode yxEypp est ensuite ppliquée à l soure extrgltique pontuelle et vrile u PISSEQHRD ve les données réentes de rFiFFFss @≤ 2014AF gette soure est très étudiée en stronomie gmm et est utilisée omme référene dns rFiFFF pour optimiser et rendre ompte de l9évolution des performnes de reonstrution des γ u ours du développement des di'érentes versions du logiiel d9nlyse des donnéesD risnlysisF hns e trvil les résultts d9nlyse de l soure sont présentés de mnière omprtive pour les on(gurtions wono @gS seulA et téréo @gIESAF v9exès de γ est oservé à PRFQσ et RHFRσD respetivementD l reonstrution téréo étnt plus performnte r plus préise pour l reonstrution et l9identi(tion des γF eussi le spetre en énergie est reonstruit à prtir de UH qe @ontre ∼ IHH qe uprvnt ve rFiFFFsA et justé pr une loi de puissne Γ = 3.389 ± 0.099D omptile ve les préédents résultts puliés sur ette soureF h9utre prtD les événements mesurés dns les régions ypp utour de u PISSEQHR ont été onsidérés @l9idée fut ensuite ndonnée u pro(t d9une solution plus ppropriéeA pour modéliser le ruit de fond hdronique présent dns l région du gq pour l reherhe de lignes de wx @0.6AD le gq et u PISSEQHR étnt tous les deux oservés sous de files ngles zénithux @e `PH • A et don ve un seuil en énergie omprleF 0.4. La méthode standard d'analyse ON-OFF pour la détection de sources astrophysiques et de Matière Noire ix 0.4.3 Recherche d'un signal de Matière Noire en provenance de la Galaxie Naine du Sagittaire v méthode d9nlyse yxEypp estD (nlementD ppliquée en diretion de l qlxie xine phéroïde du gittire @grhAD une qlxie stellite de l oie vtée quiD en plus de s proximitéD est supposée ontenir une grnde quntité de wx @wsse totleGwsse visile ∼ IHAF in prtiulier grh est supposée voir orité utour de l oie vtée une dizine de fois dns son existene lors que les fores de mrée qui en résultent urient déjà du l déstruturer depuis longtempsD e qui pporte un rgument supplémentire en l fveur de l9existene de l wx dns ette régionF ves qlxies xines ne sont ps sensées émettre de ryonnement γ strophysique à très hute énergie et pr onséquent un exès de signl en provenne de es ojets pourrit être diretement orrélé ve l présene d9un hlo de wxF grh été oservée plusieurs fois pr rFiFFF entre PHHT nd PHIP sns toutefois trouver d9exès de signlD pr onséquent des limites sur l setion e0e d9nnihiltion de l wx ont été produitesF hns e trvil grh été réEnlysée ve rFiFFFsD en ppliqunt des ritères de séletion plus strits @en prtiulier des ngles zénithux `QH • et les runs omplets de PV minutes pris ve les R télesopes de rFiFFFsAF ur les THh de données séletionnées ve risunulityD un potentiel exès de signl à ∼PFTσ été oservé à l position exte de l qlxie xineD uEdessus de QHH qeF v9exès tteint Qσ en ne onsidérnt que les énergies uEdessus de SHH qe Y l rte et l distriution de l signi(tivité dns le hmp de vue de rFiFFF insi que l distriution ngulire des γ détetés et l9évolution de l signi(ne ve le temps d9oservtion sont représentés sur l pigure 6 pour ette oupure en énergie i b SHH qeF v9exès est visile dns l rte de signi(tivité et dns l distriution ngulire des événementsF eussi et exès est stle en hngent l version du logiiel d9nlyse de donnéesD et ugmente en signi(tivité lorsque l oupure en énergie ugmenteD e qui est rtéristique des soures strophysiques pontuellesF ve signl pourrit insi provenir de l wx ou plus prolement d9une soure lointine omme un xoyu etif de qlxie @eqxA situé dns l même trjetoire que grhD ou ien enore d9un vieux pulsr pprtennt à l qlxie xineF gependnt l distriution de l signi(tivité est omptile ve de pures )ututions sttistiques du ruit de fondD de même que son évolution ve le temps d9oservtion qui ne semle ps suivre une loi σ ∝ √ t omme e qui est ttendu pour un réel signlF in onlusion l9exès est pour le moment omptile ve une )utution du ruit de fond @≤ QσAF lus de données seront néessires pour pporter une onlusion dé(nitive à e sujetD e qui ser possile dns les prohines nnées ve de nouvelles oservtions de grh ve rFiFFFssF our le moment des limites sur l setion e0e d9nnihiltion de l wx moyennée sur tous les nux d9nnihiltion rént des photons seondires @spetre ontinuD voir 0.1.2A ont été lulées et puliées @qF vmnn et lD PHIQ IISA en utilisnt une hine d9nlyse lterntive ve une séletion des données moins striteD et dns lquelle uun exès n9 été oservéF v meilleure ontrinte est otenue à IEP e ve < σv >∼ 4 × 10 -23 cm 3 .s -1 F ges limites ne sont ependnt ps ompétitives ve les limites de permiEve pour les qlxies xines et ve les vleurs prédites pr les modèles de wx tels que le xwwF x Figure T ! in hut X grte et distriution de l signi(tivité dns le hmp de vue de rFiFFFsD où un exès de signl à Qσ est oservé uEdessus de SHH qeF in s à guhe X distriution ngulire des événements détetés dns le hmp de vueD les Q premiers ins orrespondnt à l région yx d9nlyse entrée sur grhF in s à droite X ivolution de l signi(tivité du signl ve le temps d9oservtion 0.5. Développement d'une méthode de Maximum de Vraisemblance Complète non-binnée pour la recherche de raies γ de Matière Noire avec H.E.S.S. xi 0.5 Développement d'une méthode de Maximum de Vraisemblance Complète non-binnée pour la recherche de raies γ de Matière Noire avec H.E.S.S.

fien que l méthode stndrd d9nlyse yxEypp présentée en 0.4.1 soit utilisée mjoritiE rement dns rFiFFF pour l9étude des soures strophysiquesD des méthodes de wximum de risemlne en provenne de l hysique des rtiules sont prfois utilisées pour l reonstrution du signlF ne méthode de wximum de risemlne nonEinnée été développée dns le dre de ette thèse et optimisée pour l reherhe de ries spetrles de wx en ryons γF gelleEi est rtérisée de 4gomplète4 r elle omine X

• une méthode 4onventionnelle4 de wximum de risemlne oissonienneD où les nomres d9événements signl @N s A et ruit de fond @N b A dns l région yx suivent une loi de oisson et sont déterminés à prtir des nomres totux d9événements estimés dns les régions yx et yppF

• une estimtion de l proilité qu9un événement donné dns l région yx soit du signl ou du ruit de fondD évluée à prtir de l9énergie de et événement en fisnt l9hypothèse de l forme des signtures spetrles ttendues pour le signl et le ruit de fondF v9expression de l funtion de wximum de risemlne gomplète est l suivnte X

L(N s , N b |N ON , N OF F , E i ) = (Ns+N b ) N ON N ON ! e -(Ns+N b ) × (αN b ) N OF F N OF F ! e -αN b × N ON i=1 η × P DF s (E i ) + (1 -η) × P DF b (E i ) @IA
où N ON et N OF F sont les nomres d9événements mesurés dns les régions yx et yppD α le fteur de normlistion entre es régionsD et E i les énergies individuelles des événements détetés dns l région yxF P DF s et P DF b sont les fontions de densité de proilité référnt ux formes spetrles ttendues pour le signl et le ruit de fondF si uun signl n9est soustrit diretement @ontrirement à l méthode yxEyppA e qui permet de onserver l totlité de l9éventuel exès dû à l wx dns l région yxF eussi l présene du seond terme dns l9expression de L permet de reonstruire des informtions dditionnelles sur les modèles de signl et ruit de fond étudiésF si les prmètres reonstruits pour l reherhe de wx sont l frtion de signl dns l région yx η = Ns Ns+N b et l9énergie de l rie monohromtique reherhéeD qui est égle ii à l msse du neutrlino m χ F ne proédure nonEinnée estD d9utre prtD mieux dptée à ette étude r les nomres d9événements et de prmètres d9justement impliqués sont su0smment petits pour ne ps voir à onsidérer de inning Y le lul de -2ln(L) est insi plus extF xii 0.5.1 Fonctions de Densité de Probabilité (PDFs) our l reherhe de ries monohromtiques de wx l forme spetrle du signl γ ttendu est une qussienne entrée à l msse du neutrlino m χ r pondérée pr l réponse de l9instrument @en prtiulier l résolution en énergieAF our le ruit de fond l forme spetrle peut être estimée à prtir de simultions wonteEgrlo @wgA ou diretement à prtir de l distriution en énergie des événements dns les régions yppF hns le ghpitre suivnt @0.6A l reherhe de ries monohromtiques se fit dns l région du gq en estimnt le ruit de fond diretement dns les régions yppD qui ontiennent à l fois une omposnte hdronique et une omposnte di'use de γ strophysiquesF gependnt dns le présent hpitre les performnes de l méthode sont évluées ve des hp purement simuléesD où les formes spetrles des omposntes hdronique et di'use suivent hune des lois de puissne d9indies respetifs PFU et PFQF ves hps sont dns les deux s des formes spetrles mesuréesD 9estEàEdire pondérées pr l réponse de l9instrumentF 0.5.2 Performances de la méthode avec les simulations Monte-Carlo ves performnes de l méthode sont évluées dns le ontexte de l reherhe de ries spetrles de wxD à prtir de données simuléesF ne région yx irulire de ryon θ = 0.25 • est dé(nieD dptée pour l9nlyse de soures étendues et su0smment lrge pour ontenir l pluprt du signl ttendu en provenne du hlo de wx de notre qlxie @en supposnt que l région yx est entrée sur le hloAF hes événements signl @wxA et ruit de fond @rdronsD émission di'useA sont simulés pour un ouple donné de vleurs des prmètres vris (η, m χ ) vrai F v proédure est testée pour des vleurs de η omprises entre S7 et SH7 et pour m χ omprise entre PSH qe et P eF ve nomre d9événements ruit de fond est rtéristique du nomre d9événements oservé dns l région du gentre qltiqueD sous de files ngles zénithux @e `PH • A et pour SHh de temps d9oservtionF v9énergie de hun de es événements signl et ruit de fond est ensuite simulée suivnt l forme de l hp orrespondnte @ii l forme de P DF b est (xéeD tndis que P DF s dépend de m χ AF our le lul de l fontion de wximum de risemlne gomplète @eqF 5.6A seuls les événements dont l9énergie est située entre PHH qe et Q e sont onsidérésD e qui donne un rs de levier en énergie su0snt pour l disrimintion entre les formes spetrles P DF s et P DF b F ves prmètres (η, m χ ) reco sont (nlement reonstruitsF v proédure est répétée SHH fois (n de lirer les erreurs de reonstrution à WS7 de degré de on(ne @gvAF eussiD les performnes de l méthode sont omprées pour les fontions de réponse de rFiFFFss en on(gurtion wono @gS seulA et téréo @les S télesopes ensemleAF v pigure 7(a) montre l distriution en énergie des événements ruit de fond simulés pour l9une des SHH reprodutions de l9expérieneD en on(gurtion rFiFFFss téréoF v hp orrespondnte est représentée en trit noir pleinF hns et exemple une rie spetrle de wx à @η = 5%, m χ = 300GeV A est simulée uEdessus du ruit de fond @l9exès est représenté en rougeAF 0.5. Développement d'une méthode de Maximum de Vraisemblance Complète non-binnée pour la recherche de raies γ de Matière Noire avec H.E.S.S. xiii

Figure U ! (a) histriution des événements wg simulés pour l9évlution des performnes de l méthode de wximum de risemlne gomplète @pour l9une des SHH reprodutions de l9expérieneAF hns et exemple une rie spetrle de wx à @η = 5%, m χ = 300GeV A est simulée uEdessus d9un ruit de fond rtéristique de l région du gentre qltiqueF v hp du ruit de fond @renormlisée pr rpport ux donnéesA est représentée en trit noir plein entre PHH qe et Q eF (b) erformnes de l méthode pour l reonstrution de m χ D

ii pour une vleur (xée de η = 5%F ves résultts pour les on(gurtions rFiFFFss wono et téréo sont omprées Résultats :

n exemple des résultts pour l reonstrution de m χ est présenté dns l pigure 7D ii pour η (xé à S7F ves résultts sont très enourgents X l méthode permet de reonstruire des ries spetrles de wx pour des frtions de signl b S7 et des msses b PSH qe ve des erreurs de moins de QH7 @wono et téréoA sur l reonstrution de η et de moins de PH7 @wonoA et IH7 @téréoA sur l reonstrutions de m χ D à WS7 gvF ges erreurs deviennent inférieures à quelques 7 ve des vleurs simulées η > 10% et m χ > 250GeV F v reonstrution téréo donne des résultts plus préis grâe à une meilleure résolution en énergie qui permet insi de distinguer plus filement une rie spetrle du ruit de fondF eussi l plus petite frtion de signl η qu9il est possile de reonstruire été évluée à IFS7 @wonoA et IFQ7 @téréoA pour une msse de QHH qeD et à HFQ7 à P e pour les deux on(gurtionsF gel orrespond à des )ux de γ de 1 -2 * 10 -4 γ.m -2 .s -1 et 1 -4 * 10 -5 γ.m -2 .s -1 à QHH qe et à P eD respetivementF xiv 0.6 Recherche de raies spectrales de Matière Noire au Centre Galactique avec H.E.S.S.II 0.6.1 L'excès de signal à 130 GeV observé dans les données de Fermi-LAT n exès de signl orrespondnt à une rie spetrle à IQH qe été oservé dns les données de permiEve en PHIP dns l région du gqD ve une signi(tivité de 3.2σ ITP et en fisnt l9hypothèse 4lssique4 d9un hlo de wx oinident ve le gqF v setion e0e d9nnihiltion de l wx néessire pour réer e signl est évluée à < σv >= (1.27 ± 0.32 +0.18 -0.28 ) × 10 -27 cm 3 .s -1 pour un pro(le de densité de wx de type 4iinsto4F h9utre prtD l signi(tivité de e signl tteint le seuil de détetion à 5σ @sns prendre en ompte les fteurs de 4trils4 ependntA en onsidérnt un hlo de wx délé en longitude de EIFS • pr rpport u gq ISQD e qui orrespond à un délge d9environ PHH pF gette éventulité n9est ps prévue pr les modèles tuels de formtion des strutures et reste don un mystèreF e l9heure d9ujourd9huiD e signl à IQH qe disprît peu à peu des données en ugmentnt l sttistiqueD et serit don ttriué à une somme de )ututions sttistiques et systémE tiquesF rFiFFFss est à e jour l seule expériene en gmm ple de véri(er e résulttD et de on(rmer ou exlure dé(nitivement e signl à IQH qeF our el l9utilistion du inE quième télesope @gSA est essentielle r le seuil en énergie qui en résulte @∼ VH qeA est su0smment s pour prétendre oserver et exès de signl potentiel dns les donnéesF 0.6.2 Prise de données hes données dédiées à ette étude ont été prises u rintemps PHIRD les télesopes de rFiFFFss pointnt à une dizine de positions di'érentes le long du ln qltique X -2.3 • < l < 0.5 • @ve un ps de 0.7 • A et b = ±0.8 • F n minimum de R télesopes fontionnels lors l prise de données été requis @inlunt gSA (n d9ssurer l meilleure reonstrution possile pour les ryons γ détetésD insi que des ngles zénithux `PH • pour isser le seuil en énergie à environ ∼ VH qeF ves données ne stisfisnt ps les ritères de qulité stndrds tels que dé(nis dns risunulity @voir 0.3A sont rejetésF ur les données restntesD environ PHh u totl permettent une nlyse à l position du mxiE mum du signl de wx tel que dé(nit dns les données de fermiEve X @l = -1.5 • , b = 0 • AF ur es PHh de données seulement PFVh orrespondnt à evril PHIR @ériode RA ont pour l9instnt été nlysées (n de tester l proédure d9nlyse et véri(er que rFiFFFss est sensile à l détetion du signl à IQH qe reherhéF 0.6.3 Stratégie d'analyse v méthode de wximum de risemlne gomplète présentée en 0.5 est ppliquée pour l reherhe de ries spetrles de wx dns l région du gqD sur le lot de données R prises en PHIRF v on(gurtion téréo est hoisie pour l reonstrution des événements γ r elle présente une plus grnde sensiilité pour l reherhe de ries spetrles tout en onservnt un seuil en énergie su0smment s pour permettre une étude à IQH qeF v région yx est entrée à l position où l signi(tivité du signl oservé dns les données de permiEve est 0.6. Recherche de raies spectrales de Matière Noire au Centre Galactique avec H.E.S.S.II xv l plus grnde @l = -1.5 • , b = 0 • AF v tille de l région yx est optimisée ve des simultions wg pour une rie à IQH qeD en supposnt un hlo de wx de type iinsto entré sur ette région d9nlyse et une vleur de < σv > orrespondnt u signl oservé dns les données de permiEveF in étudint l signi(tivité du signl reonstruit en fontion du ryon de l région yx et en tennt ompte des limittions tehniques dues à l dimension du hmp de vue et à l9eptne rdileD un ryon optiml de θ ON = 0.4 • est otenu pour l région d9nlyseF hns ette étudeD l reherhe de ries spetrles de wx ne se limite ependnt ps à l seule msse de IQH qe Y un exès de signl est églement reherhé de mnière plus générle dns l région d9nlyseD pour des msses llnt de IHH qe à P eF v fontion de densité de proilité du signl @P DF s A est déterminée pour hque msse onsidérée à prtir de simultions wgD omme en 0.5.1F gependnt l fontion de densité de proilité du ruit de fond @P DF b A est ii diretement justée sur les données issues des régions yppD dé(nies dns le même hmp de vue tout utour de l région d9nlyse @voir 0.4.1AD et e en exlunt les soures strophysiques onnuesF ille est représentée sur l pigure 8@AF P DF b est insi supposé représenter (dèlement le ruit de fond présent dns l région yxD les omposntes de fond hdronique et d9émission di'use strophysique présente dns le ln qltique étnt prises en ompte toutes les deuxF ves erreurs systémtiques de l méthode ont été évluées pour l reonstrution de η Y elles inluent les inertitudes sur l prmétristion de l P DF b @soure d9inertitudes dominnte à sse énergieAD sur l omposnte d9émission di'use inluse dns le ruit de fondD insi que sur les fontions de réponse de rFiFFFss @téréoAF Figure V ! @A pontion de densité de proilité pour le ruit de fond @P DF b AD représentée en trit noir pleinD justée à prtir des événements issus des régions ypp dns les données RF v P DF s orrespondnt à une rie spetrle à SHH qe est représentée en rouge à titre inditifF @A wéthode de lul de l limite supérieure sur η à WS7 gvD en s de nonEexès oservé dns les données xvi 0.6.4 Analyse préliminaire avec la méthode ON-OFF hns un premiers temps l méthode stndrd d9nlyse yxEyppD dérite en 0.4.1D est ppliE quée u lot de données R (n de mettre en évidene l9existene d9un exès de signl dns l région yxF i tel est le s l méthode de wximum de risemlne v permettre de rtériser et exèsD en prtiulier l msse m χ orrespondnte dns le s d9une rie speE trle de wxF v (gure 9 montre le résultt de ette nlyse stndrdF euun exès de signl n9est oservé dns les données R @σ = 0.6AD dns l région d9nlyseF v9exès oservé dns les rtes et dns l distriution de l signi(tivité orrespond l9émission strophysique en provenne du gqF Figure W ! ésultts de l9nlyse stndrd yxEypp ppliquée u lot de données RF in hut X rtes d9exès et de signi(tivité dns le hmp de vueD et distriution des vleurs de l signi(tivitéF in s X distriution ngulire des événements reonstruits dns le hmp de vueF ve niveu de ruit de fond est indiquéF euun signl n9est déteté en provenne de l région yx d9nlyse 0.6. Recherche de raies spectrales de Matière Noire au Centre Galactique avec H.E.S.S.II xvii 0.6.5 Calcul des limites sur le ux et la section ecace d'annihilation de la MN avec la méthode de Maximum de Vraisemblance Complète euun signl n9ynt été oservé dns l région d9nlyse @l = -1.5 • , b = 0 • AD des limites sur le )ux et sur l setion e0e d9nnihiltion de l wx dns le nl χχ → γγ sont luléesD à WS7 gvF our elD une limite supérieure sur l vleur reonstruite de η est lulée pour hque msse m χ D à prtir de l fontion de wximum de risemlne gomplète en proédnt omme indiqué sur l pigure 8@AF heux domines en énergies distints sont dé(nis pour le lul de l fontion de wximum de risemlneD à svoir VH qe Y I e et PHH qe Y Q eD dptés pour l reherhe de ries spetrles entre IHH qe et SHH qe et entre SHH qe et P eD respetivementF gei permet d9ssurer un rs de levier en énergie su0snt dns hun des s pour l disrimintion entre les formes spetrles P DF s et P DF b F e prtir de η 95%CL une limite supérieure sur le nomre d9exès de γ détetés est ensuite déterminée X N 95%CL γ = N b × η 95%CL 1-η 95%CL où N b est estimé à prtir des régions yppF e prtir de N 95%CL γ les limites sur le )ux de gmm Φ 95%CL et sur l setion e0e d9nnihiltion < σv > 95%CL χχ→γγ sont en(n luléesD suivnt les expressions X

Φ 95%CL = N 95%CL γ T OBS × Emax E min dN dEγ (E γ )dE γ Emax E min A ef f (E γ ) dN dEγ (E γ )dE γ , < σv > 95%CL = 8πm 2 χ 2Φ astro × Φ 95%CL @PA
où T OBS est le temps d9oservtionD A ef f l surfe e'etive de rFiFFF pour l détetion des γD dN dE (E γ ) = 2δ(E γ -m χ ) est le spetre di'érentiel des γ monohromtiquesD et Φ astro est le fteur strophysiqueD relié à l densité de wx intégrée dns l région d9nlyse et le long de l ligne de viséeF our un pro(le de densité de type iinsto le fteur strophysique est ii évlué à Φ astro = 2.46 × 10 21 GeV 2 .cm -5 F eussi le hlo de wx est supposé s9étendre uEdelà de l région yxD pr onséquent une frtion du signl de wx est inluse dns les régions yppD à un niveu estimé à ∼PS7 du signl présent dns l région yxF ves limites lulées tiennent ompte de et e'etF 0.6.6 Résultats ves limites sur les données R @PFVhA sont représentées sur l pigure 10 @points de données violetsA en omprison ve les résultts préédemment puliés en PHIQ ve rFiFFFs @IIPhA et permiEve @QFU nsAD ien que es études ient été rélisées en onsidérnt un hlo de wx oïnident ve le gqF ves résultts sont églement omprés ve les limites issues de lots de données simulées et lirées sur SHH expérienesD pour hque msseF v médine des vleurs reonstruites de N 95%CL γ sur es SHH simultions est prise omme limite liréeD à prtir de lquelle Φ 95%CL et < σv > 95%CL sont lulés Y ii seuls des événements ruit de fond ont été simulés @η = 0AD pour un temps d9oservtion de PHhD et dont leur distriution en énergie suit l forme de l hp déterminée dns les données ypp de RF ves erreurs systémtiques sur es limites wgD dues ux inertitudes sur l prmétristion de P DF b @systémtique dominnte à sse énergieAD sont représentées pr un trit leu en pointilléF e titre omprtifD les limites wg @PHhA sont églement renormlisées à un temps xviii d9oservtion de PFVh @trit plein violetA et IHHh @trit plein juneAF in(nD le point de donnée en vert représente l vleur de < σv > orrespondnt u signl oservé à IQH qe dns les données de permiEve @PHIPAD ve ses rres d9erreur @sttistiqueCsystémtiqueA Scan complet en masse : ves résultts sur les données R montrent une très onne omptiilité ve les limites issues des simultions wgF ve domine en énergie ouvert pr es mesures omplète e0ement les préédents résultts puliés en PHIQ ve rFiFFFs TI et permiEve IHF eve un lot de données plus onséquentD en prtiulier en nlysnt le totl de PHh de données disponilesD les limites lulées seront ompétitives ve les limites les plus ontrignntes à l9heure tuelle sur les modèles d9émission de ries spetrles en γ dns le domine d9énergie ouvert pr rFiFFF Contraintes à 130 GeV : e IQH qe les limites sur le )ux et sur < σv > déterE minées ve les données R sont les suivntes X

Φ 95%CL (130GeV ) = 9.95 × 10 -4 γ.m -2 .s -1 .sr -1 < σv > 95%CL (130GeV) = 1.64 × 10 -27 cm 3 .s -1
v limite < σv > est un fteur ∼ IFQ uEdessus de l vleur orrespondnt u signl oservé dns les données de permiEve en PHIP @1.27 × 10 -27 cm 3 .s -1 AF v9nlyse du lot de donnée omplet est don là ussi néessire et devrit permettre d9exlure e signl à plus de WS7 gvD inlunt les erreurs systémtiques sur l hp du ruit de fondF 0.6.7 Perspectives v9nlyse du lot de données omplet @∼ PHhA ve l méthode de wximum de risemlne gomplète est prévue en eptemre PHISF lus de IHHh de données sont églement disponiles ve rFiFFFss pour une nlyse u gentre qltique @l = 0 • , b = 0 • AD à l mnière de e qui été fit dns les préédents ppiersF in(nD dns un future plus lointinD l reherhe de wx entrer dns une nouvelle ère grâe u réseu de télesopes geD dont l sensiilité permettr sns doute de lever le voile sur l nture de l wtière xoireF Figure IH ! vimites à WS7 gv sur l setion e0e d9nnihiltion de l wx dns le nl χχ → γγF oints de données violets X limites lulées à prtir des données nlysées R @PFVhAF in leu X limites lulées à prtir des simultions wgD pour un temps d9oservtion de PHhF ves erreurs systémtiques sur l prmétristion de l P DF b sont représentées ve un trit leu en pointilléF rits pleins violet et june X limites wg renormlisées à PFVh et IHHh de temps d9oservtionD respetivementF ves limites R et wg sont omprées ux préédents résultts puliés en PHIQ ve rFiFFFs @en rougeA et permiEve @en noirA pour l reherhe de ries spetrles u gentre qltiqueF in(nD l vleur de < σv > orrespondnt u signl oservé à IQH qe dns les données de permiEve @PHIPA est représentée en vertD ve ses rres d9erreur @sttistiqueCsystémtiqueA

F F F F F F F F F F F F F F F F F F F F F F F F F F F P IFIFI ividene for osmologil hrk wtter F F F F F F F F F F F F F F F F F F P IFIFP prmework X ΛEghw nd sw F F F F F F F F F F F F F F F F F F F F F U IFIFQ rtile ndidtes for sw hrk wtter F F F F F F F F F F F F F F F W IFP owrds indiret detetion of the hrk wtter in γErys F F F F F F F F F F F F IP IFPFI Q omplementry detetion pprohes F F F F F F F F F F F F F F F F F F IP IFPFP γEry )ux from hrk wtter hlos F F F F F F F F F F F F F F F F F F F F IV IFPFQ hrk wtter oservtionl trgets nd reent results with γEry oserE vtories F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F PQ IFQ gonlusions F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F PS
F F F F F F F F F F F F F F F F F PV PFP he rFiFFF telesope rry F F F F F F F F F F F F F F F F F F F F F F F F F F F F QR PFPFI gmers F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F QS PFPFP rigger system F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F QU PFPFQ glirtion F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F QW PFPFR eutofous system F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F RT PFPFS eonstrution of the γEry events F F F F F F F F F F F F F F F F F F F F RV PFQ gonlusions F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F SS
F F F F F F F F F F F F F F F F F F SU QFP he risunulity softwre F F F F F F F F F F F F F F F F F F F F F F F F F F F SV QFQ tndrd run seletion with rFiFFFs F F F F F F F F F F F F F F F F F F F F F F TH QFR edpting risunulity to rFiFFFss nlyses F F F F F F F F F F F F F F F F TR QFRFI truture nd modi(tion of the ode F F F F F F F F F F F F F F F F F F TR QFRFP elesope seletion E gS F F F F F F F F F F F F F F F F F F F F F F F F F TT QFRFQ gS trigger seletion F F F F F F F F F F F F F F F F F F F F F F F F F F F F TU QFRFR gS roken pixel seletion F F F F F F F F F F F F F F F F F F F F F F F F F TV QFRFS gS utofous seletion F F F F F F F F F F F F F F F F F F F F F F F F F F TV QFRFT glirtion E qin seletion F F F F F F F F F F F F F F F F F F F F F F F F TW QFRFU etmosphere E rnspreny oe0ient F F F F F F F F F F F F F F F F F F UH QFRFV smplementtion of seletion pro(les in risunulity F F F F F F F F UQ QFRFW vog(le E vist of rejeted runs F F F F F F F F F F F F F F F F F F F F F F F UQ QFRFIH ummry tle 8 hisussion F F F F F F F F F F F F F F F F F F F F F F F UT QFS gonlusions F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F UW xxii
RFI tndrd yxEypp nlysis F F F F F F F F F F F F F F F F F F F F F F F F F F F F VP RFIFI riniple F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F VP RFIFP ole mode F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F VQ RFIFQ yxGypp pirs from di'erent (elds of view F F F F F F F F F F F F F F F VU RFIFR igni(ne of the signl F F F F F F F F F F F F F F F F F F F F F F F F F F VV RFP enlysis of strophysil soures F F F F F F F F F F F F F F F F F F F F F F F F F VW RFPFI petrl nlysis in rFiFFF F F F F F F F F F F F F F F F F F F F F F F F F VW RFPFP enlysis of ri tIURIEQHP F F F F F F F F F F F F F F F F F F F F F F F F WI RFPFQ enlysis of u PISSEQHR F F F F F F F F F F F F F F F F F F F F F F F F F WU RFQ ixmple of
F F F F F F F F IHQ RFQFP hwrf pheroidl qlxies F F F F F F F F F F F F F F F F F F F F F F F F F IHQ RFQFQ he gittrius hwrf qlxy F F F F F F F F F F F F F F F F F F F F F F F IHU RFQFR ht qulityD run seletion nd uts F F F F F F F F F F F F F F F F F F F IHW RFQFS tndrd yxEypp nlysis results F F F F F F F F F F F F F F F F F F F F III RFQFT vimits on potentil hw gontinuous signls F F F F F F F F F F F F F F F IIR RFR gonlusions F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IIU
F F F F F F F F F F F F F F F F F F F F F F F F F IPH SFIFI riniple F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IPH SFIFP finned wximum vikelihood F F F F F F F F F F F F F F F F F F F F F F F IPH
SFIFQ wodi(ed oisson wximum vikelihood with yx nd ypp regions @olkeAIPI SFIFR finned oisson wximum vikelihood with energy sideEnds

F F F F F IPI SFIFS nEinned wximum vikelihood F F F F F F F F F F F F F F F F F F F F F IPP SFIFT owrds n extended unEinned 4pull4 vikelihood method for hrk wtter serhes F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IPP SFP pull vikelihood method F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IPQ SFPFI qenerl desription of the method F F F F F F F F F F F F F F F F F F F F IPR SFPFP hevelopment of the method F F F F F F F F F F F F F F F F F F F F F F F F IPU SFPFQ ttistil estimtors F F F F F F F F F F F F F F F F F F F F F F F F F F F F IRH SFPFR erformnes of the method with wonteEgrlo simultions F F F F F F F IRS SFQ gonlusions F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F ISS
TFI sntrodution F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F ISV TFIFI riEs nd permi vine serh results F F F F F F F F F F F F F F F F F F ISV TFIFP IQH qe vine spetrl feture oserved in permiEve dt E permi rotspot F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F ISW TFIFQ qenerl strtegy with rFiFFFss F F F F F F F F F F F F F F F F F F F F F ITI
F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F ITQ TFP FyFsF optimiztion F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F ITT TFQ gontriution of nery soure ri tIURIEQHP F F F F F F F F F F F F F F F F F IUI TFR gontriution of nery soure ri tIURSEQHQ F F F F F F F F F F F F F F F F F IUP TFS vine sn ht mple F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IUQ TFSFI yservtions of the vine n F F F F F F F F F F F F F F F F F F F F F F F IUQ TFSFP ht qulity nd run seletion F F F F F F F F F F F F F F F F F F F F F F IUS TFSFQ nElinding of the vine n R dtset F F F F F F F F F F F F F F F F F IUW TFSFR tndrd nlysis of the vine R dt F F F F F F F F F F F F F F F F F F IVH TFT inergy rnge for the pull vikelihood (t F F F F F F F F F F F F F F F F F F F F F F IVR TFU ghoie of rFiFFFss reonstrution X wono G tereo F F F F F F F F F F F F F F F IVT TFV roility hensity puntions F F F F F F F F F F F F F F F F F F F F F F F F F F F IVV TFVFI vine signl FhFpF F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IVV TFVFP fkground FhFpF F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IVW TFW hw signl lekge in the ypp regions F F F F F F F F F F F F F F F F F F F F F F IWU TFIH ystemtis F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F IWV TFIHFI ystemtis on the sFFpFs F F F F F F F F F F F F F F F F F F F F F F F F F IWV TFIHFP ystemtis on the kground hp (t F F F F F F F F F F F F F F F F F IWV TFIHFQ ystemtis on the di'use emission omponent F F F F F F F F F F F F F IWW TFIHFR ummry on the systemtis F F F F F F F F F F F F F F F F F F F F F F F PHH TFII pdte E xew softwre version relese @vFQHA F F F F F F F F F F F F F F F F F F F
F F F F F F F F F F F F F F F PPI TFIR gonlusions F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F F PPP Conclusion 223
Bibliographie 227

Preface " he serh for the hrk wtter in the oservle niverse onstitutes one of the mjor sienti( hllenges of the PI st enturyD whih ene(ts from extensive nd omplementry ontriutions in the (elds of rtile hysisD estroprtile hysis nd gosmologyF he existene of the hrk wtter ws (rst limed in IWQQ in the study of the gom qlxy glusterD loted t out ∼IHH wegprses from usD sine the mount of visile mtter ws not su0ient to explin the mesured veloity dispersion of its qlxy onstituentsF prom now its existene nd dominne hs een lrgely demonstrted through its grvittionl in)uene on mny more visile ojets t the strophysil nd osmologil slesD nd nturlly enters s omponent into the tndrd wodel of gosmology whih infers the glol rhiteture of the hrk wtter in the niverseF roweverD its deep nture in terms of prtile elements is still elusive nd tully relies on theories eyond the tndrd wodel of rtile hysisF sn n ttempt to solve this puzzleD some of the most relevnt theoretil models sugE gest tht the hrk wtter prtiles my selfEnnihilte nd produe seondry prtile messengers suh s eletronsGpositronsD protonsGntiprotonsD neutrinos nd gmmErysD trvelling down to the irth nd detetle with modern spe nd groundEsed oservE toriesF he oservtion of hrteristi spetrl signtures ove the stndrd kground )uxes of these messengersD suh s γEry ontinuum with energy utEo' or monohromti lineD would provide ompelling indiret evidene of the existene of the hrk wtter with further indition on its intrinsi prtile propertiesF he work presented in this thesis is uilt on this indiret detetion frmeworkD where the hrk wtter prtiles ould e deteted in gmmErys in the IHH qe E IHH e energy rnge with the rFiFFF experimentD groundEsed smging etmospheri gherenkov elesope @segA rry loted in the xmiin desertF he struture of this work is sudivided into T hpters X

• Chapter 1 gives generl introdution out the onept of hrk wtterD its oE servtionl evidene nd its possile interprettion in terms of prtile ndidteD s well s urrent detetion methods with modern spe nd groundEsed oservtoriesF sn prtiulr the indiret detetion of the hrk wtter in γErys will e disussed in detilsF

• Chapter 2 desries the priniple of γEry detetion with smging etmospheri gherenkov elesopesD nd then fouses on the tehnil properties of the righ inergy tereosopi ystem @rFiFFFAD the γEry instrument used in the frme of this thesis workF xxvi

Table des matières

• Chapter 3 onerns the hievement of high priority tsk for the rFiFFF gollE ortion X the upgrde of the run qulity seletion softwre tht is used efore proeeding to physis nlyzesD nd whih needed to e dpted for proper working with the new ig gherenkov telesope dded t the entre of the rFiFFF rry in PHIPF

• Chapter 4 introdues the stndrd yxEypp nlysis method ommonly used in rFiFFF in the study of strophysil souresF his method is pplied to ri tIURIEQHPD n extended soure lose to the qlti gentreD nd then to u PISSEQHRD right extrglti lirtion soure in rFiFFF he lst setion of the hpter is dedited to the use of this yxEypp method for hrk wtter serhesD with the serh for potentil exess signl in the gittrius hwrf qlxyF

• Chapter 5 presents the development of new unEinned pull vikelihood method designed for hrk wtter serhesD nd optimized in the ontext of monohromti γEry line detetionF he performnes of the method for the reonstrution of hrk wtter signl over the strophysil nd osmiEry kgrounds re evluted over wide rnge of msses etween PSH qe nd P eD nd for signl frtions down to S7 of the totl numer of mesured eventsF

• Chapter 6 orresponds to the lrgest prt of the work presented in this thesis X the serh for hrk wtter γEry line signl in the qlti gentre regionD with rFiFFF dt tken in PHIRD nd using the pull vikelihood method presented in ghpter 5F rere n dditionl omplexity is dded in onsidering the energy region elow PHH qeD lose to the threshold of the instrumentF e omplete optimiztion of the method is done for proper estimtion of the strophysil nd osmiEry kground omponentsD together with systemtis studiesF his ends up with the hievement of ompetitive limits on the nnihiltion rossEsetion of the hrk wtter prtiles for msses down to IHH qeD nd with the disussion on the exlusion of potentil hrk wtter lineElike signl reported in the permiEve telesope dt in PHIP he ltest results from the vrge rdron gollider @vrgA provided very strong veri(tion of the tndrd wodel of rtile hysis @wAF sn prtiulr the disovery of the riggs oson ompleted the detetion of ll of the predited w prtilesD while no experimentl result hs een widely epted s de(nitively ontrditing the tndrd wodel t the Sσ levelF yn the other hndD studies t the osmologil sle nd in prtiulr the reent results from the lnk stelliteD re in entire greement with the tndrd wodel of gosmologyD the ΛEghw wodelF lnk hs one more on(rmed the existene of dominnt 4hrk4 omponents in the mssEenergy udget of the niverseD not ssoited with ryoni mtterD tht e0iently onnet theory preditions with oservtionl evideneF hrk inergy represents out TW7 of this mssEenergy udget nd hs een proposed in the ΛEghw wodel s n explntion for the oserved elertion of the expnsion of the niverseD while hrk wtter @hwA ounts for PT7 nd is fully onsistent with struture formtion nd with severl oservtionl results t the glti nd osmologil slesD where hidden mss is required for onsistent interprettionsF rowever the deep nture of the hw remins unknownD the presently fvoured senrio eing goldD wssive nd ekly snterting rtiles @swsA not provided within the wD thus needing its extension @eFgF modelsAF his urrently onstitutes one of the mjor puzzles in pundmentl hysisF his hpter gives n overview of the hw properties within the tndrd wodel of gosmology @ΛEghwA @1.1A nd then fouses on the priniple of the detetion of the hw prtiles with modern γEry oservtories suh s rFiFFF @1.2A he (rst ever oservtionl hint for the existene of hidden mss in the niverse me from the erly PH th entury with works of Öpik @IWPPA IQR nd yort @IWQPA IQQ who reported tht luminous mtter in glxies @endromed nd the wilky yD respetivelyA ws not sufE (ient to explin their dynmisF rowever pF wiky @IWQQA hs een the (rst one to propose the existene of non visile mss s onsistent explntionD thus introduing the onept of hwF ris works priniplly foused on the dynmis of individul glxies in the gom glusterD where he onluded tht their rdil veloities were too lrge to mke them hold on grvittionlly in the luster systemD unless n invisile omponent ensured the system stility ITVF elmost gentury lter oservtionl evidene of the hw hs een reported in mny experiE ments ll over the world nd t di'erent physis slesD relying on the study of the dynmis of qlxies nd qlxy glustersD qrvittionl lensingD s well s onstrints from osmologil models nd their oservtionl veri(tionsF 1.1.1.1 Dynamical constraints on Galaxies and Galaxy Clusters he mesurement of the irulr veloities of strs in nery qlxiesD lled rottion urvesD provide ompelling evidene for the hw existeneF he expression of the irulr veloity of str oriting qlxy is given y the formul X

v(r) = GM (r) r @IFIA
where G is the grvittionl onstnt nd M (r) = r 0 ρ( r)d 3 r is the mss ontined in spheril volume entred t the grvittionl entre of the glxy of rdius rF feyond the entrl luminous hlo of the qlxy the rdil veloity is expeted to derese s ∝ 1/ √ rD however mesurements show tht this veloity eomes onstnt t lrge distnesF e striking exmple is shown in pigure 1.1 with the qlxy xqg TSHQ @QSD IWWIAF his ehviour is not omptile with lssil xewtonin mehnis nd therefore implies the presene of ertin mount of nonEluminous mtter eyond the visile extension of the qlxyF e hw hlo with rdil pro(le s ∝ 1/r 2 nd whih ontins the qlxy is suitle nd likely explntion for the str motionF imilr onlusions were rehed in more reent studies @RUD PHHIAF his lso pplies t lrger sles with the study of the qlxy glustersF he mss of the qlxy glusters n e otined from the distriution of the rdil veloities of their qlxy omponentsD y the pplition of the iril heorem QIIHRSPF his method led to the (rst evidene of the existene of the hw y pF wiky in IWQQ ITVF sn these ses the required mount of hw for eing onsistent with lssil mehnis is muh lrger thn the mount of luminous mtter nd hot gs in the lusterF e wy of mesuring the hw exess is the mssEtoElight rtio @wGvAF sn qlxies this rtio is usully of the order of IHD while t the qlxy gluster sle M/L ∼ IHHF fut the most promising hw trgets re hwrf pheroidl qlxies @dphA tht re the most hw dominted systems known so frD with wGv rtios up to severl thousndsF he se of dphs will e further studied in ghpter 4 @4.3AF 1.1.1.2 Gravitational lensing eording to iinstein9s theory of the qenerl eltivityD light is de)eted y the grvittionl (elds generted y mss onentrtionsF e photon emitted y n strophysil soure nd trvelling through spe down to the oserver9s eye will e de)eted y mssive ojets @visile of notA loted ll long its wy nd will provide distorted imge of the soure in the telesopesF his e'et is lled grvittionl lensingF he mss of invisile ojets n therefore e inferred from the study of these distorted imgesF yne of the most remrkle exmple is the fullet gluster SVRVD shown in pigure 1.2F sts ryoni distriution in Erys nd its grvittionl mss hve een mpped y grvittionl lensingD nd show two lerly distint mssive sustrutures @in lue on the (gureA o'set with respet to the luminous mtter @in redAF his result suggests the presene of two merging qlxy glustersD with their respetive hw hlos pssing through eh other s result of grvittion onlyF yn the other hnd the ryoni mtter hs een slowed down y eletromgneti intertionsD thus eing ompelling evidene tht the hw is ollisionlessF e omplete review of hw serhes y grvittionl lensing is presented y wssey et lF @IPPD PHIHAF o dte grvittionl lensing e'ets hve een oserved in more thn IHH qlxy glustersF Figure IFP ! smge of the fullet glusterD in fke oloursF he luminous @ryoniA mtter from two interting qlxy glusters is shown in red while their respetive hw hlos re represented in lueD reveled y grvittionl lensingF gredit X xee 1.1.1.3 The Λ-CDM cosmological model he previous oservtionl results imply the existene of the hw s dominnt omponent in qlxies nd in qlxy glustersF his senrio hs een pprohed y osmologil modelsD tht should predit the right mount nd the sptil distriution of the hw in the niverseF he most prominent model so fr tht (lls ll of the requirements is the tndrd wodel of gosmologyD lled ΛEgold hrk wtter wodel @ΛEghwA where Λ is the osmologil onstnt @iFeF the hrk inergy omponentAF he fig fng heory is lso one of its most importnt pillrsF sn the ΛEghw wodel the niverse is onsidered s homogeneous nd isotropiF sn tht frme the iinstein9s eqution of qenerl eltivity redues to priedmn equtions tht desrie the evolution of the niverse through the osmi sle ftor a(t) nd the totl mssEenergy density ρ tot suh tht X

ρ tot = ρ r + ρ m + ρ Λ @IFPA
where ρ r D ρ m nd ρ Λ re the density of rdition @photons nd neutrinosAD the density of nonE reltivisti mtter @ryoni C hw iFeF ρ b + ρ DM A nd the density of osmologil ontntD respetivelyF sn se of )t niverse @k = 0AD urrently fvoured y the ltest lnk stellite mesurements TTD the totl density ρ tot is equl to the ritil density ρ c = 3H 2 0 /8πG where H 0 nd G re the rule nd the grvittionl onstntsD respetivelyF he di'erent density omponents re then written s frtion of ρ c nd re lled density prmeters

Ω i suh tht X Ω tot = ρ tot /ρ c = Ω r + Ω m + Ω Λ = 1 -Ω k @IFQA
where Ω k is the urvture density ontriutionF his nottion will e used in the following prgrphs nd setionsF he vlues of the di'erent ΛEghw density prmeters n e otined through mny types of osmologil mesurementsD ll eing omplementryF sn prtiulr the hw density

Ω DM nturlly derives from Ω m nd Ω b F
• The Cosmic Microwave Background (CMB) : Ω m n e derived from the mesuE rement of nisotropies in the gwf tht ws emitted in the erly niverse @∼ 4 × 10 5 yers fter the fig fngAD nd from whih the results re in good greement with )t niverse @k = 0A nd with the existene of nonEryoni mtterF he rdition density Ω r is lso inferred from these mesurementsF

• Type-1a supervovae : hese re thermonuler explosions of hite hwrves reting mtter from inry ompnion strF he typeEI supernove re onsidered s stndrd ndles of the niverseD s they hve preditle solute luminosities due to the uniformity of the msses of hite hwrvesF he mesurement of their pprent luminosities nd redshifts gives indiret evidene of the elertion of the expnsion of the niverse thus implying non zero vlue for Ω Λ F st lso llows ontrining the rnge of the prmeters @Ω m , Ω Λ AF

• Baryonic Acoustic Oscillations (BAO) : he temperture ngulr power spetrum @or nisotropy spetrumA of the gwf shows the preise mesurement of ousti peksD well (tted y the ΛEghw wodel TTF hey orrespond to ousti wves generted in the reltivisti plsm of the primordil niverseD tht ould hve 'eted the density nd distriution of the ryonsF his leds to the mesurement of Ω b F hen omining the onstrints from gwfD typeEI supernove nd fey mesureE ments in the @Ω m , Ω b A PhEspe the vlues of these osmologil prmeters n e inferred with high preisionF pigure 1.3 shows the omintion of these mesurements done in PHHV @uowlski et lF IIPAF he ltest PHIS lnk onstrints t TV7 gv re represented in red on top of the (gure TTD showing the gret improvement in the preision of the mesurement over the yersF he vlues of some of the relevnt osmologil prmeters determined y lnk nd pulished in heemer PHIS re summrized in pigure 1.4F sn prtiulr the hw ounts for Ω DM = 0.2589 ± 0.0022 iFeF lmost PT7 of the totl mssEenergy of the niverseD while out TW7 for the hrk inergy nd only S7 for the ryoni mtterF hotons nd neutrinos ontriute with Ω r < 0.1%F hese results on(rm the dominne of the hrk omponents in the niverseF qiven the lrge frtion of the hw in the mssEenergy udget of the niverseD the hw omponent plys dominnt role in strutures formtionF gwf mesurements hve shown tht the mplitude of the )ututions of the ryoni density @in 7A ws t the level of 10 -5 t the time of the gwf emission @reomintion epohD δ ∼ 4 × 10 5 yers fter the fig fngAF sn ryonEdominted niverse δ should e tody t δ < 0.1D while the oservtion of present strutures @eFgF qlxiesD qlxy glustersA requires δ 1F he hypothesis of the hw existene nswers the prolemF sn prtiulr hw should hve deoupled from mtter nd formed strutures erlierD in whih mtter hs ollpsed fterwrdsF prom these onlusions it is possile to onstrin the properties of the hw prtileF o form struture the freeEstreming length of the hw prtiles should e smller thn the struture sleD otherwise they re freely sttering nd prevent its formtionF Q types of prtile ndidtes hve een proposed X

• Hot Dark Matter : hese re reltivisti prtiles tht hve very lrge freeEstreming lengthF ery lrge strutures @superlustersA should hve formed (rst nd then frgmented into smller strutures @qlxy glusters nd then qlxiesAF he study of highEredshift qlxies disrds this senrio IQWF

• Cold Dark Matter : hese re nonEreltivisti prtiles tht hve smll freeEstreming lengthF trutures t the qlti sle ut lso t the irth mss sle re llowedD omptile with the oservtionl dtD thus going into fvour of old hw prtile model ISIF sn old hw senrio smll strutures should hve formed (rstF • Warm Dark Matter : his is the lterntive senrio etween hot nd old hwD from whih hw prtiles hve freeEstreming length t the qlti sleF eove this sle the struture formtion hppens following to the hot hw senrioD nd follows the old hw senrio t smller slesF he hoie etween these di'erent types of hw ndidtes does not only rely on oE servtionl evideneF sndeed xEody simultions suh s i vte ss USD equrius ISP or willenium RS hve een used to proe osmologil struture formtion in the frme of the ΛEghw wodelF hese simultions try to urtely reprodue the oservle niverseD nd the est greement so fr is hieved with old hrk wtter @ghwA prtilesD s stted in the nme of the gosmologil wodelF elso these simultions on(rm tht these prtiles should e wekly interting with ryoni mtterF eording to the xEody simultions with old hwD the hw strutures re hierrhilly distriuted in the niverse Y hw hlos oexist t di'erent slesD forming grvittionl wells in whih ryoni mtter is onentrtedF sn onsequene qlxies re ontined into qlti hw hlosD qlxy glusters re themselves loted into lrger hw hlosD then the sme hppens t the superluster sle nd so onF 1.1.2.2 Thermal relic density he seond onstrint on the nture of the hw prtileD lso rought y the ΛEghw wodelD it set y its therml reli density Ω DM F sf new stle prtile exists @whih is now strongly suggestedAD it should hve een t the therml equilirium in the primordil niverseD s long s the mient temperture ws ove the hw prtile mssF huring the oolingEdown proess of the niverse due to its expnsionD this temperture dropped elow the hw prtile mss nd the therml equilirium rokeF he density of the hw prtiles fell down exponentillyF his is shown in pigure 1.5F roweverD s the niverse kept expnding hw prtiles eme so diluted tht they ould not nnihilte or intert with eh others nymore thus leding to freezeEout in the hw densityD lled therml reli densityD tht depends on the nnihiltion rossEsetion of the hw prtiles weighted y their reltive veloities < σv > nd on the hw prtile mssF sn onsequene n dequte hw prtile ndidte should ount for the mesured vlue of the hw reli density Ω DM 0.26F ekly snterting wssive rtiles @swsA re urrently the preferred senrio in the sienti( ommunity s they follow ll of the ove requirementsF hey onstitute the frmework of this thesisF e good supporting rgumentD lled the 4sw mirle4D is the ft tht the sw therml reli density nturlly mthes the osmologil vlue for Ω DM F king into ount the sw properties into the foltzmnn eqution tht predits the evolution of the hw prtile density in time IHPD the lultion of the hw therml reli density for the sws gives X

Ω DM h 2 3 × 10 -27 cm 3 .s -1 < σ ann v > @IFRA
where h is the redued rule onstnt h = H 0 /(100 km.s -1 .M pc -1 ) nd < σ ann v > is the nnihiltion rossEsetion of sws weighted y their reltive veloitiesF his result is independent from the sw mssF es Ω DM is onstrined in the ΛEghw wodel @Ω DM 0.26 → Ω DM h 2 0.12A this implies veloityEweighted nnihiltion rossEsetion for the sws of the order of X < σ ann v > 3 × 10 -26 cm 3 .s -1 @IFSA tht is tully hrteristi of the wek intertionsD thus on(rming the sttus of sws s exellent hw senrioF elso from the reli density lultion n upper limit for the sw mss is set RR nd orresponds to m DM ≤ 120 T eV F 1.1.3 Particle candidates for WIMP Dark Matter elthough the tndrd wodel of rtile hysis @wA is well estlished nd hs de(nitely proved its vlidity with the reent disovery of the riggs foson t the vrgD this model is still fing theoretil prolemsF sn prtiulr the w does not ount for the grvittionl intertion nd for the existene of swsF hen it eomes neessry to look eyond the frontiers of the w for (nding n pproprite sw hw ndidteF 1.1.3.1 Beyond the Standard Model emong the list of lterntive models tht propose sw ndidtes (gures supersymmetriE l extensions of the w suh s the winiml upersymmetri tndrd wodel @wwA VPD the onstrined winiml upersymmetri tndrd wodel @wwA ITR or the miniml upergrvity wodel @mqeA STF upersymmetry @A suggests tht eh w prtile hs newD undisovered prtner prtileD with the sme guge intertions nd quntum numersD prt from the spin tht di'ers y IGP thus leding to new symmetry etween fermions nd osonsF he list of the w prtiles with their ssoited prtners is given in le 1.1D in the frme of the ww modelF provides potentil solutions to some of the most importnt prolems rised y the w X it o'ers pnel of ndidtes for sw hwD solves the hierrhy prolem @iFeF the understnding of the unexpetedly lrge di'erene etween the mss sles of the wek nd grvittionl intertions ITSAD nd o'ers the possiility to unify the guge ouplings of the w VHF otentil prtile ndidtes for sw hw re the spin H slr sneutrinos @ν e Dν µ Dν τ A nd spin IGP fermions lled neutrlinos @ χ0 1 D χ0 2 D χ0 3 D χ0 4 AD s prt of the ww modelF e potentil ndidte is lso found in the mqe wodel whih is the spin QGP fermion grvitino @ £ qAD the prtner of the grvitonF he sneutrinos hve too lrge nnihiltion nd sttering rossEsetions ompred to the osmologil preditionsD thus not eing good ndidte for the sw hwF yn the other hnd grvitinos re theoretilly relevnt ndidtes ut only intert grvittionlly thus mking their detetion lmost speultive with present experimentsD the ide eing to detet its signtures from the dey of hevier prtilesF 1.1.3.2 The neutralino χ he lowest mss neutrlinoD simply lled neutrlino χD is the preferred sw hw ndidteD whih is one of the mss eigensttes produed in the mixing of neutrlD spin IGP fermions shown in le 1.1 @ino BD wino W3 nd higgsinos H0 1 nd H0 2 AF his neutrlino is stle nd is lso the lightest prtile @vAF st is represented s liner omintion of X

χ ≡ χ0 1 = N 11 B + N 12 W 3 + N 13 H0 1 + N 14 H0 2 @IFTA
where the oe0ients N ij re inferred from the digonliztion of the neutrlino mss mtrixF he neutrlino is wjorn fermionD so its own ntiprtileD leding to nnihiltion proesses produing detetle w prtilesD disussed lter on in 1.

3 complementary detection approaches

sn the sw senrio the hw prtile my ouple with norml mtter thus o'ering di'erent omplementry strtegies for its detetion with modern experimentsF hree min detetion tehniques re reportedD represented in pigure 1.6 X the prodution of the hw prtile in elertorsD diret detetion through hw sttering on nulei in detetorD or the indiret detetion of its nnihiltion produts oming from hw hlosF sn this lst detetion method the hw prtile should e proed through vrious nnihiltion hnnelsD whih re tndrd wodel prtilesF he prodution nd diret detetion methods re rie)y reviewed in this setionD while the indiret detetion method will e the entre of the present investigtionsF sn prtiulrD the nnihiltion of sws my produe exoti spetrl signtures in γErys tht ould e deteted with present γEry experiments suh s rFiFFF Figure IFT ! he tree min priniples for the detetion of sws 1.2.1.1 Production in accelerators he ide is to produe pir of hw prtiles @χA from the highly energeti ollisions of proton ems in prtile elertorsF his senrio is presently studied in the eve nd gw experiments t the vrgD from ollisions t UEV e @in the entre of mssA nd lso now t IQ e with the most reent dtF wore generllyD in rtile hysis the serh for xew hysis eyond the w is n outstnding sujetD mostly onentrted on prtners of the wF elso with the onservtion of the Eprity hevy prtiles my dey into qurk nd gluon jets s well s in pir prodution of the lightest prtile @vAD iFeF the neutrlino in most of the studied modelsF hese hw prtiles nnot e diretly oserved ut n e reveled from missing trnsverse energy in the detetorsF p to now the nonEdetetion of these hw prtiles llowed to set strong onstrints in the most simple models IIIF sn prtiulr pigure 1.7 presents the expeted onstrints on the prmeter spe @m 0 , m 1/2 A of the ww model for the vrg working t IR eD in omprison to other predited onstrints from the future ixyxEI diret detetion experiment s well s indiret detetion with the gherenkov elesope erry @geAD thus showing e0ient omplementrity etween diretD indiret nd elertor studiesF yn the 1.2. Towards indirect detection of the Dark Matter in γ-rays 13 other hndD detetion would give preise informtion on the hw prtile mss nd reli densityD s well s on the nnihiltion nd nuleonEintertion rossEsetionsF Figure IFU ! redited onstrints on the prmeter spe @m 0 , m 1/2 A of the ww model relted to the serh for hw t the vrg working t IR e @lueAF m 0 nd m 1/2 re the uniE versl slr nd gugino mssesD respetivelyF he predited onstrints from the ixyxEI diret detetion experiment @orngeAD from the indiret detetion of hw in γErys t the qE lti gentre with the gherenkov elesope erry @geA @greenAD nd onstrints from the future mesurement of the rnhing rtio f@B s → µ + µ -A t vrg in un ss @mgentA re lso representedF he projeted vrg un ss WS7 gFvF exlusion limit for diret serhes @squrks nd gluinosA is shown y the red solid line for referene QHF pigure tken from oszkowski et lF @IRSD PHISA 1.2.1.2 Direct detection ine ryoni mtter is supposed to e onentrted into the grvittionl wells of lrge hw struturesD the lol hw density t the un is nonEzero @ρ ∼ 0.4 GeV.cm -3 A nd then sws should onstntly pss towrds the irthD thus mking their detetion possile if using groundEsed detetorF he diret detetion method onsists in oserving the elsti ollisions of hw prtiles interting with dense medium of hevy nuleiD usully loted in deep underground lortories for redution of the kground indued y osmiErysF he expeted elsti intertion rossEsetion is of the order of σ ∼ 10 -43 cm 2 thus llowing the 14 Chapitre 1. Introduction detetion of less thn I hw event per dy nd per kg of the detetor mterilF sn prtieD the hw prtiles re deteted from the mesurement of the reoil energy of the nulei in the mediumD this energy eing deposited in the detetor through sintilltionD ioniztion or het produtionF es the rte of nuler intertions is very lowD the dt is highly dominted y kground events from nturl rdiotivity @mostly γ rditionD neutronsD nd α prtiles in lower extentA interting with the mediumF fkground disrimintion onstitutes the most importnt hllenge for diret detetion experimentsF o dte no hw signl hs een deteted ove the 5σ level in the existing diret detetion experiments @more thn PH ll over the worldAD thus setting onstrints on the mss nd on the intertion rossEsetion of the hw prtileF he most onstrining limits so fr hve een otined with enonIHH PW nd v PPF hey re shown in pigure 1.8 together with limits from other experimentsF Figure IFV ! vimits on the intertion rossEsetion nd on the mss of the hw prtilesD from diret detetion experiments @≤ 2014AF he most onstrining limits so fr hve een otined with enonIHH @PWD PHIPA nd v @PPD PHIQAF pigure dpted from iF pigueroE peliino @sgg PHISA 1.2.1.3 Indirect detection es sws re wjorn prtiles they selfEnnihilte in regions of high hw onentrtion produing w prtilesD mostly hevy fermion pirs @χχ → b b, t t, τ + τ -A ut lso guge nd riggs osons @χχ → ZZ, W + W -, HA, hA, ZH, Zh, ZA, W ± H ∓ A where HD hD A nd H ± re the riggs osons of the ww modelF hen these primry nnihiltion produts undergo hdronistion nd dey proesses resulting in the prodution of eletronsD positronsD protonsD ntiprotonsD ntideuteronsD neutrinos nd γErysF he indiret detetion of the hw onsists in the mesurement of these seondry produts to infer or onstrin the hw prtile properE tiesF sn prtiulr Q di'erent types of indiret detetion experiments n e distinguished X

• Searches for antimatter in charged cosmic-rays : ghrged osmiErys mostly onsist in protons @∼ WH7AD helium nuleiD eletrons nd deuteronsF ynly very smll frtion @H FI7A re stle ntiprtiles suh s positronsD ntiprotons nd ntideuteronsF he preise mesurement of the frtion of these rre ntimtter elements in the isotropi osmiEry spetrum my indiretly hrterize the presene of the hw in the niverseF por thisD exE periments suh s ewiveD permiEveD rFiFFF nd more reently ewEHP re serhing for n nomlous ntimtter omponent ove the expeted )ux from stndrd strophysiE l proessesF sn PHHW he ewive experiment found n unexpeted rise in the positron frtion @e + /(e + + e -)A in the IFSEIHH qe rnge IPF he most reent results from the elph wgneti petrometer @ewEHPA mesured the positron frtion with n unequlled preision nd up to RSH qe VD s shown in pigure 1.9@AF he exess n e interpreted s hw omponent ut ould lso result from elertion proesses in the presene of nery pulsrs or supernov remnnts IHUF wore sttistis is required t the highest energies to onludeF yn the other hndD n exess hs lso een reported from the mesurement of the @e + + e -A )ux up to Ie with permiEveD nd ould e of similr origin QD however in ontrdition with similr mesurements provided y rFiFFF up to out Q e TSF he ntiprotonEtoEproton rtio hs lso een mesured with ewEHP WRD not onsistent with hw senrio ut rther omptile with elertion proesses in supernov remnnts IHUF pinlly ntideuterons re lso onsidered s potentil hw nnihiltion hnnel ut results

hve not yet een shown y ewEHPF

• Neutrino telescopes : xeutrinos re expeted to e produed in sw nnihiltion proE essesD mostly from the dey of hevy qurksD tu leptonsD guge osons nd riggs osons ut lso s primry nnihiltion produt @χχ → ν νAF nlike hrged osmiErysD neutrinos re not de)eted y mgneti (elds nd thus n e oserved in the diretion of their sites of produtionF he most prominent trgets for neutrino detetion re the qlti gentre nd the unF sndeedD hw prtiles re ptured y the un grvittionl well nd umulte in thereD where their nnihiltions give rise to neutrino emission tht espe outwrdsF he irth itself is lso studied s potentil trget for hw serhesD lthough the onentrtion of sws is expeted to e muh lower thn in the un RQF e neutrino exess from these soures ould indiretly indite the presene of the hwF p to dte no hw signl hs een reported y present neutrino telesope experiments suh s exei nd segueF pigure 1.10 shows the most reent limits on the nnihiltion rossEsetion of the sws for neuE trinoD γEry nd osmiEry experimentsF he est limits from the neutrino telesopes hve Figure IFW ! wesurements of the positron frtion @A nd of the ntiprotonEtoEproton rtio @A with ewEHP @VDPHIR nd WRDPHISAD oth showing exesses ompred to the expeted )uxes from stndrd strophysil osmiEry proesses een otined y segue elow QSHqe in the χχ → ν ν nnihiltion hnnel @PD PHISAD nd y exei ove QSHqe in the χχ → τ + τ -hnnel @IID PHISAD oth looking in the diretion of the qlti gentreF rowever these limits re not ompetitive with the most reent results from γEry telesopes @permiEveD rFiFFFD weqsgAD disussed in the folloE wing setionsF

• γ-ray telescopes : hotonsD s neutrinosD trvel to the irth in stright lines from their sites of prodution nd re lmost unsored in the lol niverseF por sw hw the photon emission results from the dey of the primry hw nnihiltion produts @mostly b bDt tDτ + τ -AD ut n lso e produed s primry nnihiltion produtsF hey re expeE ted in the qeEe rnge of present γEry telesopesF he resulting γEry energy spetrum my ontin hrteristi signtures suh s n energy utEo' or one or severl nrrow line fetures round the sw mssF he most prominent trgets of present γEry experiments suh s rFiFFFD weqsgD erits nd permiEve re the qlti gentreD hwrf qlxies nd qlxy glustersD with the est nnihiltion rossEsetion limits rehed so fr in the χχ → τ + τ -nnihiltion hnnelF hese results re shown in pigure 1.10F elso exesses omE ptile with the hw existene hve een reported reently with permiEve dt nlysis t the qlti gentreD relted to line ITQ@gF enigerD PHIPA nd ontinuous UH@rooper et lFD PHIRA spetrl signl serhesD s well s in the study of the etiulumEss hwrf qlxy WH@qeringerEmeth et lFD PHISAF he indiret detetion of the hw in γErys onstitutes the frmework of this thesisD serhing for exoti γEry spetrl signtures in the gittrius hwrf qlxy @ghpter 4A nd in the qlti gentre region @ghpter 6A with the righ inergy tereosopi ystem @rFiFFFAF wore detils on hw γEry serhes nd on the ltest results re provided in the next setionsF Figure IFIH ! vimits on the nnihiltion rossEsetion of the hw prtiles with reent neuE trinoD osmiEry nd γEry experimentsF flue X segueEheepgore UW limits with PHIHEPHII qlti gentre dt in the χχ → ν ν nnihiltion hnnel @PD PHISAF ell other presenE ted limits orrespond to the χχ → τ + τ -nnihiltion hnnelF flk X segue limits with PHHWEPHIH irgo gluster dt @ID PHIQAF ed X exei limits with PHHUEPHIP qlti gentre dt @IID PHISAF qreen X permiEve limits with PHHVEPHIR hwrf qlxy stking dt @THD PHISAF urple X weqsg limits with PHIIEPHIQ egueEI hwrf qlxy dt @PRD PHIRAF yrnge X rFiFFFs limits with PHHREPHIR qlti gentre dt @IIVD PHISAF goloured ellipses X snterprettion of the eletronGpositron exesses s hw selfEnnihiltionsD from eE wive @orngeA nd ewiveCpermiEveCrFiFFF @greenA @IPTD PHIHAF he dshed line indites the nturl sle for whih sw is therml reli of the erly niverse @see 1.1.2.3AF pigure dpted from II 1.2.2 γ-ray ux from Dark Matter halos he nnihiltion of hw prtiles into γErys leds to very distintive spetrl signtures tht n e deteted with spe nd groundEsed γEry experimentsF prom this mesured informtion it is then possile to hrterise the nture of the hw nd its sptil distriuE tionF he )ux oming from hw region of interest is the produt of two terms X

dΦ dE γ (E γ , ∆Ω) = Φ astro (∆Ω) × dΦ pp dE γ (E γ ) @IFUA
where E γ is the energy of the γErys nd ∆Ω = 2π[1 -cos(θ res )] the oservtion soE lid ngle @in sterdinsAF θ res is the ngulr resolution of the instrumentF

The astrophysical factor he strophysil ftor hrterizes the hw density distriution in the oserved region of interestF st is expressed s funtion of the squre hw density pro(le ρ(r(l)) integrted long the line of sight @l.o.s.A represented y the l oordinteD nd over the solid ngle ∆Ω X

Φ astro (∆Ω) = ∆Ω dΩ l.o.s. dlρ 2 (r(l)) @IFVA
The particle physics factor he prtile physis ftor hrterizes the γEry nnihiltion proesses in the hw region of interest nd depends on the veloityEweighted nnihiltion rossEsetion of the sws < σ ann v >D the sw mss m χ nd the spetrl pro(le of the γEry signture X

dΦ pp dE γ (E γ ) = < σ ann v > 8πm 2 χ × dN γ dE γ (E γ ) @IFWA
ρ iso (r) = ρ S 1 + r r S 2 @IFIIA
where ρ S is the hrteristi density nd r S the sle rdiusF his pro(le predits the orret rottion urves for strs round the entre of their respetive qlxies s well s the orret veloity dispersion of the qlxies in qlxy glustersF rowever t lrge rdii r r S the isotherml pro(le nnot reprodue the oserved visile mtter distriution in the qlxies SIF he (rst xEody simultions rereting the hierrhil struture of ghw hlos hve rought the de(nition of new universl hlo pro(leD proposed y xvrroD prenk nd hite @IQPD IWWUA X

ρ NFW (r) = ρ S r r S 1 + r r S 2 @IFIPA
por r r S this pro(le hs entrl powerElw uspF he xp pro(le hs een widely onsiE dered in the literture when setting onstrints on the nnihiltion rossEsetion of swsD nd provides exellent (ts of the simulted hw distriutions on wide mss rnge etween 3 × 10 11 nd 3 × 10 15 solr mssesF elso woore et lF @IQHD IWWVA proposed uspier pro(le for (tting the hw distriutions otined with further simultionsF rowever the existene of entrl usp in hw hlos is di0ult to ssess with simultionsD tht require (nite mount of hw t the entre @r = 0AF por this reson more urte hlo pro(le hs een proposed y werritt et lF @IPUD PHHTAD initilly introdued y tF iinsto in IWTS UW X

ρ Ein (r) = ρ S .exp - 2 α r r S α -1 @IFIQA
where α 0.17 for wilky yEmss hlosF his model is very similr to the xp pro(le t the intermedite sles @r ∼ r S A ut here the entrl density symptotilly rehes (nite density t r = 0D providing more onsistent (t to the simulted hw hlosF sn prtiulr the iinsto pro(le orretly desries qlti nd qlxy gluster hlos nd orresponds to the estE(t model for the reent equrius simultions @ISHD PHHVAD t ll hlo mss slesF 20 Chapitre 1. Introduction sn this thesis n iinsto pro(le @α = 0.17A will e lter onsidered for the hw nE lysis in the qlti gentre region @ghpter 6AF st orresponds to the iinsto pro(le shown in pigure 1.11F he sled rdius r S for the wilky y hlo is equl to PH kpD tken from the equrius simultions IQUD while the hrteristi density ρ S is lulted from the lol hw density t the un ρ = 0.39 GeV.cm -3 SQD suh tht ρ Ein (r 0 ) = ρ where r 0 is the distne from the un to the qlti gentreD equl to ∼VFS kpF • Secondary photons -Continuum he dominnt soure of γEry emission is the dey of neutrl pions reted s result of hdroniztion proesses of the primry sw nnihiltion produts @hevy fermions nd guge osonsAF his results in the emission of γEry spetrl ontinuum with utEo' t the kinemti energy limit E γ = m χ D nd whih usully peks t out one order of mgnitude elow m χ F his spetrum is very similr for ll the possile nnihiltion hnnels nd would show up s ump ove the spetr generted from strophysil proessesD tht re usully powerElw distriutedF everl prmetriztions re proposed in the litertureD suh s fergstrom et lF @QWD IWWVAD sitsiomi et lF @ISRD PHHPAD pornengo et lF @VSD PHHRA nd vF ollnd @IRQD PHHSAF en exmple of ontinuous γEry nnihiltion spetrum t m χ = 700 GeV @smered y the response funtions of the rFiFFF telesopes nd normlized to I over the energy rngeA is shown lter on in ghpter 5 @pigure 5.3AD generted from vF ollnd prmetriztion X

dN γ dE γ =          p 1 m χ . e -p 2 Eγ mχ Eγ mχ p 3 + p 4 for E γ ≤ m χ 0 for E γ > m χ @IFIRA
rowever some stndrd γEry strophysil proesses n mimi the hw ontinuumD suh s the γEry emission from pulsrs tht is expeted to utEo' t energies in the qeEe rngeF

• Monochromatic Line he nnihiltion of sws n diretly produe pir of γErys or γ nd Z osonF he result is the emission of monohromti spetrl linesD seen s nrrow peks due to the energy resolution of the detetor QWF por the χχ → γγ proess the line energy is

E line = m χ D while for χχ → γZ it is E line = m χ (1 -m 2 Z /4m 2 χ )
F elso in the )ux lultion the di'erentil energy spetrum for the χχ → γγ hnnel must ount for n dditionl ftor P for the two gmms produed per nnihiltion X

dN γ dE γ χχ→γγ = 2 × δ(E γ -m χ ) @IFISA
he oservtion of these line signtures would e smoking gun evidene for the existene of the hw s suh n exoti spetrl signture is not expeted from stndrd strophysil soures or pulsrsF elso it hs the dvntge of eing more esily distinguishle from strophysil powerElw kgrounds ompred to the hw ontinuumF rowever the γEry line emission mehnism is oneEloop suppressed nd then its rnhing rtio is generlly negligile ompred to the ontinuous emission @out I to Q orders of mgnitude elow petive spetrl signturesF op X seondry photons from neutrl pion deyD produing ontinuous spetrum with utEo' t the sw mssF widdle X γγ or γZ diretly produed s primry nnihiltion produtsD resulting in monohromti spetrl line t the sw mssF fottom X snternl fremsstrhlung emission from hrged nnihiltion produtsD produing γErys y pinl tte dition @pA or irtul snternl fremsstrhlung @sfA proessesD nd resulting in peked energy spetrum lose to the sw mss 1.2. Towards indirect detection of the Dark Matter in γ-rays

23

QVAF es result the relted onstrints tht re set on the sw nnihiltion rossEsetion @eFgF if no line signl found in the oservtions of hw region of interestA nnot e diretly ompred to the vlue required for produing the oserved hw reli density in the niverseD tht hs to ount for this rnhing frtion @< σ ann v > relic ∼ 10 -27 -10 -29 cm 3 .s -1 AF he serh for hw γEry line signtures is t the entre of this thesis work @ghpter 6AF

• Internal Bremsstrahlung snternl fremsstrhlung @sfA emission rises in hw nnihiltion proesses involving the retion of hrged fermions RWF wo types of proesses re distinguished X the pinl tte dition @pA where the γErys re produed from the rdition of these hrged prtilesD nd the irtul snternl fremsstrhlung @sfA proess where γEry is emitted during the exhnge of virtul hrged prtile @see pigure 1.12AF he orresponding spetrl signtures re peked t the highest energiesD lose to the sw mssD ut hve lrger extension thn monohromti linesF yn the other hndD in mny ses the expeted hw )ux from sf emission is higher thn for monohromti lines RWF sn order to detet γEry signl mong the disussed sw nnihiltion hnnelsD it is neessry for the hw prtile mss m χ to lie within the sensitivity rnge of the instruE mentF por the rFiFFF experiment the hw n e proed for msses rnging from ∼IHH qe nd up to ∼IHH eF 1.2.3 Dark Matter observational targets and recent results with γ-ray observatories he γEry )ux from hw nnihiltions is proportionl to the squred density pro(le of the onsidered hlo @1.2.2AD thus fvouring high hw density trget regions for the nlysesF he distne from the hlo is lso n importnt riteri nd should e s smll s possile for mximizing the deteted hw γEry )uxF elso lrge mssEtoElight rtios M/L re preferred for inresing this )ux nd in the mentime minimizing the kground omponent from stndrd strophysil proessesF sn generl the hoie of the nlyzed hw trgets onsists in ompromise of ll the ove riteriF

• The Galactic Centre region :

st is the losest known hw region of interest @∼ VFS kpA nd is one of the most prominent nd most studied trgets for hw serhesF he hllenge here is to del with the numerous strophysil kground ontriutions suh s the gentrl lk hole regionD the nery supernov remnnts nd pulsr wind neul s well s signi(nt ontriution from di'use γEry emission long the qlti lneF he qlti gentre region is extensively studied y reent γEry experiments suh s rFiFFF nd permiEveF sn prtiulr the hw ws serhed with rFiFFF in regions ove nd elow the qlti lne nd provided the est onstrints so fr on the nnihiltion rossEsetion of sws ove QHH qe for oth ontinuous nd line emissions @SD PHIIA@TID PHIQAF he limits for the hw ontinuum hve tully een onsiderly improved in the lst monthsD with the presenttion of the ltest rFiFFFs results t the sgg PHIS gonfereneD using muh lrger dtset @IIVD PHISAF his limit ws shown erlier in pigure 1.10 for the τ + τ -nnihiltion hnnelF sn PHIP line signl ws reported in permiEve dt ITP ove the Qσ levelD t n energy of ∼IQH qeF he signi(ne even rehed the Sσ level when onsidering hw hlo entred t EIFS • longitude from the qlti gentreF his issue hs rised lot of interest within the sienti( ommunity in the lst yersD lthough hw interprettion for the exess is urrently eing exluded y lrger sttistisF he serh for hw line signtures in the qlti gentre region nd onentrting on this prtiulr o'set hlo on(gurtion onstitute lrge prt of the presented thesis workD desried in detils in ghpter 6F wore reently ontinuous γEry exess hs een oserved in the IHH we E SH qe rnge y rooper et lF @UHD PHIRAD using the ltest ville permiEve dtF he spetrl distriution ws fully omptile with hw interprettionD showing n energy utEo' t out QTESI qe nd prediting the orret therml reli densityF rowever this exess ould lso e onsistently interpreted y the presene of previously undeteted popultion of milliseond pulsrs @QQD PHISAF

• Dwarf Spheroidal Galaxies : hese re nery stellite qlxies of the wilky yD nd re the most hwEdominted trgets in the niverse with M/L rtio etween IH nd IHHHF hey re not expeted to e the soure of ny stndrd strophysil γEry emission thus llowing nlyses with low strophysil kgroundF e omplete overview of hw serhes with hwrf pheroidl qlxies is done in ghpter 4 @4.3AD followed y the hw nlysis in the gittrius hwrf qlxyF gurrently the most onstrining limits for the hw ontinuum re provided y permiEve joint nlysis of IS hwrf qlxies @SWD PHISA for energies elow QHH qe @overtken y the reent rFiFFFs limits ove QHH qeAF his limit ws shown in pigure 1.10F hwrf qlxies re lso extensively studied with the weqsg @PRD PHIRA nd erits @PTD PHIPA telesopes with the reent results on egueEsF pinlly the reent nlysis of the etiulumEss hwrf qlxy found the most signi(nt γEry signl ever reported for hwrf qlxyD t QFUσ level @VWD PHISAF he oserved ontinuous exess is omptile with hw interprettion t m χ elow few hundred of qeF

• Galaxy Clusters :

qlxy glusters re the lrgest known grvittionlly ound strutures in the universe nd re the ltest tht hve formedF hey re hrterized y M/L rtio t the order of ∼IHH thus eing good oservtion trgets for indiret hw serhesF woreoverD the qlti suEhlos ontined in the min luster hlo ontriute to lrger strophysil ftor nd inrese the potentil for the hw detetionF roweverD qlxy glusters re distnt @b IS wpA nd their qlxy ontent re the soure of strong strophysil γEry emissions resulting in lrge kground omponentF sn spite of their hw mssesD the potentil of detetion of the hw is rther wek nd the reent limits re not ompeting with the limits from the qlti gentre nd from the hwrf qlxies WPSF e 3.6σ exess hs een reported in the omined study of IV of the rightest qlxy glusters with permiEve dtD showing two γEry lines t IIH qe nd IQH qeF wore dt is required to onlude on this point @WTD PHIQAF

• Dark Matter Sub-halos :

pinlly the omintion of )uxes from ll the nonEresolved suEhlos in the oservle niE verseD t oth the qlti nd osmologil slesD ould e responsile for n lmost isotroE pi di'use hw γEry emission whih hs een proed with permiEveD without ny onlusive results @PUD PHIQAF yn the other hndD it is not exluded tht prtiulr lss of hw suE hlos hs developed without ny presene of ryoni mtterD espeilly the smllest ones whih do not hve strong grvittionl wellsF hese suEhlos re ompletely 4drk4 with no expeted strophysil γEry emissionD thus eing good ndidtes for hw serhes lthough their lotions re unknownF he wilky y is expeted to house lrge mount of these suEhlosF nidenti(ed γEry soures from the permi gtlog hve een reviewed for (nding potentil suEhlo ndidte mong themD with negtive result @SHD PHIHAF he detetion of γErys from strophysil or exoti @eFgF hrk wtterA soures n e done from spe with stellite experiments suh s iqi @IWWI IHQAD eqsvi @PHHU ISSA nd permi @PHHV ISUAD whih detet eletronEposition pirs resulting from the intertion of the primry γEry with dense mterilD nd reonstrut the energyD diretion nd time of rrivl of γErys from few we up to hundred of qeF yn the other hnd groundEsed γEry oservtories re telesopes designed for the detetion of γEry interting with the tmosphereD tht produe sde of seondry prtiles with gherenkov light emission in the rngeD ptured y very sensitive mersF hey lso llow for reonstrution of the diretionD energy nd time of rrivl of the primry γEry eventsD nd o'er lrger e'etive re ompred to the spe telesopes resulting in the detetion of γEry t energies from tens of qe to hundreds of eF uh experiments re referred s smging etmospheri gherenkov elesopes @segsA nd urrently inlude weqsg @PHHQ QPA nd erits @PHHS ITIA in the xorthern hemisphere nd the rFiFFF experiment @PHHP WVA in the outhern hemisphereD plus the future ge projet tht should strt tking dt y the end of the dedeF his hpter reports on the righ inergy tereosopi ystem @rFiFFFA nd gives n overview of the tehnil onepts of the experiment suh s the lirtion of the insE trumentD the priniple of reonstrution of the γEry events nd their disrimintion from the osmiEry kgroundF purther onepts suh s stndrd dt nlysis nd spetrl reonstrution re developed in ghpter 4F Chapitre 2. The H.E.S.S. experiment 2.1 Detection of the Very High Energy gamma-rays he oservtion of strophysil ojets in γErys involves the following onstrints on oth spe nd groundEsed telesopes X E he e'etive re of the telesopes should e lrge enough s it de(nes the sensitiE vity of the instrument iFeF the minimum detetle γEry )ux under resonle oservtion timeD usully SHEIHH hoursF E e lrge (eld of view @pyA is required for the study of extended soures suh s supernov remnnts nd hw signlsF E e good resolution t low energies is neessry for preise spetrl reonstrution nd to proe prtile elertion mehnisms t the ri sleF sn prtiulr good energy resolution is essentil when serhing for exoti spetrl signtures from nnihilting hw prtilesF E e good ngulr resolution mkes possile the identi(tion of γEry soure with respet to its deteted ontriution in rdioD optil or ErysD nd lso llows proing lol emission regions from n extended strophysil soureF hue to their smll e'etive res @ few squre meterA spe experiments re not senE sitive to γEry )uxes ove ∼ QHH qeF qroundEsed experiments tke over t very high energies @riAD from hundreds of qe up to hundred of eF he priniple of γEry detetion with groundEsed experiments is sed on the smpling of the gherenE kov wvefront @with experiments suh s givii WID geg IPID wsveqy IPS nd more reently reg WSA or sed on the imging gherenkov tehnique used in segs @rFiFFFD weqsgD eritsD nd formerly hippleD hurhm wrk TD riqeD ge nd gexqeyyAF ynly the imging gherenkov tehnique is presented in this ghpterF ri γErys trvel from their site of prodution stright to the irth nd then penetrte the tmosphere where they intert with the goulom (eld of the tmospheri nulei nd produe n eletronEpositron pirF hese seondry prtiles undergo fremsstrhlung emission in the sme goulom (eld nd produe new γErys of smller energiesD tht will gin intert with the tmosphere nd rete new pir of eletronEpositronsF he result is the development of n eletromgneti shower in the tmosphereD s shown in pigure 2.2D tht n ontin illions of seondry prtilesD with longitudinl extension of few kilometres nd lterl extension of out tens of metersF he shower stops developing one the energy of the seondry eletronEpositions flls elow ∼ VH we @this vlue tully depends on the ltitude of the (rst intertionA where ionistion eomes dominnt over the fremsstrhlung emission nd do not prtiipte nymore in the shower developmentF he ir shower rehes its mximum of development t out IH km ove se levelF Figure PFP ! hevelopment of n eletromgneti showerD from the intertion of primry γEry with the tmosphere he seondry hrged prtiles trvel ove the speed of light in the ir @ut still elow the speed of light in vuumA nd rete n eletromgneti shokEwve tht results in the emission of gherenkov photons in the ner ultrviolet @λ ∼ 300 -600 nmAF his gherenkov emission n e represented y light one emitted in the diretion of propgtion of the showerF he emission ngle θ depends on the refrtive index of the medium nD the prtile veloity v nd the speed of light in vuum c he priniple of γEry detetion with segs is shown in pigure 2.4 @next pgeA nd onsists in olleting nd fousing the gherenkov light from eletromgneti showers t the fol plne of lrge set of mirrorsD where the light is foused on mers onstituted of very sensitive photomultipliers @wsAD with the use of fst quisition systems @typil integrtion time of ∼I nsA s the gherenkov light is produed on very short time slesF he gherenkov light illumintes totl re of out 10 5 m 2 on the ground llowing to hieve suh lrge e'etive re with n rry of telesopes set t di'erent positions within the gherenkov light poolF e single telesope only sees frgment of the shower under prtiulr ngleD tht gives n lmost elliptil light distriution in the merF he igger the mirror isD the righter the imge will e sine more gherenkov light is foused on the merD nd then the lower the energy threshold for the reonstrution of the γEry events will e @ minimum intensity is required in the ws for triggering the eventsD see 2.2.2AF he energy threshold of the instrument depends on the olletion re of one telesope @AAD the solid ngle of the ws @ΩAD the verge luminosity of the night sky @φ N SB ) @in photoEeletron rte in the ws per unit re nd solid ngleAD the optil e0ieny of the telesope @εA nd the integrtion time @∆tA X

X cosθ = c n.v ∼ 1 n for v ∼ c @PFIA et ∼ IH
E th ∝ Ω.∆t.φ N SB A.ε @PFPA
fy omining di'erent imges of the sme shower seen from severl telesopes loted t di'erent positions within the gherenkov light pool it is possile to reonstrut the energy nd the diretion of the primry γEry with stereosopyF he oservtion of soures with multiple telesopes inreses the preision of the reonstruted energy nd position of the soure nd help disriminting the γEry events with respet to hdroni nd muoni kgroundsD disussed in the next prgrphF xeverthelessD the diretionEenergy reonstrution of deteted prtile is still possile with single telesope @eFgF muonsA for soures with known position in the skyF he kground essentilly onsists in di'use osmiErys hdrons tht lso intert with the tmosphere ut produe vrious distint seondry prtile omponents in the shower X

• rdroni omponent X nuler frgmentsD nuleonsD π nd K mesons • iletromgneti omponent X seondry gmms from π 0 → γγ nd other rditive deys • wuoni omponent X prodution of muons from the dey or hrged mesons @π ± nd K ± A • etmospheri neutrinos omponent from the dey of π ± D K ± nd µ ± he kground showers re mostly initited y protons nd helium nuleiD tht folE low powerElw spetrl distriution of spetrl indexes of PFUV nd of PFTVD respetivelyF feuse of ll the omponents present in the shower the shpe of the imges of hdroni shoE wers in the mers re irregulr nd spred over lrger re ompred to eletromgneti showersD giving the possiility to disriminte hdrons from γErys s it will e disussed in 2.2.5F he hdroni kground is the dominnt kground in segsF sn se of very strong soure s the gr xeulD the γEry )ux in the (rst phse of rFiFFF is ∼QHH times the )ux from hdrons t the energy threshold @IHH qeA efore nlysis disrimintion proedureD tht is ∼ 10 1 -10 3 times righter thn most of the deteted γEry soures in rFiFFF his results in very low initil signlEtoEkground rtios for fint souresF pigure 2.5 shows the longitudinl nd lterl pro(les of typil eletromgneti @A nd hdroni @A showerF Electrons gosmiEry eletrons produe similr eletromgneti showers s γErysD ut they intert t higher ltitudes in the tmosphere @shorter primry depthA nd hve spetrl index of out QFQ thus dominting the hdroni kground t very low energies onlyD t the order of few tens of qeF iletrons ply minor role in present seg9s experiments s they impt the nlysis proedures t very low energies only nd re disriminted from γErys y their di'erenes in primry depthF Muons etmospheri muons produed in hdroni showers @from the dey of hrged pionsA re often deteted s single events in the telesopes nd re used to mesure the optil e0ieny of the instrumentD s they hve very distintive gherenkov signture @ring shpeA visile with single telesopeF his will e lter disussed in 2. he righ inergy tereosopi ystem @rFiFFFA is n rry of (ve imging tmospheri gherenkov telesopes loted in the uhoms righlnd in xmiiD t IVHHm ltitude ove se levelF he nme ws hosen in triute to itor ressD who disovered the existene of osmiErys in IWIP @nd won the xoel prize in IWQTAF he rFiFFF experiment is dedited to the oservtion of the very high energy skyD from ∼SH qe to IHH eF he site lotion ws hosen for its ir purityD with dry tmosphereD low kground luminosity y night nd low loud overgeF elso its lotion in the outhern hemisphere llows the oservtion of the qlti gentre regionF First phase of H.E.S.S. (2002 -2012) rFiFFF sw its (rst light in tune PHHP fter the onstrution of (rst telesopeD followed y the ompletion of the rry with Q other telesopes in PHHQD working in stereosopyF he four telesopes re identilD nd onsist in IPm dimeter proli dish with QVH mirrors tht fous the gherenkov light on mer loted t the fol plneF hey form squre networkD with distne etween the telesopes equl to IPHmD optimized for the detetion of ri γErys with n energy threshold t out IHH qeF e totl of UW strophysil γEry soures hve een oserved with rFiFFFs @lzrsD supernov remnntsD pulsrsD miroqusrs nd other unidenti(ed souresAD nd hve een ojet of more thn ISH pulitionsF Second phase of H.E.S.S. (> 2012) sn PHIP the rFiFFF rry hs een upgrded with the ommissioning of (fth telesope t the entre of the rryD onsisting in PVm dimeter dish nd VUS mirrorsD whih is the lrgest gherenkov telesope in the worldF he im of this (fth ig telesope ws to lower the energy threshold down to out SH qeD hievle y olleting nd fousing more gherenkov light on its merD nd to get more preise reonstrution of the γEry events y stereosopy @tereoAF gS lso opertes in monosopi @wonoA mode for the detetion of events t the lowest energies @∼ energy thresholdA for whih the shower imges re not right enough to trigger gIER mersF he monosopi reonstruE tion of the primry γEry prmeters remins possileD lthough sujet to lrger systemtisF he four smll telesopes re lled gherenkov elesope IER @gIERA in the following setions nd hptersD nd gS for the ig telesopeF 2.2.1 Cameras he rFiFFF mers onsists in rrys of hundreds of photomultipliers @wsAD lso lled pixelsD loted t the fol plne of eh telesopeF hey llow (ne pixelistion of the showers imges nd provide e0ient night sky kground @xfA suppression with the use of fst quisition nd trigger eletronis for integrting the gherenkov signl @the wvefront of the gherenkov light lsts for ∼ IH nsAF ih w is equipped with inston one tht guides the gherenkov light onto the photoEthodeD limits the py of the instrument to the tul size of the mirror nd (lls ded spes etween the wsF gIER mers ontin WTH ws tht hve solid ngle 0.16 • D for totl py of out 5 • F yn the other hnd the gS mer ontins PHRV ws of 0.07 • solid ngle for totl py of out 3.2 • F Figure PFU ! Left X photogrph of rFiFFFs merF Right X piture of drwer from the merF he gherenkov photons re foused y inston ones @eA nd re olleted y the photomultipliers @fA where the signl is onverted into photoEeletrons nd then in n eletri signl @gAF his nlogue signl is (nlly smpled y the quisition eletronis @hA nd sved into memories he ws re grouped in units of IT ws lled drwers ITHF here re TH drwers in gIER nd IPV drwers in gSF ih drwer ontins ll the quisition nd ontrol eletronisD high voltge supply nd prt of the trigger eletronis for the IT ssoited wsF pigure 2.7 shows piture of drwer from the gIER mersF he entrl Chapitre 2. The H.E.S.S. experiment quisition nd trigger units is loted t the k of the merD to ensure fst proessing of the eletroni signlsF he digrm of rFiFFF mer eletronis is shown in pigure 2.8F he gherenkov light enE ters w through inston one nd onverts into sde of out 10 6 photoEeletrons @pFeFA with the pplition of high voltge @rA in the photoEthodesF he pFeF9s onvert into n output tension tht seprtes into two smpling hnnels @with mpli(tionA nd one trigger hnnel @see 2.2.2A on the nlogue rdF he high gin @rqA hnnel is dpted to the detetion of single pFeF with dynmil rnge of I E ISH pFeFD while the low gin @vqA hnnel is dpted for the detetion of righter signls tht over rnge of out PH E PHHH pFeF he ommon rnge is used for lirtion purposes @see 2.2.3AF efter Figure PFV ! higrm of the rFiFFF mer eletronisD tken from IRR eing proessed in the low nd high gin hnnels the signl is smpled t frequeny of I qrz in n enlogue ing mpler @eA for gIER nd in wift enlog wemory @ewA for gSD whih stores the lst IPV signl smples @PST for gSA in memoriesF et the end of the eletroni hin nd when trigger deision ours from setor of the mer the signl informtion ontined in the nlogue memories is digitlised y n enlog to higitl gonverter @ehgA nd onverted into ehg ounts @I ehg ount a IFPP mAD tht is proportionl to the input signl in terms of pFeF his informtion is used fterwrds for the reonstrution of the primry events @see 2.2.5AF purthermore the eletronis in gS hs improved pilities tht llows mesuring the time of mximum hrge @ywA in oth the rq nd vq hnnels of the wsD used for seleting the rightest imges of the prtile showers from the PST smples in memoryF he nlogous rd lso fetures time ove threshold @eA informtion in order to derive the signl durtion in eh wF edditionlly the redout speed in the gS nlogue memories hs een improved y ftor IH ompred to gIER eletronisD resulting in lower ded time etween the triggered events nd then lrger trigger rte @ftor ∼IH lrger thn in gIERAF 2.2.2 Trigger system he trigger deision ours when the distriution of the gherenkov light in the mers ful(l set of requirements t the lol level @in single telesopeA nd t the entrl level @oinidenes etween multiple telesopesAF

• Local trigger level ITH
his level is spei( to eh individul mer nd sets the miniml onstrints tht re required on the shower imges for sending trigger request to the entrl system of the telesopesF he mers re divided into QV setors of TR pixelsD tht overlp eh othersF he trigger deision ours when the gherenkov signl in single setor exeeds R pFeF @pixel thresholdA in t lest Q neighouring pixels @setor thresholdA nd in time window of ∼ IFQ ns @for rejeting xf eventsAF pollowing the trigger deision the nlogue memories re stopped Y the mer digitlises the nlogue informtion in the ehg nd send it through dt us to the entrl trigger systemF

• Central trigger level VU his level mnges the trigger orders reeived from the individul telesopesF e entrl trigger deision is generlly mde when t lest P telesopes send triggering order within oinidene window of VH nsF his enles rejeting muons @the typil sptil extension of muoni light signtures is less thn the distne etween two telesopesA xf events @lthough not ll the xf events re rejeted t the trigger levelA nd ensures the e0ient determintion of the primry γEry prmeters suh s the diretion nd the energyF hen trigger deision ours t the entrl levelD trigger on(rmtion signl is sent k to eh of the onerned mersD tht strt operting ginF he olleted shower informtion is sved onto omputer in the rFiFFF dt frmF sn se no on(rmtion signl is reeived within time window of ∼ 5 µs the nlogue memories re lened Y the telesope strts operting gin ut no informtion is trnsferred to the dt frmF Dead time he time etween trigger deision in single telesope nd the reeption of the entrl trigger on(rmtion signl in tht telesope @C few ns if no on(rmtion signl is sentA is lled ded timeF st inreses with the telesope trigger multipliity @the numer of telesopes prtiipting in the triggerAD nd is ≥ RRT µsF sn totl out S to IS7 of the run durtion onsists in ded timeF he e'etive oservtion time during run is lled livetime nd is otined y sutrting the totl ded time of the telesopes to the tul durtion of the runF he livetime serves s sis in the lultion of the γEry )ux nd for spetrl reonstrutionF Chapitre 2. The H.E.S.S. experiment Monoscopic events with CT5 ith the gS ig telesope it is now possile to reonstrut monosopi @wonoA events without requiring seond telesope in the triggerF et the lowest energies @∼ SH qe to IHH qeA the gherenkov light olleted y the gIER mers is not su0ient to get lol trigger signlF he gS telesope nd its lrger dish tkes over sine more gherenkov light is foused on its merF hen lol trigger deision is sent from gS to the entrl systemD the entrl trigger requirements re ypssed nd the olleted shower informtion is svedF sn future seond level trigger @vPA will e dded in the hin X the nlogous signls in the ew will e ompred to referene imge ptterns with dedited lgorithm in order to vlidte the wono trigger deisionF his deision should tke etween PH nd IHH µs depending on the omplexity of the lgorithmD tht dds to the ded time of the telesopeF yn the other hnd improvements mde in the eletroni hin of the gS mer @in prtiulr pspy u'ers instlled on eh nlogue rdA strongly redues the glol ded time of gSD tht is in the end less thn I7 over the durtion of the runD ompred to SEIS7 in gIERF ith monosopi events it is still possile to infer the diretion nd energy of the primry γEryD lthough sujet to lrger systemti errorsF his will e further disussed in 2.2.5F

Calibration

he lirtion of the instrument is n essentil step efore the dt nlysisD neessry for sptil nd energy reonstrution of the γEry eventsF he lirtion onsists in deriving the onversion oe0ients etween the totl mesured gherenkov light of n event @stored in ehg ounts for eh pixelA nd the numer of gherenkov photons rriving on the telesopesF his is done in two mjor stepsD (rst mesuring the onversion oe0ient etween ehg ounts nd photoEeletrons @mer lirtionA nd then determining the glol optil trnsmission e0ieny of the system @solute energy sle lirtionA for eh telesopeD tht inludes mirrorsD inston ones nd sorption in the tmosphereD to derive the orresE ponding mount of olleted gherenkov lightD this leding to the energy of the primry γErysF pigure 2.9 summrises the evolution steps of the primry γEry events through the di'erent elements of the hin from their (rst intertion in the tmosphere to the (nl numer of ehg ounts in the mersD nd showing the lirtion @PFPFQA nd reonstrution @PFPFSA stges tht llow to get k to the physil properties of these primry events @diretionD impt prmeter nd energyAF 2.2.3.1 Camera calibration e detiled presenttion of the mer lirtion steps is given in IQF he im is to derive the onversion oe0ients etween the ehg ounts nd the numer of pFeFD in oth the high nd low gin smpling hnnelsF hese oe0ients re lulted for eh w nd re given y the following formuls X

A HG = ADC HG -P HG γ HG × F F A LG = ADC LG -P LG γ HG × (HG/LG) × F F @PFQA
where ADC HG nd ADC LG re the mesured hrgesD in ehg ountsD in the high nd low gin hnnels of the wF P HG nd P LG re the rq nd vq pedestls tht represent the numer of ehg ounts generted y the kground noise of the eletroni hin @tht inludes pure eletroni nd xf omponentsAF γ HG is the nominl high gin of the system tht de(nes the numer of ehg ounts ove the pedestl P HG nd per photoEeletronF he nominl low gin of the system nnot e diretly lulted s the vq hnnel is not sensitive to single photoEeletronsD ut it n e inferred from γ HG nd from the highEtoE low gin rtio @rqGvqA otined from diret mesurements of the ehg ounts in the two hnnelsD in their overlpping rngeF @rqGvqA is lulted for eh runF pinlly pp is the )tE(eld oe0ient of the wD tht orrets for the dispersion of the optil nd quntum e0ienies of the w with respet to the verged mer vluesF Figure PFW ! qenerl sheme of the lirtion nd of the γEry event reonstrution in the rFiFFF experimentF his summrises the evolution steps of the primry γEry events through the di'erent elements of the hin from their (rst intertion in the tmosphere to the (nl numer of ehg ounts in the mersF he mer lirtion onsists in mesuring the onversion oe0ient etween the numer of ehg ounts nd the orresponding mplitude in photoEeletronsF he solute energy sle lirtion involves the lultion of the glol optil trnsmission e0ieny of the system for eh telesopeD using tmospheri muonsD to derive the mount of olleted gherenkov lightF pinlly the reonstrution of the physil properties of the primry γErys @iFeF diretionD impt prmeter nd energyA nd their disrimintion with the osmiEry kground is done fter the lirtion steps nd relies on full wonteEgrlo simultions of the tmospheri showers nd of the instrument response @see 2.2.5A

The H.E.S.S. telescope array 41

Gain calibrationγ HG he gin of eh w is derived from dedited lirtion runs done every two nightsF he mers re prked into shelter efore nd fter oservtion nights to protet them from d wether nd to perform di'erent sorts of lirtion runsF his ene(ts from the very low kground light inside the shelter with lmost no ontmintion from xf eventsF he gin lirtion onsists in using )shing vih pulsed t UH rzD pled ∼ P m in front of the merD with intensity djusted to produe single photoEeletron @in vergeA in the photoE thodes with homogeneity of out SH7 over the mer wsF he trigger is synhronised with the vih pulsesF his llows mesuring the numer of ehg ounts orresponding to single pFeFD in the high gin hnnel only @the low gin hnnel is not sensitive to single pFeFAF Figure PFIH ! qin lirtion X hrge distriution in ehg ounts over single pFeF runF he (rst pek @leftA represents the eletroni pedestlD nd the seond pek the single pFeF hrgeF he high voltge is set up for hving high gin γ HG of VH ehg ounts over the pedestl in gIERD nd SH ehg ounts in gSF he distriution is (tted with douleEqussin funtionF pigure tken from UP he hrge distriution in terms of ehg ounts is shown in pigure 2.10F he (rst pek orresponds to the numer of ehg ounts generted y the eletroni pedestl in the high gin hnnelD with typil width of ∼ IT ehg ountsF he seond is the single pFeF pek Y the high voltge in the ws ws initilly set for rehing high gin of VH ehg ounts ove the pedestl for single pFeF nd in the gIER mersF sn gS the high gin is set to SHF rere the lirtion step provides the tul verged gin in eh w s well s the gin dispersion over the whole merF he hrge distriution for signl of n pFeF is (tted with douleEqussin prmetriztion Y the high gin γ HG D the high gin eletroni pedestl of men P HG e nd width σ P D the width of the single pFeF pek σ γ D the verge intensity µ of the light reeived y the w nd the normliztion onstnt N S re set s free prmetersF x is the totl numer of single pFeF events triggered y the merF he prmetriztion in terms of ehg ounts @xA is the following IST X

G(x) = N × e -µ √ 2πσ P exp - (x -P HG e ) 2 2σ 2 P + N × N S m 1 n=1 e -µ √ 2πnσ γ µ n n! exp - (x -(P HG e + nγ HG )) 2 2nσ 2 γ @PFRA
he high gin γ HG in eh w is then inferred from the (tF High-to-low gain ratio -(HG/LG) st is not possile to derive the low gin with single pFeF mesurements s the low gin hnnel opertes in the dynmil rnge PH E PHHH pFeF gonsequently the low gin is determined from the high gin y mesuring the rtio rqGvq in eh pixelD one during eh runD in the overlpping dynmil rnges of the two hnnelsF his oe0ient is of the order of (HG/LG) = 13.5 with dispersion of out IH7 from one run to notherF Pedestal -P HG , P LG he pedestl from pure eletroni noise @∼ IT ehg ountsA n e otined during the gin lirtion @rq hnnelAF here re lso dedited pedestl runs performed with the mer lid losed @without single pFeF vihA for mesuring the rq nd vq eletroni pedestls nd to investigte vrious instrumentl e'ets suh s their evolution with the tempertureD tht hs very strong impt @∼ IH ehg ounts per degree gelsiusAF rowever for lulting the onversion oe0ient @eqF 2.3A the lultion of the eletroni pedestls is not su0ient mesurementD nd the true pedestls tht inlude the tul temperture nd xf level during the oservtion runs must e lulted instedF he rq nd vq pedestls P HG nd P LG re mesured in the nonEtriggering pixels of the reorded eventsD eh time the men pedestl vlues over the mer moves y more thn IH ehg ounts in t lest four pixelsF his llows preise mesurement of their temporl evolutionD due to temperture nd xf vritionsF pigure 2.11 shows n exmple of the impt of the xf level on the rq pedestl distriution in the rFiFFFs mersF por xf level of out IHH wrz @verge xf level during oservtionsA the rq pedestl is similr to the shpe of the photoEeletron spetrumF he only di'erene is tht the xf events rrive rndomly on the mers nd then most of them do not pss the trigger levelsF xevertheless signi(nt frtion of xf events still remin in the reorded eventsD t the lowest energiesF Flat-eld coecient -F F he lultion of the )tE(eld oe0ients is the lst step of the mer lirtionD tht onsists in orreting the onversion oe0ient @eqF 2.3A for the reltive di'erene in the light intensity @relted to the optil C quntum e0ieniesA reeived y the individul ws omE pred to the verged vlue on the whole merF st is inferred during spei( )tE(elding lirtion runs performed monthly @iFeF for eh oservtion periodA inside the mer shelE terD using )shing vih pled t the entre of the telesope dish nd equipped with di'user for sending uniform light intensity over the whole merF he )tE(eld oe0ient is lulted s the rtio of the verged light intensity on the whole mer nd the verged intensity in the individul w X

F F = < I > Camera < I > PMT @PFSA
he verges re de(ned over the oservtion periodF he )tE(eld oe0ient is lulted in eh wD nd in the rq or vq hnnel depending on the vih intensityF

Absolute energy scale calibration

he ginD pedestl nd )tE(eld lirtion oe0ients desried in the previous setion re used to lulte the onversion oe0ients etween the numer of ehg ounts in the rqGvq hnnels nd the numer of photoEeletrons t the photoEthodeD the mesurement eing mde for eh individul wF rowever the numer of pFeF is not su0ient to get physis interprettion of the gherenkov signl nd to reonstrut the energy nd diretion of the primry γErysF sn onsequene the lultion of the solute olletion e0ieny of the instrument is neessry to (nd the onversion oe0ient etween the numer of pFeF nd the tul numer of gherenkov photonsF his oe0ient depends on the re)etivity of the mirrorsD inston ones nd entrne window of the wsD the olletion e0ieny of these re)etive elements @tht depends on their plement nd orienttionA nd the olletion nd quntum e0ieny of the wsF es these ftors depend on the wvelength this requires to perform the lirtion over the omplete spetrl rnge of the gherenkov lightD lmost impossile in prtieF sn onsequene the solute lirtion in rFiFFF nd in ll present segs relies on the mesuE rement of the gherenkov light emitted y tmospheri muons to lirte the instrument nd lulte the light olletion e0ieny of the system @µAD lso lled optil or muon e0ienyF

Optical/muon eciency he gherenkov light emitted y tmospheri muons is similr to the gherenkov light produed y eletrons in γEry showersD ut hs the spei(ity of produing one of gherenkov light nd t lower ltitude thn the gherenkov emission from γEry indued showersF his results in hrteristi ring or r imges in the mersF pigure 2.12 shows typil ring imge in rFiFFFs mer when the muon flls lose to the entre of the telesope dish @A nd n r imge when it flls on the side or next to the telesope @AF Figure PFIP ! ixmple of muon imges reorded y the rFiFFF mersF @A gomplete gherenkov ring used y muon flling lose to the entre of the telesope dishF @A rtil gherenkov ring @rA used y muon flling on the side or next to the dishF pigure tken from IRR sn stereosopi mode most of the muons re rejeted y the entrl trigger sine the gherenkov light ones re not extended enough to reh seond telesope Y only few muoni events re deteted per telesope nd per hour nd re used in the lultion of the optil e0ieny of the instrumentF he imges reeived on the mers re ompred with n nlytil model of muoni gherenkov ligh emission from whih the glol optil e0ieny is lulted for eh telesopeF sn onlusion only less thn IH7 of the gherenkov photons rehing the telesopes re tully detetedD whih de(nes the optil e0ieny of the instrumentF he systemti unertinties on the solute liE 2.2. The H.E.S.S. telescope array 45 rtion re of the order of IHEIS7 PHD nd out S7 on the mer lirtion @2.2.3.1A TRF pigure 2.13 shows the evolution of the verged optil e0ieny of gP etween PHHR nd PHIRD run y runF he degrde in the re)etivity of the di'erent re)etive elements result in derese in the optil e0ieny over the yersF he sudden inrese round run numer TIHHH orreltes with the reEluminiztion of the mirrors in PHIHF elso the high voltge in the ws is periodilly rised for reEdjusting the ginsD nd results in periodil inrese in the optil e0ieniesF

Figure PFIQ ! ivolution of the optil e0ieny in gP etween PHHR nd PHIRF pigure tken from SS woreover the optil e0ienies implemented into the run dtse re tully onverted into reltive optil e0ieniesD the referene vlue @IHH7A eing inferred from wonteEgrlo simultions y lunhing muons on perfet telesope nd reonstruting them using the muoni model lgorithmF hese reltive optil e0ienies re used s orretion ftors for the reonstrution of the energy nd the )ux of the primry γErysD tht is sed on the omprison of the rel shower imges with wg simulted imges s it will e desried in setion 2.2.5F ypil reltive optil e0ienies in PHIR re ∼THEUH7 in gIER nd ∼VH7 in gSF 2.2.4 Autofocus system sn the rFiFFFs telesopes the mers @iFeF the surfe of the wsA re not extly loted t the fol plne of the mirrorsF snsted of fousing t the in(nity they re o'set from the fol plne y few entimetres suh tht the gherenkov light emitted t out IH km ltitude genertes lener imges in the mersD whih results in lrger trigger rteD etter reonstrution of the energy nd diretion of the primry γErysD etter gmmEhdron disrimintion nd smller ngulr resolutionF sn the seond phse of rFiFFFD the new gS telesope hs een equipped with n utofous systemD tht llows vrying the distne etween the mer position nd the fol plne of the telesope utomtillyF he utofous system is shown in pigure 2.14F

Figure PFIR ! iture of the utofous system instlled on gS he reltionship etween the fous distne @in kilometresA nd the fous position @in millimetresA is the following X

F distance = 1 36000 - 1 (36000 + F position + 20.6) -1 × 10 -6 @PFTA
where QTHHH orresponds to the fol length of the mirrors in mmD iFeF QT metres for gSF pigure 2.15 shows the impt of the utofous distne on simulted shower imges in the gS merD for zenith oservtions of PHH qe γEryF sn this se the est mer response is otined for fous t IR kmD while spred in the shower imge is oserved when fousing t the in(nityD s expetedF ith this dditionl fility it is now possile to dpt the fous position of gS with respet to the oservtion onditions in eh runD nd improve the generl performnes of rFiFFF for γEry reonstrution nd osmiEry kground disrimintionF sn prtiulr the oservtion zenith ngle hs n impt on the imge qulity in the mer s the distne etween the telesope nd the mximum of the shower development hngesF he fous distne of the gS telesope n e written s funtion of the ssoited ltitude ove the ground F altitude @fous ltitude in kilometresA nd the zenith ngle θ z @in degreesA X

F altitude = F distance × cos (90 -θ z ). π 180 @PFUA
por the moment the gS telesope essentilly opertes with (xed fous position of CTT mm tht orresponds to fous distne of IS kmD whih ws optimized with wonteEgrlo simultions IIRF he glol wonteEgrlo performnes of the utofous system hve een lso investigted in this ited pperD for vrious zenith ngles nd γEry energiesF woreover the sttus of the gS utofous in eh run is now used s new onstrint for run qulity seletions @see 3.4.5AF

Reconstruction of the γ-ray events

efter dt tking nd fter ompletion of the lirtion step desried in 2.2.3D the reonstrution nd the identi(tion of the primry prtiles triggered y the instrument is performed @efore physis nlysesAF his onsists in the reonstrution of the diretionD the impt prmeter @the impt position on the groundA nd the energy of the prtilesF he gmmGhdron seprtion relies on the omprison of the shower imges in the mers with imges generted from wonteEgrlo @wgA simultions of the showers leding to disriminE ting vrilesF pigure 2.16 shows n exmple of typil shower imges seen in eh rFiFFF merD for primry γEry @A nd osmiEry hdron @A triggered y ll the S telesopesF rere two mjor methods in use in the rFiFFF experiment re desried X • he (rst method @2.2.5.2AD lled rills reonstrutionD is sed on the hypothesis tht the distriutions of hrged prtiles in γEry showers hve n ellipsoidl shpeD thus reduing the shower imges to few numer of prmeters @PEdimensionl ellipsesAF he diretion of the primry γErys is inferred geometrilly while the energy is otined from the mplitude of the shower imges nd from the omprison of the ellipses with ssoited wg preditionsF • he seond method @2.2.5.3AD lled wodel reonstrutionD is more preise ut lso more omplex s the shower imges re ompred pixel per pixel with the simultionsD using vikelihood (t nd set of new disriminnt vriles for gmmGhdron seprtionF he rills reonstrution hs een extensively used for the prodution of physis reE sults sine PHHTD while the wodel reonstrution is more reent nd is urrently used y the prenh ommunity of the rFiFFF gollortionD under the Parisanalysis nlysis nd reonstrution softwre developed y wthieu de xurois @vv E iole olytehniqueD liseuAF he two methods re dpted for stereosopi reonstrutionD now with the S telesopesF he wodel reonstrution is eing used for ll the work presented in this mnusriptD s fundmentl step efore proeeding to the dt nlysis nd produing physis results @ghpters 4D 5 nd 6AF 2.2.5.1 Full Monte-Carlo simulations he reonstrution of the primry prtiles requires relisti simultions of the shower imges in the rFiFFF mersD tht re used in oth rills nd wodel reonstrutionsF sn (rst step the ueuehi ode IHS @IWWRAD initilly developed for the hipple exE periment IHT nd upgrded for rFiFFF nlyses WQD provides full simultions of the tmospheri shower development for vrious primry prtiles suh s γErysD eletronsD protons nd lso helium nuleiF sn prtiulr they inlude the di'erent intertion proesses in the tmosphereD the energy losses from ioniztionD fremsstrhlungD inelsti sttering nd positron nnihiltionD the e'et from the geomgneti (eld nd (nlly the genertion of the gherenkov photons from the seondry prtiles nd their sorption in the tmosphereF ynly gherenkov photons flling in the detetle wvelength rnge of the ws re onsideredD resulting in the end in relisti numer of gherenkov photons rriving on the rFiFFF mersF Figure PFIT ! ixmple of rel shower imges seen in the rFiFFF mersD here for primry γEry @A nd for osmiEry hdron @A triggered y ll the S telesopes hen the output (le from the ueuehi shower simultions is used s the input of the msh ode WQ developed for rFiFFF nlysesD whih provides full simultion of the instrument response to the input gherenkov photons nd genertes the shower imges in the individul pixels of the simulted rFiFFF mersD tht will e used s referenes for the reonstrution of the rel eventsF msh simultions inlude in prtiulr the re)etivity of the mirrors nd of the inston onesD the geometril ostles @eFgF telesope mounts nd mersA tht re on the wy of the gherenkov light nd prevent them for rehing the mirrorsD the onversion of gherenkov photons to photoEeletrons in the ws nd their proessing y the lol triggerD entrl trigger nd quisition systemsF ell the informtion out the deteted wg events @nd in prtiulr the intensity in eh mer pixels iFeF the shower imgesA re stored in (le of the sme nture thn the rel dtF he disriminnt vriles for the reonstrution nd the identi(tion of the primry prtiles in given reonstrution method @here rills nd wodelA re derived for vrious input prmeters on the primry prtiles nd on the telesopes oservtion onditions suh s the energyD impt prmeterD zenith ngleD zimuth ngle nd wole o'set @see 4.1.2AF he result is tle tht ssoites the input prmeters with their output disriminnt vrilesD used for dtGwg omprisonsF 2.2.5.2 Hillas reconstruction his pproh ws developped y eF wF rills in IWVS WU nd ws (rst pplied to the hipple telesopes dt nd is sed on the hypothesis tht the distriutions of hrged prtiles in γEry showers hve n ellipsoidl shpeF he resulting imges in the mers re (tted y PEdimensionl ellipse modelsD thus reduing the shower imges to smll numer of hrteristi prmetersF pirst the imges re lenedEup in order to keep only the pixels tht took prt in the gherenkov emission PHF por eh mer imge the prmeters re the length nd width of the ellipseD the totl imge mplitudeD the imge ryentre nd the distne etween the ryentre of the ellipse nd the entre of the merF he priniple of the rills reonstrution is shown in pigure 2.17 @AF Reconstruction of the direction hen ringing the imges from the di'erent mers in ommon virtul mer referentil the diretion nd impt prmeter of the primry γEry n e inferred y stereosopy from the intersetion of the mjor xis of the di'erent ellipsesF he reonstruted diretion di'ers from the expeted soure diretion y n ngle Θ from whih the distriution for pointElike soure de(nes the ngulr resolution of the instrumentD of the order of HFI • in rFiFFF for oservtions lose to the zenithF elso the shower impt position on the ground is otined from the geometril intersetion of the plnes in the sky ontining the telesopes nd the shower trkF sn monosopi telesope on(gurtion @done with gS onlyA the diretion of the primry prtile is diretly otined from the rills prmeters @the lengthD width nd orienttion ngle of the ellipse with respet to the mer entreA using tles @wg simultionsA nd dditionl disriminnt vriles to rek the degenery etween the di'erent possile reonstruted diretionsF

E reco = 1 N tel × tel E tel @PFVA
where the individul energies re inferred from the totl imge mplitude nd from the omprison of the imges in the mers @redued to the rills prmetersA with wg simulted imgesD using the wg tles desried in 2.2.5.1F

Gamma-hadron separation he disrimintion etween eletromgneti nd hdroni shower imges is done using sled disriminnt vriles y the omprison of the length nd width of the rills ellipses with the verged length < l > nd width < w > from the wg simultion tlesD nd then renormlized y their respetive vrines σ l nd σ w tht ount for the )ututions rising in the shower development X

S l = l-< l > σ l ; S w = w-< w > σ w @PFWA
he gherenkov light signtures eing di'erent etween eletromgneti @pure elliptil imgesA nd hdroni showers @impreise imgesD no prtiulr shpeA the distriution of these disriminnt prmeters S l nd S w n e used s sis for gmmEhdron seprtionF pigure 2.17 @A shows the distriution of the men sled width M S w verged over the telesopesD where wg simulted γErys re represented in grey nd pure kground dt events @tken in region exempt from souresA y the lk dotsD well omptile with the wg preditions for hdrons @here osmiEry protonsAF guts re pplied on M S w showed y the vertil linesD to rejet ll the events tht do not enter in the ut rngeF ypil vlues of the men sled prmeters in the nlysis of n strophysil soures of spetrl index Γ = 2.0 re M S l ∈ [-2; 2] nd M S w ∈ [-2; 0.9]F et is n e oserved in pigure 2.17 frtion of the γErys re lso exluded in the proessD while signi(nt ontriution of the hdroni events remins nd re identi(ed s γErysD lled γElike eventsF purther rejetion of the residul hdrons n e done t the nlysis level @see ghpter 4AF

Model reconstruction

his seond pproh is urrently extensively used in rFiFFF nd espeilly in prenh nlysesF st ws inspired y the method developed for the ge experiment IIU nd hs een dpted nd ompleted y wF de xurois nd vF ollnd for rFiFFF he method is explined with more detils in UR @PHHWAF he wodel reonstrution is more preise thn the rills pproh desried in 2.2.5.2D s it mkes use of the full informtion present in eh of the individul mer pixels @wsAF Reconstruction of the direction and energy e mximum likelihood proedure @see 5.1A ompres the shower imges in the mers with the expettion from the full wg simultions @2.2.5.1AD pixel per pixelF he logrithmi likelihood funtion for single pixel is written X lnL = -2.lnP (s|µ, σ e , σ N SB ) @PFIHA where P (s|µ, σ e , σ N SB ) is the density proility to oserve signl s in pixel where the expeted signl in µF he totl likelihood funtion for single telesope is the sum of the individul likelihood ontriutions for eh pixel of the merF ith this tehnique it is possile to infer the energyD diretion nd impt prmeter of primry prtile nd lso the primry depth @tht ws ssumed in the rills pprohAF he response funtions of the instrument @iFeF the eptneD energy is nd resolutionD nd ngulr resolutionA will e disussed lter on in ghpter 5 @5.2.2.1AF es n exmple pigure 2.18 shows the omprison of the rills nd wodel performnes with pointElike soures in terms of energy nd ngulr resolutionD using stndrd uts @iFeF t lest P telesopes hving minimum imge mplitude of TH pFeF nd mximl nominl distne of 2 • etween the entre of the shower imge nd the entre of the merA nd lso fint soure uts for rills @imge mplitudes b PHH pFeFAF es expeted the model reonstrution is performing etter thn rills y out PSESH7D nd even more in terms of ngulr resolution for energies elow I eF for the rills nd wodel reonstrutionsD using stndrd uts @imge mplitudes b TH pFeFA nd fint uts @b PHH pFeFD here only for rillsA dpted for pointElike soure nlysisF pigure dpted from UR Gamma-hadron separation e disriminnt vrile lled 4goodness of (t4 sed on the likelihood funtion @eqF 2.10A hs een proposed in UR s powerful wy of rejeting the hdroni eventsF st is de(ned s di'erene etween the lulted logElikelihood funtion lnL(s|µ) nd the one predited from wg simultions < lnL > | µ D summed over ll the mer pixels X

G = pixel i [lnL(s i |µ i )-< lnL > | µ i ] √ 2 × N d.o.f. @PFIIA
where N d.o.f. is the numer of degree of freedom @iFeF N pixel -6 hereAF prom this vrile two other quntities re derived X

• he Shower GoodnessD de(ned s the qulity of the (t for the pixels prtiipting in the shower imgeF

• he Background GoodnessD iFeF the qulity of the (t for the nonEprtiipting pixelsF pigure 2.19 shows the distriution of the Shower Goodness disriminnt vrile for the nlysis of the pointElike soure u PISSEQHR @4.2.3A tht is ompred to the wg preditions nd to the kground distriution in nery region exempt from souresF es for the rills pproh uts re de(ned on these disriminnt vriles to rejet most of the osmiEry hdronsD lthough signi(nt frtion remins fter utsF por rFiFFFs nlyses the stndrd Shower Goodness ut is set to HFTF he e0ieny of the identi(tion of the deteted events is ftor PS7 higher for wodel ompred to the rills reonstrution UIF elso other disriminnt vriles re de(ned in the wodel reonstrution suh s spei( uts for rejeting xf events @eFgF NSB GoodnessA nd Primary Depth uts to help disriminting etween γErys nd the di'use osmiEry kgroundD espeilly eletrons tht dominte t the lowest energies nd intert erlier in the tmosphere thn γErys @see 2.1.0.3AF

Figure PFIW ! histriution of the Shower Goodness disriminnt vrile in the nlysis of pointElike soure u PISSEQHRF e ut is pplied @vertil lineA to rejet most of the hdroni kground events from the nlysisF pigure tken from UR he wodel reonstrution will e used for ll the dt nlyses presented in this mE nusriptD with further desription of its performnes @eFgF response funtionsA nd of the seleted uts on the minimum hrge nd on the disriminnt vriles @tndrdD vooseD pintA in the relted hptersD to dpt the reonstrution to the type of nlysis performed @eFgF strophysil pointElike or extended souresD or hrk wtter serhesAF sn prtiulr di'erent sets of uts re de(ned for monosopi @gSA nd stereosopi nlysesF

Conclusions

he rFiFFF experiment is one of the leding groundEsed γEry oservtories of its genertionD nd proly the most dvned rry of smging etmospheri gherenkov elesopes @segsA sine the ommissioning of the iggest gherenkov telesope in the world in PHIPD enling oservtions of the γEry sky from ∼SH qe up to out hundred of eF eout UW γEry soures mong pulsrsD lzrsD supernov remnnts nd some unidenti(ed soures hve een dded in the rFiFFF soure tlogue during the (rst phse of the experimentD with lot more expeted in its seond phse Y in prtiulr the inresed sensitivity t the lowest energies is idel for the detetion of new etive qlti xulei nd espeilly miroqusrsD s well s for the serh for pulsed emission from pulsrs s models predit utEo' in their spetr t out IH to SH qeF his ws hieved in PHIR s one of the most prominent results from the seond phse of rFiFFF with the detetion of pulsed emission from the el pulsrD with the use of ultr loose uts llowing rehing energies down to PH qe VVF elso the privileged lotion of the telesopes in the outhern hemisphere o'ers the possiility to investigte the ri emission from the qlti gentre regionD hievle with the other urrent segs weqsg nd erits t very high zenith ngles only @nd then with lrge energy thresholdsAF rFiFFFss omplements studies done y the permiEve spe experiment t lower energies @eFgF di'use emissionD entrl nd nery γEry souresAF sn prtiulr the rFiFFF experiment is in very good position for setting onstrints on nnihilting hrk wtter prtilesD for wide rnge of msses t ri @b IHH qeA nd now with dditionl overge in the high energy prt of the permiEve sensitivity @SH qe E QHH qeAF hrk wtter studies will e extensively overed in the next hpters of this mnusriptF he importnt steps in the lirtion of the instrument nd in the reonstrution of the γEry events hve een desried in this hpterD sed on the mesurements of the gherenkov light emitted y seondry hrged prtiles nd initited y the intertion of the primry γErys with the tmosphereF sn prtiulr the wodel reonstrution developed on the prenh side of the rFiFFF gollortion nd integrted in the ParisAnalysis hin llows reonstruting the diretion nd energy of these primry γErys with n unequlled preision ompred to other methodsD with the possiility to perform monosopi @with gS onlyA nd stereosopi reonstrutions @with ll S telesopesAF roedures for dt nlysis nd for the prodution of physis results re desried in ghpters 4D 5 nd 6F xevertheless the strting point towrds good dt nlysis is to produe list of good qulity runs tht follows set of requirements sed on the generl stte nd lirtion of the instrument nd on the qulity of the tmosphereF his will e desried in ghpter 3F huring the dt tking it is usul to fe tehnil prolemsD suh s spontneous rsh of the entrl dt quisition @heA systemD fulty drwers or ded pixels in the mersD or mehnil issues tht 'et the motion of the telesopesF elso the oservtion of very right trnsient ojets suh s shooting strs entering the py of the telesopes is very ommon nd uses the mer photomultipliers @wsA to sturteF wost of 'eted runs re not disrded nd the dt olleted y the system efore the prolem ourred is ville for the rFiFFF nlysesF yn the other sideD externl ftors suh s the ir humidity levelD the wind speed nd loud overge my lso strongly degrde the qulity of the oservtionsF hese vriles re monitored y wether sttion loted ner the telesopesF ell these Chapitre 3. Improvement of the run quality selection software for H.E.S.S.II analyses tehnil nd externl ftors my ompromise the reonstrution of the γEry events on the nlysis side nd produe unexpeted @or t lest less relileA physis resultsF es n exmple the spetrl reonstrution in rFiFFF @see 4.2.1A relies on wonteEgrlo simultions tht re produed ssuming n tmospheri model typil for the rFiFFF site X the imge size on the mers my e misinterpreted if the oservtion runs re tken with rther di'erent wether onditionsD leding to ised energy reonstrution of the gmmElike events nd vrition of the energy thresholdF st seems then neessry to monitor the qulity of the oservtion runs efore proeeE ding to the dt nlysesD nd to de(ne quntittive wys of rejeting runs tht do not (ll stndrds in terms of dt qulityF por this im run qulity seletion softwres hve een developed within the rFiFFF gollortion to (lter the rFiFFF dtse with preEde(ned @or ustomA sets of run seletion riteriD nd produe sfe run list for physis nlysesF eprt from the rejetion of d qulity runsD the runs n e (ltered following to riteri suh s the trget region in the sky @essentil for ll run seletionsA the numer of opertionl telesopes during the dt tking or the zenith ngle of the trget soure verged over the durtion of the runD to (t the requirements for prtiulr physis seF sndependent odes re ville oth for reidelerg nd ris nlysesF rere we report on the seond run seletion softwreD lled risunulityF 3.2 The ParisRunQuality software risunulity is the prenh rFiFFF run seletion softwre used to generte run lists for physis nlysesF st is oded in pythonGgCC nd inorportes grphil user interfe @qsA for esy monitoring of the run seletionsF he min qs window is presented in pigure 3.1F he left pnel ontins ll the uttons tht re used to lod nd (lter runs from the dtse or from input run listD nd to sve the (nl run list in (leF he top pnel shows the list of runs eing urrently seletedD with informtion suh s the run numerD the trget soureD the numer of opertionl telesopes or the run durtionF he middle pnel displys ontrol plots with the distriution of ll individul run qulity vrilesD very useful for intuitive monitoring nd optimiztion of the seletion utsF ristogrms re (lled with glol run informtion or with individul telesope informtion depending on the nture of the informtionF por instne the run durtion is glol vrileD wheres the roken pixel frtion is di'erent in eh telesope of single runF pinlly the ottom pnel is used to de(ne the seletion utsD llowing to nvigte through individul suEmodules for eh lss of seletion riteri suh s 4rget4D 4rigger4 nd 4weteo4D nd set the vlues for eh individul utF fy liking on 4erun (lters4 on the left pnel the urrent run seletion is updted with respet to the new utsF elso runs n e diretly (ltered y hnd using the top pnelF et the end of the seletion proess the run list is sved into Fvs (le tht is used s n input of the rFiFFF nlysis softwre risenlysis for produing physis resultsF he risunulity softwre hs een initilly set up for rFiFFFs nlyses with the gIER telesopesD therefore mjor upgrde in the ode ws mndtory for prtiulr 3.2. The ParisRunQuality software 59 use with the gS telesope in the run seletion proessD whih hs een set s high priority tsk within the rFiFFF gollortionF sn this hpter the run seletion proess with risunulity is (rst introdued for stndrd rFiFFFs nlyses @3.3AF hen developments tht re spei( to the use of the gS telesope will e disussed in detilsD s well s some new dditionl fetures essile from the qs @3.4AF he list of ll individul run vriles tht re used in risunulity is presented elowF he defult uts tht re urrently pplied on these vriles when produing run lists with rFiFFFs dt @gIERA re given in le 3.1F

• Target the runs n e seleted from their trget positionD eFgF keeping runs tht ontin the nme of the trget in the run heder or runs from whih the pointing position of the telesopes lie inside irulr region of hosen extension round the trget soureF his enles omintion of runs tken t di'erent trget soures ut shring ommon region in their respetive (elds of view @pyAD where the nlysis n e performedF his is prtiulrly useful in the qlti gentre region where strophysil soures suh s ri tIURSEQHQ @6.4A nd ri tIURIEQHP @4.2.2A re oserved from the sme dtset tken t the entrl soure gittrius eBF

• Run properties he runs n e seleted with respet to the numer of telesopes tht re opertionl during the dt tkingD whih is set to minimum of Q telesopes y defult for rFiFFFs nlyses to ensure the good stereosopi reonstrution of the γEry eventsF guts re lso pplied on the run durtionD the stndrd durtion for omplete run eing PV minutesF rowever tehnil or externl ftors my use the run to stop efore eing ompleteD s it ws disussed in 3.1F e minimum run durtion of S minutes is set y defult in risunulity to provide su0ient event sttistis nd to derive urte pedestl vlues of the mer pixels @see the lirtion setionD 2.2.3AF pinlly uts n e pplied on the minimum nd mximum run identi(tion numersD eFgF to llow seleting runs in given oservtion periodF

• Tracking e trking module is ville in risunulity to ut on the oservtion onditions of the trget souresD here the zenith nd zimuth nglesF he inrese in zenith ngle uses n inrese in the energy thresholdD sine the γErys hve to ross longer distne in the tmosphere nd loose more energy efore produing the gherenkov photonsF he zimuth ngle lso hs strong impt on the energy thresholdD s it will e lter disussed in 6.8.2.1F everl soures eFgF the qlti gentre nd u PISSEQHR re oserved during di'erent oservtion periods in yerD under vrious zenith nd zimuth nglesF his leds to inhomogeneous dtsets in terms of energy thresholdD nd this n e voided y seletion on these vrilesF xo ut on the zenith nd zimuth ngles re set y defult in risunE ulityF por exmple for the hw vine nlysis presented in ghpter 6 it is neessry to lower the energy threshold s muh s possile then only runs with zenith ngles ≤ 20 • re seletedF

• Meteo he ir humidity levelD the wind speedD loud overgeD nd the temperture in the upper tmosphere re mong the possile uses for degrdtion in the qulity of the oservtions nd then in the reonstrution of the energy nd diretion of the γEry eventsD s lredy 3.3. Standard run selection with H.E.S.S.I 61 explined in 3.1F he lol tempertureD pressureD ir humidity nd the wind speed nd diretion re mesured y meteo sttion loted ner the telesopesF he loud overge on the full sky is monitored y snning rdiometerF hisD omined with mesurements of the wind speedD llows to stop the oservtions nd put the mers in sfe mode efore rin oursF elso eh of the four telesopes of rFiFFFs re equipped with rdiometer tht points t the sme py s the telesopes nd mesures the temperture of the skyD whih is relted to the humidity level nd the loud overge in the pyD lthough they do not mesure the ltitude of the loudsF he defult meteo uts in risunulity re listed in le 3.1F sn prtiulrD sine the verge sky temperture over run should e similr in ll telesope rdiometers the relted qulity riteri @verged temperture nd wA should only e ful(lled y one of the R telesopesF

• Trigger he trigger system of the rFiFFF experiment hs een introdued in ghpter 2F guts re ville in risunulity on oth the individul telesope trigger informtion nd the entrlGsystem trigger for the seletion of stereosopi eventsD nd on the twoEfold ded time frtion etween the triggered events @iFeF the ded time frtion for events triggered y t lest two telesopesAF rigger seletions re useful to remove runs tht present hrdwre prolems @eFgF normlly lrge vlues of the telesope trigger or entrl trigger rtesA nd to omplement the meteo seletions disussed in the previous prgrphF he presene of louds redues the intensity of the shower imges in the mers Y the pixel nd setor thresholds @tht set the trigger for the individul telesopesA eing (xedD the result is n inrese in the energy threshold of the triggered events nd then derese in the trigger rteF elso the louds move ll over the durtion of the run resulting in vritions in the trigger rte Y for this reson vrile lled 4trigger rte stility4 is sved in the dtse for eh run nd is de(ned s the w of the trigger rte over the runF hese issues re prtiulrly dngerous for spetrl reonstrution in rFiFFF s the energy distriutions produed with wonteEgrlo simultions hve (xed energy threshold under stndrd nd stle wether onditionsF elso the oservtion zenith ngle hs strong impt on the energy thresholdD s explined in the 4trking4 setionD nd then on the trigger rteF his issue is fully hndled in wonteE grlo simultionsD with γEry showers eing generted t vrious zenith nglesF xevertheless vrile lled 4orreted trigger rte4 is sved into the dtse nd orresponds to the telesope trigger rte normlized t zenith ngle of 0 • Y this simpli(es the run seletion proess in risunulityD the orreted trigger uts eing then independent of the zenith ngleF his orretion is lso pplied to the entrl trigger rteF sn risunulity it is possile to ut on X E he telesope trigger rte nd w E he zenithEorreted telesope trigger rte E he pixelGsetor threshold E he ded time frtion of single telesope E he PEfold ded time frtion E he zenithEorreted system rte nd w @entrl triggerA Chapitre 3. Improvement of the run quality selection software for H.E.S.S.II analyses elso minimum numer of telesopes tht pss the telesope trigger uts n lso e set in the seletion proessF rowever for stndrd rFiFFFs seletions only the entrl trigger uts re pplied y defultD with zenithEorreted entrl trigger rte etween IHH rz nd THH rz nd PEfold ded time frtion ≤ 20%F ypil individul telesope trigE ger rtes @zenithEorretedA rnge from IHH rz to QHH rzD with ded time frtions elow IH7F

• Electronic calibration -Broken Pixels he qulity of the γEry reonstrution n e spoiled if prts of the shower imges re missing in the rFiFFF mersF elso the determintion of the optil e0ienies n e 'eted RTF his hppens when some of the WTH pixelsGphotomultipliers @wsA in the rFiFFF mers re ded @hrdwreErelted issuesA or 4hot4 @sturtedAF yn the hrdwre level there n e missing high voltge for some pixelsD unEloked enlogue ing mpler @eA for righ qin nd vow qinD d righEvow qin rtio nd righ oltge @rA instilities during the dt tkingF hese prolems n e present for the durtion of single run only @eFgF unloked eA or persist for n entire oservtion period @eFgF missing rA if one or severl ws need to e repledF yn the oservtion level the mount of photoEeletrons in one or severl pixels n e unexpetedly high if the imge of right str is seen in the pyD tht my trigger the overEurrent protetion of individul ws nd use them to e turned o'F his prolem my dispper t the next run if moving to di'erent pyF elso right trnsient ojets suh s shooting strs @meteoritesAD lightningsD irplnes or stellites re not predited nd lso use ws to turn o' during the dt tking up to the end of the runF pinlly for some runs hrdwre prolems suh s omplete mer filing or orrupted mer (le my use the roken pixel frtion of one or severl telesopes to e set to IHH7F sn risunulity ut is ville on the roken pixel frtion of eh individul telesopesD lthough it does not ount for the sptil distriution of the roken pixels in the mersF he defult ut is roken pixel frtion ≤ 15% on t lest Q of the R telesopes of rFiFFFsF Summary table -list of default cuts with H.E.S.S.I le 3.1 shows the impt of eh of these individul defult qulity seletion uts on the totl numer of runs ville with rFiFFFs @R telesope rry onlyAF sn totl out PS7 of the totl numer of runs ville with rFiFFFs re rejeted with defult qulity seletion utsF he orreted entrl trigger rteD wD nd the roken pixel frtion re the most sensitive vriles tht rejet TFI7D IHFI7 nd IHFH7 of the runsD respetivelyF elso sine roken pixels re essentilly hrdwreEreltedD the seletion on the roken pixel frtion is lmost independent of the other qulity seletions @tht re mostly linked to meteorologil ftorsA Y this explins why lrge numer @∼ 10%A of the runs tht pss ll the other seletion uts n e still rejeted fter the roken pixel utF for rFiFFFss runs he mximum numer of telesopes is now set to SD nd it is possile to mke seletions with nd without gS X • riP @require gSA X the run is rejeted if gS is not tking dtF his is wy to selet 4pure4 rFiFFFss runsF • riI @runs without gSA X only runs tken with the gIER telesopes re onsideredF his llows seleting rFiFFFs runsF • wixed riI nd riP X there is no ondition on gSF he run list n mix rFiFFFs nd rFiFFFss dtF his option is useful sine the tereo nlysis lgorithm in risenlysis now performs on suh omined run listsF por gS wono nlysis the informtion of the gIER telesopes is ignored in riE senlysis Y t the run seletion level it is therefore reommended to sk for minimum of I telesope in the dt tkingD to selet 4riP @require gSA4 nd to detivte ll uts spei( to gIERF yn the other hnd for stndrd tereo nlyses @either rFiFFFs or rFiFFFssA minimum of Q telesopes is set y defult to ensure the good reonstrution of the γEry eventsF e seletion pnel hs een reted for utting on the roken pixel frtion in the gS merD independently to the roken pixel seletions with gIERF he gS mer ontins PHRV pixels @wsA nd re sujet to similr prolems t the hrdwre nd oservtion levels s in the gIER mers @see 3.3AF rowever the eletroni signls in the high nd low gin hnnels of the gS ws re smpled into wift enlog wemories insted of e @see 2.2.1A whih mens tht gS nnot e sujet to unEloked e prolemsF sn gIER this usully uses out IHEPH7 of roken pixels in the mersF he distriution of the roken pixel frtions in gS is shown in pigure 3.6D with telesope multipliity ≥ Q required in eh runF he dt tken efore PHIR ws lso rejeted sine gS ws not yet fully opertionl t tht timeD nd enountered severl prolems t the mer hrdwre levelF eout VW7 of the runs disply roken pixel frtions elow IH7 in gSD mostly due to missing drwers in the merF e preliminry defult ut 4roken pixel frtion ≤ S74 ws however de(ned s it hs een soure of gret improvements t the lirtion level for rFiFFFss nlysesD in prtiulr for solving unstle pedestl prolems tht indued lrge positive nd negtive spikes in the exess nd signi(ne mps of soures in the pyF his ut on the gS roken pixel frtion results in loss of out IV7 of the rFiFFFss runsF 3.4.5 CT5 autofocus selection risunulity hs een upgrded with gin seletion pnelD referring to the righ qin @rqA hnnel of the mer ws @see 2.2.1AF guts re pplile on the verged nominl rq in eh mer @gIESAD iFeF the numer of ehg ounts over the pedestl for single photoEeletronD nd on the gin dispersion @wA over the mer pixelsF hese uts re implemented in the glirtion module of risunulityD like the roken pixel utsD s they oth highlight hrdwreErelted prolems suh s missing high voltge @rAD unEloked eD d righEvow qin rtio nd r instilities during the dt tkingF rowever the roken pixel seletions hve the spei(ity of proing the proportion of unusle pixels in the mers tht re responsile for misinterprettion of the shower imgesD while the gin seletions re rther relted to the glol stte of the mers for whih the expeted vlues of the gins hve een lirted eforeF sn gIER the rq is lirted to e ∼VHD however the gins re not stle t the long timeEsle nd it ws neessry to djust the r in eh mer in wy PHIR to get etter homogeneity of the gins round the vlue of VHF por gS the rq ws initilly (xed t RH ut ws inresed to SH fter the r djustment for etter disrimintion of the photoE eletrons over pedestl vluesD resulting in P distint peks in the gS gin distriution over the runs s shown in pigure 3.8F sn prtiulr the gin seletion pnel n e used to rejet runs eforeGfter wy PHIR for the prodution of homogeneous rFiFFFss dtsetsF qin seletions re not tivted y defult in risunulityF Chapitre 3. Improvement of the run quality selection software for H.E.S.S.II analyses 3.4.7 Atmosphere -Transparency coecient Figure QFW ! he trnspreny oe0ient seletion pnel with relted ontrol plots e new tmospheriErelted vrile hs reently een implemented in the run dtseD following to extensive studies done y gF wriudF @vv iole olytehniqueD risAF he ide ws to de(ne oe0ientD lled trnspreny oe0ient @gAD tht desries the tmosphere qulity nd llows improving rFiFFF nlyses t the run seletion levelF sn prtiulr the tmospheri trnspreny dereses during erly summer periods @eugustE ytoerA euse of frequent lnd (resD reduing the qulity of the oservtionsF he g is de(ned for eh telesope nd depends on the zenithEorreted trigger rte @AD the men w high gin over the mer @gA nd the optil e0ieny @µAF he g omplements the sky tempertureD humidity level nd trigger rte seletions lredy implemented in risunulityF he lultion of the g is done ssuming the two following hypotheses X E he minimum detetle imge size in the mer η min is proportionl to the priE mry energy of the prtile t the origin of the showerD whih de(nes the energy threshold E 0 of the experiment t the mer level X η min ∝ E 0 @QFIA E η min is inversely proportionl to the tmospheri sorption ηD the men gin @gA nd the optil e0ieny µ X η min ∝ (η.µ.g) -1 @QFPA he g is proportionl to the tmospheri sorption ηF he energy threshold E 0 n e inferred from the zenithEorreted trigger rte @A tht is given @t the (rst orderA y the lol proton spetrum X

R = ∞ E 0 dEA ef f (E)f (E) = N 0 ∞ E 0 dEA ef f (E)E -2.7 = k.E -1.7 0 @QFQA
where A ef f is the e'etive re of the instrument for protonsF elso orreltion etween nd the optil e0ieny µ ws reently found in the rFiFFF dtD well desried y powerElw funtionF sn onsequene the dependeny of the g with µ ws ounted y orretion ftor pplied diretly on the trigger rteD tht is now orreted for oth the zenith ngle nd the optil e0ienyF e possile orreltion etween nd the men gin g is lso eing investigted ut will not e disussed hereF fy omining 3.4. Adapting ParisRunQuality to H.E.S.S.II analyses 71 equtions 3.1D 3.2 nd 3.3 the expression of the g for the i th telesope is X

t i = R -1.7 cor i g i @QFRA
et the run qulity seletion level it is more onvenient to work with the men vlue of the g over the telesopes in the runD tht tkes into ount the unertinties on the di'erent mesurements dt i F he men g vlue for given run is lso normlized y ftor k n tht depends on the telesope multipliity in the run @nA nd on the telesope on(gurtion @iFeF whether gS is present in the run or notD or whether one of the gIER telesopes is missingAD s t i di'ers for eh telesope nd is in prtiulr signi(ntly lrger for gSF he expression of the men g vlue over single run is then X

< T C >= k n n × i t i dt 2 i i 1 dt 2 i @QFSA
pigure 3.10@DA shows the men g distriution for runs tken with the R telesopes of rFiFFFs @A nd runs tken with ll the S telesopes @AF he peks of the distriutions orrespond to < T C >= 1 s result of the normliztion proess disussed oveF

Summary table & Discussion

he new risunulity qs interfe is shown in pigure 3.14D implemented with ll the new uts nd onvenient tools tht hve een presented in the former setions of the hpterF le 3.2 shows the impt of eh of these individul defult qulity seletion uts on the totl numer of runs ville with rFiFFFss @ll the S telesopesA etween HIGPHIR nd HTGPHISF he dt tken efore PHIR is not onsidered here sine gS ws not yet fully opertionl t tht timeD nd enountered multiple prolems t the mer hrdwre levelF he tle is orgnized suh tht uts relted to gS re pplied (rst @rFiFFFss wono stndrd pro(leA nd then uts relted to gIER @rFiFFFss tereo stndrd pro(leAF he frtion @7A of runs pssing the individul uts re de(ned reltively to the totl numer of runs tken with gS @b PHIRA iFeF totl of PVRU runsF eout QI7 of these runs re rejeted with defult qulity seletion uts spei( to the gS telesopeF he most sensitive uts re the orreted trigger rte nd the roken pixel frtion in gSD tht rejet out IQ7 nd IT7 of the runsD respetivelyF he orreted trigger rte is essentilly tmosphereEreltedD while the roken pixel frtion is mostly ssoited with hrdwre prolemsD tht is why these two uts re together responsile for the rejetion of out PS7 of the rFiFFFss runsF hese results re resonle in the sense tht out PS7 of the rFiFFFs runs were rejeted fter defult seleE tions with the former version of the risunulity softwreD s it hs een disussed in 3.3F yn the other hnd some of the stndrd uts pplied on gIER @whih were initilly de(ned for rFiFFFs run seletionsA hve een revisited in the ontext of the rFiFFFss nlysesF he telesope ded time frtion in gIER tully inresed t the eginning of the seond phse of rFiFFF euse of the instlltion of gS in the glol trigger systemF his n e seen in pigure 3.15 where the distriution of the ded time frtions hs een shifted y out CS7 with rFiFFFssF yn the other side the roken pixel frtion in the gIER mers hs lso inresed y out S7D thus showing degrdtion t the hrdwre level over the yersF sn onsequene these uts hve een relxed y S7 in stndrd rFiFFFss seletions in order to void unexpetedly lrge run rejetionF sn the end out RU7 of the rFiFFFss runs do not pss the stndrd seletions when pplying defult qulity uts on oth gIER nd gS vriles @rFiFFFss tereo seletion pro(leAF uh lrge rejetion mostly results from the roken pixel frtions tht re independent in the gIER nd gS mers @s they re essentilly hrdwreEreltedAF elso IQFS7 of the runs hve een tken with less thn Q telesopes nd re then rejeted in the tereo seletion proessF en upgrde is urrently eing rought to the gIER mers y repling the IHE yers old onEord eletronis with modernEdy tehnologies @eFgF fster eletronisAD in order to redue the ded time frtion in the telesopes nd t the entrl trigger levelD nd to lso inrese the stility of the mer opertions during the dt tking @tht will ertinly result in lower roken pixel frtionsAF he gI mer upgrde is lredy t n dvned level while the full gIER upgrde is expeted y the end of PHITF nlyses @ll the S telesopesAF he seond olumn shows the numer of runs tht pss the orresponding ut in the (rst olumnD with respet to the totl numer of rFiFFFss runs tken etween HIGPHIR nd HTGPHIS @tht inlude gSAF he third olumn shows the numer of runs tht pss the orresponding ut nd lso ll the uts present in the previous lines of the tleF guts relted to gS re pplied (rst @rFiFFFss wono stndrd pro(leA nd then uts relted to gIER @rFiFFFss tereo stndrd pro(leA 3.5 Conclusions un seletions re mndtory efore ny physis nlysis in rFiFFF for voiding ontmiE ntion of the results y internl @mostly hrdwreA nd externl @meteoD tmosphere qulityA ftors tht n e responsile for inurte reonstrution of the energy nd diretion of the primry γEry events nd their misidenti(tion with osmiEry kground eventsD introduing lrge systemtis in spetrl reonstrutionsF he risunulity softwre reds the run informtion from the dtse nd genertes run lists for given soure fter following qulity seletion proess sed on individul qulity riteri de(ned for eh individul telesope nd on the generl stte of the rryD inluding the qulity of the tmosphereF he im of the presented work ws to dpt the risunulity softwre to the use of the new ig telesope gSD presented s high interest tsk in rFiFFF experimentF he uts tht were previously de(ned in the (rst phse of rFiFFF hve een restrined to the gIER telesopes onlyD nd new uts hve een implemented on gS suh s independent triggerD roken pixel nd utofous seletion modulesF elso uts on the verge high gin t the lirtion level nd on the tmosphere trnspreny hve een dded for reinforing the lredy existing seletionsF hefult ut vlues hve een set up in these new seletion modulesD while some of the previous uts hve een revised for gIERF hey re summrized in le 3.2F pinlly for more onvenieneD defult pro(les re ville in the grphil interfe for simple nd quik run list prodution depending on the hosen telesope on(guE rtion @rFiFFFsD rFiFFFss wonoD rFiFFFss tereoD FFFAF e text (le ontining informtion on the rejeted runs n lso e generted for helping the user in the ut optimiztion proessF he de(ned uts on gS led to the rejetion of out PS7 of the totl numer of runs tken with rFiFFFss etween HIGPHIR nd HTGPHISD similr to wht ws otined in the pst with the uts on the gIER telesopesF por the moment rFiFFFss wonosopi nlysis @gS onlyA re predominnt in the gollortion nd then ene(t from these new qulity seletionsF por tereosopi nlyses the defult uts in le 3.2 my e too strong nd ould e relxed in the futureF sn prtiulrD there is room for improvement for the optimiztion of these new run qulity seletionsD following the lrge progresses mde sine PHIP on the ommissioning nd understnding of the gS telesope for whih the performnes will ertinly ontinue to improve in the next yersF sn this hpterD the stndrd nlysis proedure for the detetion of n exess over kE ground in rFiFFF oservtions is desriedD relying on the de(nition of signl @yxA nd kground @yppA regions in the (eld of viewF sn setion 4.2 the method is pplied to stndrd γEry strophysil soures ri tIURIEQHP nd u PISSEQHRD with stndrd spetrl reonstrution of the yxEypp exessF hen in setion 4.3 the yxEypp nlysis is performed on the gittrius hwrf qlxy looking for potentil hrk wtter exessD where no strophysil γEry ontriution is expetedF Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection 4.1 Standard ON-OFF analysis 4.1.1 Principle he stndrd proedure for rFiFFF dt nlysis is sed on yxEypp sutrtionF st is prt of ll nlyses performed with smging etmospheri gherenkov elesopes on the strophysil souresF he min ide is to de(ne sptil region of interest @eFgF irulr region of ngulr extension θA round the nlysed soure positionD lled 4yx4 regionF fkground 4ypp4 regions re then de(ned round the yx region in the ville (eld of view @pyA or in nother py exempt from known souresD used to estimte the kground frtion in the nlysis regionF he numer of kground events overed y the ypp regions is normlized regrding to the surfe of the yx region nd is then sutrted from the yx eventsF he remining numer of events onstitutes the signl exessF he de(nition of the kground regions is losely relted to the oservtion ondiE tions of the studied soureF sn prtiulr it is dngerous to de(ne yx nd ypp regions in the sme py if the rFiFFF telesopes point diretly t the soure position X he oservtion onditions of the soure @yxA nd kground @yppA regions re not the sme euse these regions re loted t di'erent ngulr distnes from the pointed positionD introduing ises in the nlysisF his is due to the py eptne of the experiment tht flls down with respet to this ngulr distne for given oservtion runF xevertheless eptne orretions re done to minimize this e'etF e solution to tht prolem is otined in reonsidering telesope oservtion onditionsF snsted of pointing the telesopes diretly t n strophysil soure or other region of interestD n o'set is introdued etween the pointed position nd the soureF his is lled 4wole4 oservtionD or oservtion in wole modeF sn tht on(gurtion yx nd ypp regions n e de(ned with similr oservtion onditionsD this will e desried in 4.1.2F yn the other hnd the sptil limits of the py @round S • with rFiFFFs nd Q • with the Sth telesope onlyA is lso onstrint for the de(nition of the ypp regionsD espeilly in the se of n extended soure tht requires lrge yx nlysis regionD or when there is n extended γEry emission in the neighourhood of the soure @eFgF di'use emissionAF sn tht se it ould e more pro(tle to onsider ypp regions in di'erent pyD using yxGypp run pirs of similr oservtion onditionsF his yxEypp pproh is desried in 4.

N excess = N ON -N OF F /α @RFIA where X α = OF F A γ OF F (φ x , φ y , φ z , E, t)dφ x dφ y dφ z dEdt ON A γ ON (φ x , φ y , φ z , E, t)dφ x dφ y dφ z dEdt @RFPA
is the generl expression of the normlistion ftor of the e'etive oservtion times in the yx nd ypp regionsF A γ ON,OF F is the γEry eptne of the detetorD φ x,y the ngulr oordintes in the frme of referene of the pointing position of the telesopesD φ z the zenith ngleD i the energy of γErys nd t the time of exposureF ine yx nd ypp eptnes nd times of exposure re Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection the sme in the o'set on(gurtionD α is just the rtio of the yx nd ypp ngulr surfes X α = surfe of the ypp regions surfe of the yx region @RFQA he yxEypp wole nlysis is prtiulrly e0ient for soure of smll extension @eFgF pointElike souresA s ypp regions over wider ngle round the pointing position t given wole o'setD thus inresing kground homogeneity nd providing more urte estimtion of the kground omponent in the nlysis regionF

MultipleOFF and Ringbackground congurations here re vrious wys of de(ning the shpe of the ypp regionsF 4wultipleypp4 nd 4ingfkground4 re the min ypp on(gurtions in useD represented on pigure 4.1F he wultipleypp kground @A is omposed of severl irulr ypp regions with the sme rdius s the yx region nd distriuted round the pointing position on oth sides of the yx regionF sn tht se X α = numer of ypp regions @RFRA en lterntive on(gurtion lled 4ingfkground4 @A onsiders single ypp kE ground ring insted of severl irulr ypp regionsF he surfe of the ypp ring is overing lrger re thn the irulr ypp regionsD inluding more kground @efore normliztion y αA nd then reduing kground sttistil )ututionsF yn the other hnd α is then not nymore inditive of the numer of kground regions @whih n e less onvenientAF foth methods give in priniple similr resultsD it n lso e interesting to pply oth wultipleypp nd ingfkground nd see orresponding e'et on the numer of exess events nd signi(neD thus proing sttistil )ututions in the kground estimtionF Exclusion regions sn dditionD exlusion regions n e de(ned round known strophysil soures tht re loted lose to the oserved soure to void their ontriution into the kground lultionF ointElike soures @glti or extrgltiA re usully msked with irulr regions of extension slightly lrger tht the ngulr resolution of the instrumentD while the qlti gentre region is very tive nd ontins extended strophysil emissions suh s glti di'use emissionD often exluded from the kground lultion y msking the entire glti plneF hen the ypp regions re de(ned in the remining spe of the py tht does not interfere with the exluded regionsF sully n dditionl exlusion region @stndrd extension 0.25 • A is lso de(ned round the yx region itself to void lekge from the studied soure into the ypp regions @eFgF if the yx region is too smllAF en exmple of the yxEypp wultipleypp nd ingfkground proedure with exlusion regions is given in pigure 4.2D with one exlusion region round the yx region nd one round n hypothetil known strophysil soure in the pyF he ingfkground on(gurtion is lso more likely to e used in omintion with exlusion regions X irulr ypp region from wultipleypp tht interferes prtilly with n exlusion region is ignored from the kground lultionD leving unused spe in the pyF hile with the ingfkground method these remining spes ner the exlusion regions ontriuteD s seen on pigure 4.2F por very extended soures the ypp kground regions n not e de(ned in the sme pyF pirstD yx oservtion run is tken without ny wole o'set t the position of the soureD then n ssoited ypp run is tken in nery region where no strophysil γEry soure is expetedD with similr oservtion onditions @eFgF zenith ngleA nd with similr kground environment @eFgF night sky kground levelAF his nlysis on(gurtion is presented on pigure 4.5F

ypilly the yx nd ypp regions re seprted y n ngulr distne of ∼ 7 • @QH minutes intervl t lestD orresponding to the hrteristi durtion of runAF yservtion onditions re similr etween yx nd ypp regions exept for temporl vritions of the eptne nd possile kground )ututions oming from the oservtion of two di'erent pysD thus introduing systemtis in the yxEypp sutrtionF his method is lso e0ient if too mny exlusion regions re de(ned in the yx py @eFgF too mny strophysil souresAF pinlly with yxGypp pirs there is no need of introduing wole o'set etween the pointing position of the telesopes nd the entre of the soureD thus providing single oservtion strtegy for ll runs @while in wole mode oservtions re mde with di'erent wole o'set vlues nd ngulr distnesAF ynly oservtions in wole mode will e onsidered in this thesisF he stndrd vi&w method IIW is pplied for the lultion of the signi(ne of the oserved yxEypp exessF sn this se the generl formul for the signi(ne is given y the expression X

N σ = √ -2lnλ @RFTA with λ = α 1 + α . N ON + N OF F N ON N ON × 1 1 + α . N ON + N OF F N OF F N OF F @RFUA
where N ON nd N OF F re respetively the numer of events in the yx nd ypp regionsD nd α the normliztion ftor etween yx nd ypp regionsF sn the prtiulr se of α lose to ID eFgF when using the yxGypp pir pprohD the signi(ne n e pproximted y

N σ = N ON -αN OF F α(N ON + N OF F ) @RFVA
ypillyD vlue N σ ≥ 3 represents hint for soureGexess detetionD while N σ ≥ 5 is required for disoveryD used s referene vlue in prtile physis nd in strophysil oservtionsF pive sigm refers to detetion t more thn WWFW7 on(dene levelF st lso mens tht the deteted signl would e the result of sttistil )ututions s unexpeE tedly s quntity simulted from qussin distriution would e (ve stndrd devitions from the menF smportnt study of ll the existing systemtis when extrting the signl is requiredD s they hve to e tken into ount in the (nl signi(ne lultion efore lim for disoveryF 4.2 Analysis of astrophysical sources sn this setion two exmples of strophysil soure nlysis re desriedD using the stndrd yxEypp method for reonstruting the exess signl with ssoited signi(neF elso the strophysil properties of the two soures @eFgF the spetrl prmetersA re derived from their reonstruted energy spetrF he (rst one @4.2.2A is the unidenti(ed soure ri tIURIEQHP loted ner the qE lti gentreF he stndrd yxEypp nlysis of ri tIURIEQHP is done with the prenh rFiFFF softwre in the ontext of rossEhek nlysis done for iF yF engüner @rumoldt niversityD ferlinA using the four telesopes of rFiFFFsD with the prospets of future pulition on the strophysil properties of the soureF fut the min interests for the soure re here relted to the serh for the hrk wtterD its position eing oinident with the region of interest de(ned for the hw vine nlysis done in ghpter 6 Y its impt hs to e investigted in reltion to IQH qe lineElike feture reported in the permiEve dt t tht sme lotion ITPF sn prtiulr the )ux of the soure shown in this setion will e lter extrpolted down to IQH qe to evlute its impt on the vine nlysis @6.3AF he seond soure @4.2.3A is u PISSEQHRD wellEknown lzr @extrgltiA tht is used s lirtion soure in rFiFFF he yxEypp nlysis of this pointElike soure is done using the full potentil of the (ve telesopes @rFiFFFssAF his soure is lso of lrge interest for the hw vine studies done in ghpter 6 Y in prtiulr it is used for heking the proper working of the γEry event reonstrution lgorithm in rFiFFFss efore performing hw nlysesD nd ws the ojet of lrge numer of tests over the lst two yers for deugging nd improving the performnes of the rFiFFF nlysis softwre with the gS telesopeF elso mjor ontriution of u PISSEQHR in the hw vine nlysis is the possile use of ypp wole regions round the pointElike soure s kground model whih is not s omplex s in the region of the qlti gentreF sn further studies this senrio is (nlly disfvoured @see 6.8.2.1AF 4.2.1 Spectral analysis in H.E.S.S.

he energy spetrum is used to hrterise the strophysil properties of soure nd orresponds to its intrinsi energy distriutionD expressed s )ux in γ.cm -2 .s -1 .T eV -1 F wesured energy distriutions re not representtive of the intrinsi spetrum s they re shped y the response of the instrumentF sn prtiulr the numer of reonstruted γEry events is relted to the rFiFFF eptne tht is funtion of the true energyD the oservtion zenith ngleD the wole o'set nd the optil e0ieny of the system @onversion of the numer of deteted photoEeletrons into numer of gherenkov photonsAF elso the energy is @systemti shift etween the true nd the reonstruted energies of the γEry eventsA nd the energy resolution @sttistil unertinty on the energy mesurementA 'et the reonstrution of the γEry events resulting in energy distriutions produed in terms of the reonstruted energyF por those resons spetrl reonstrution methods hve een developed in rFiFFF 90 Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection he (rst pproh onsists in deonvoluting the energy distriution of the yxEypp exess events y the response funtions of the instrument @eptneD energy is nd energy distriution otined from full simultions of γEry showers nd of the struture of the detetorA to get the true energy distriution of the γEry soureF e spetrl model @eFgF powerElwA is (tted on top of tht reonstruted spetrumF he seond methodD implemented in the prenh rFiFFF softwreD relies on preise omprison etween the expeted nd the oserved numer of events in four dimensionl ins of energyD zenith ngleD wole o'set nd optil e0ienyD using logElikelihood (t @see ghpter 5 for the presenttion of the vikelihood formlismAF rere no sutrtion is done etween the yx nd ypp event distriutionsF en ssumption is mde on the spetrl model of the soure tht is onvoluted with the response funtions to mth the mesured dt distriutionF he proess is iterted vrying the initil spetrl model prmeters then minimizing the logElikelihood funtion to get the estE(t spetrl prmetersF rere is list of ommon spetrl models for strophysil soures X

• owerElw spetrum X dΦ dE = Φ 0 E E 0 -Γ @RFWA • gurved powerElw spetrum X dΦ dE = Φ 0 E E 0 -Γ-β×ln(E/E 0 ) @RFIHA
• owerElw with exponentil uto' X

dΦ dE = Φ 0 E E 0 × exp -E E cut @RFIIA
where Φ 0 is the referene )ux t the energy E 0 expressed in γ.cm -2 .s -1 .T eV -1 D Γ the powerE lw indexD β the urvture oe0ient nd E cut the utEo' energy vlueF he reonstruted spetrum @)uxA is plotted s funtion of the true energy with unertinties @ontoursA t TV7 on(dene levelF 4ixperimentl4 dt points with error rs re derived from the (t @while with the (rst method the (t is derived from the experimentl dt pointsA nd residuls re lulted orresponding to the rtio etween the expeted nd the mesured numer of γEry events in eh energy inD for the estE(t spetrl modelF wost reent studies done y iF yF engüner @rumoldt niversityD ferlinA hve de(ned two unequl ounterprts in ri tIURIEQHP Y min γEry extended soure nd weker pointE like soureF he eEhe oordintes of the two ounterprts re given in le 4.1F e rFiFFFs nlysis ws performed with the qermn softwre @reA with we γEry reonstrution lgorithm @hrd utsA nd wultipleypp kground on(gurtion to derive the signi(ne of the exess signl nd the reonstruted spetrum of the soureF he pointE like ounterprt of ri tIURIEQHP ws not inluded in the nlysisF he results re presented in le 4. generted with the risrunqulity softwre @see ghpter 3A using stndrd run qulity seletion riteriF st orresponds to totl livetime of IVSFW hoursF he yx region is irle entred on the min soure @e X 265.322 • D he X -30.369 • A nd of extension θ ON = 0.15 • whih is the estimted extension of the soure on the sky mpsF he pointElike ounterprt of ri tIURIEQHP ws not inluded @s for the reEwe nlysisAF he exess nd signi(ne sky mps re presented in pigure 4.9D s well s the signi(ne distriution over the pyF he numer of exess events in the yx region nd ssoited signi(ne were omputed using the wultipleypp kground on(gurtionF ixlusion regions were lso de(ned round γEry strophysil soures tht re referened in the qlti gentre regionF he mp of the exlusion regions is shown in pigure 4.10F

he nlysis results re presented in le 4.2 @third olumnAD in omprison to the reEwe resultsF elso (gure 4.11 shows the ngulr distriution of the events in the pyD entred on the position of the soureF he yx region orresponds to the (rst U ins in θ 2 F he glti di'use emission is responsile for the remining exess seen in the θ 2 distriution t lrger nglesF e signi(ne of 7.9σ ws foundD orresponding to signlEtoEkground rtio of S/B = 0.20F ery similr results were otined using the lterntive ingkground on(gurtion for the ypp regions disussed in 4. u PISSEQHR is fv verte @fv vA type of etive qlti xulei @eqxA tht presents extremely vrile γEry emissionF voted t redshift z = 0.117 it hs een disovered y the wrk T telesope SR nd ws one of the (rst soures deteted y rFiFFF in PHHQ IRF sts vrile γEry emission ws frequently oserved etween PHHP nd PHIS with rFiFFFs nd more reently with the (fth telesope @gSA IRUF sn prtiulr u PISSEQHR showed unpreedented )ux levels with strong vriility during the summer PHHTD enling temporl nd spetrl vriility studies on timesles of the order of few minutesF he very high energy emission from the soure is thought to e linked with reltivisti jet emnting from the viinity of supermssive lk holeD lthough the ssoited strophysil proesses re not well understoodF 4.2.3.1 Data quality, run selection and cuts sn this setion the γEry emission of u PISSEQHR is investigted in its low stte of vriE ilityD lled quiesent stteD with oservtion runs tken in PHIQ with the (ve telesopes of rFiFFFssF his dtset hs een used to investigte the qulity of the γEry reonstrution lgorithm efore performing the hw vine nlysis presented in ghpter 6D nd ontriuted to the reent softwre improvements tht re disussed in 6.11F elso the distriution of the ypp kground events round u PISSEQHR hs een onsidered s possile senrio for the modelling of the kground distriution in the qlti gentre regionD disussed in 6.8.2.1 Y in prtiulr oth u PISSEQHR nd the qlti gentre n e oserE ved under low zenith ngles @`20 • A then t the lowest possile energy threshold with rFiFFF rere the stndrd yxEypp nlysis results t the position of the pointElike soure re givenD for oth the rFiFFFss wono @gS loneA nd rFiFFFss tereo @t lest P telesE opes in the triggerA telesope on(gurtionsF he nlysis ws performed with the prenh rFiFFF oftwre @risnlysisA using the wodelCC lgorithm for the reonstrution of the γEry eventsF e set of 4stndrd4 uts were used for the seletion of the γEry eventsD tht hd een optimized y the rFiFFF 4enlysis nd eonstrution4 working group for ringing the highest signi(ne from strong pointElike souresF he uts re di'erent for the wono nd the tereo on(gurtionsD in prtiulr the optiml size for the yx region is 0.173 • @θ 2 ON = 0.03 •2 A in wono nd 0.1 • @θ 2 ON = 0.01 •2 A in tereoD whih ounts for di'erenes in ngulr resolutionsF he yx region is entred on the nominl position of the soure @e X 329.717 • D he X -30.226 • AF he run list onsists in SI runs tht pss the stndrd tereo run qulity seletion uts de(ned in ghpter 3 within the risrunqulity run seletion softwreD with t lest Q telesopes required in the triggerD inluding gSF st orresponds to totl livetime of PHFV hours in wono nd ITFU hours in tereoD the livetime eing de(ned s the totl oservtion time minus the dedtime etween the triggered eventsD tht di'ers when triggering with gS only or with more thn P telesopes @tht is more restritiveD resulting in shorter livetimeAF he dt ws tken with low zenith ngles @`20 • A to set the energy threshold s low s possile @this is importnt in the ontext of the hw vine nlysisAF

Results -Mono and Stereo

he exess mpsD signi(ne mps nd signi(ne distriutions over the py re presented in pigure 4.13 for oth rFiFFFss wono @left olumnA nd tereo @right olumnA on(guE rtionsF he numer of exess events in the yx region nd ssoited signi(ne were omputed using the wultipleypp kground on(gurtion @4.1.2AF xo other strophysil soures re expeted in the pyD then no exlusion regions were de(nedF he nlysis results re presented in le 4.3F pigure 4.14 shows the ngulr distriution of the events in the pyD entred on the position of the soureF he yx region orresponds to the (rst IV ins in θ 2 in wono nd the (rst T ins in tereo modeF he evolution of the signi(ne with respet to the oservtion time is lso shown nd is omptile with n evolution in √ timeD s expetedF he soure is oserved with signi(ne of 24.3σ in wono nd 40.4σ in tereoD orresponE ding to signlEtoEkground rtios of S/B = 0.26 nd S/B = 2.02D respetivelyF he results otined with the lterntive ingkground on(gurtion for the ypp regions gve very with rFiFFFs U in the quiesent stte of u PISSEQHR reported detetion t 60.5σ with RVFI hours of livetime using dt tken etween PHHS nd PHHUD tht trnsltes into ∼ 36σ when resling to the ITFU hours of livetime used for the rFiFFFss stereo nlysis @in whih signi(ne of 40.4σ ws foundAF elso with the use of the (fth telesope of rFiFFFss gmmElike events now strt to show up t out UH qe in wono nd VH qe in tereo on(gurtionsD while ∼ IHH qe for low zenith oservtions with rFiFFFsF 4.2.3.3 Spectral reconstruction he tereo spetrl reonstrution lgorithm ws not opertionl t the time of this nlysisD however the wono spetrl reonstrution ws working properly nd the results re shown in pigure 4.15F he u PISSEQHR spetrum in its quiesent stte is well (tted y powerElw funtion of spetrl index Γ = 3.389 ± 0.099 stat F his result is omptile with the spetrl indexes pulished in PHHS IR @3.37 ± 0.07 stat ± 0.10 syst AD in PHIH U @3.53 ± 0.06 stat A nd in PHIS IRV @3.25 ± 0.08 stat AF elso the use of the new ig telesope rings the energy threshold for the reonstruted spetrum down to IHH qeD while PHH qe with rFiFFFsF he presented results show very good potentil of rFiFFFss for the nlyses of sE trophysil soures in IHH qe rnge in energyF he nlysis of SI runs tken t the position of u PISSEQHRD seleted with strit qulity riteri nd low zenith ngleD led to reonstrution of the γEry signl from the soure t RHσ levelD with improved performnes with the (fth telesope ringing the rFiFFFss sensitivity to γErys down to UH qe in wono on(gurtion nd down to VH qe with the full telesope rry @tereoAF he energy spetrum ws reonstruted down to IHH qe using powerElw model with spetrl index Γ = 3.389 ± 0.099 stat D well omptile with former pulitionsF u PISSEQHRD s well s the gr xeul nd the lzr q ISSQCIIQD re urrently the min lirtion soures used in rFiFFF for testing nd improving the performnes of the γEry reonstrution softwreF rowever the gr xeul nd q ISSQEIIQ re only oservle with lrge zenith nglesD ove 45 • nd 35 • D respetivelyF his mkes u PISSEQHR very good nd relile ndidte for testing nlysis proeduresD when nlysing dt t the lowest energiesF his is the se for the hw vine nlysis presented in ghpter 6 where the serh energy window extends from VH qe to Q eF sn this ontext the present nlysis of u PISSEQHR ws performed severl times over the lst P yers to ensure the good reonstrution of the γEry events t eh mjor step of the evolution of the rFiFFF nlysis softwreD sine the ommissioning of the (fth telesopeF sn prtiulr normliztion prolems were found etween the numer of events in the yx nd ypp regionsD tht were responsile for lrge exesses found elow PHH qe in reE gions of the sky where no strophysil signls re expeted @disussed lter in 6.5.4 nd 6.11AF

pinllyD the use of ypp events from the nlysis of u PISSEQHR were onsidered s privileged senrio for the modelling of the kground omponent in the qlti gentre regionD in the ontext of the hw vine serh presented in ghpter 6F foth u PISSEQHR nd the qg re oserved t low zenith ngles @`PH • A resulting in similr energy thresholdsF elso the hrged osmiErys produed in the qlxy represent one prt of the di'use kground whose )ux my e mesured lose to u PISSEQHRF his is disussed in detils in 6.8.2.1F rowever this senrio ws (nlly exluded due to the too lrge di'erene in night sky kground @xfA levels nd the presene of the strophysil di'use emission long the qlti plneD not existing in the u PISSEQHR dt smpleF sn se of the extrtion of hrk wtter @hwA signlD the yx region is de(ned on potentil hw region of interest ssuming tht most of the hw hlo signl is inluded in the nlysis region nd knowing the possile ontriutions from the strophysil soures loted nerGin the yx regionF sn se of hwrf qlxies @ddressed in this setionA no strophysil γEry signl is expetedD nd n exess oserved from yxEypp nlysis my diretly e relted to the hw nnihiltion signlD or n unknown strophysil soure on the lineEofEsightF por study lose to the qlti gentreD exlusion regions ndGor knowledge of the surrounE ding strophysil soures nd di'use emission ontriutions re required for interpreting potentil exess in the dtF iither wole or ypp pirs nlysis ould e onsidered for suh omplex studyF roweverD with simple omprison of the numer of events in the yx nd ypp reE gions @nd ssoited signi(neA it is not possile to investigte the deep nture of the potentil exessD unless the stndrd spetrl nlysis @presented in 4.2.1A is used in the mentime to detet hrteristi hw fetures in the spetrum @this pplies to strong yxEypp exessesAF xevertheless in se of no exess oservedD limits on the hw γEry )uxGnnihiltion rossEsetion n e set t given on(dene levelD onstrining hw models Y this will e done here with the study of the gittrius hwrf qlxyF enother vet of the yxEypp method is to fe possile prtil sutrtion of the investigted signl tht ould lso e present in the ypp regionsF hese importnt points will e further developed in the vine serh nlysis @ghpter 6AF

Dwarf Spheroidal Galaxies

hwrf pheroidl @dphA qlxies re prtiulr lss of low luminosity nd lmost spheroidl nery glxies oriting round the wilky y or round the endromed qlxy @wQIAF he (rst of themD the ulptor dphD ws deteted in IWQU from the visul inspetion of photogrphi pltesF his tehnique ws lso used for the disovery of dph ll long the PHth entury nd up to IWWH with the disovery of the extns hwrf qlxy IHID nd y PHHT out dozen of 4lssil4 dph glxies hd een identi(edD inluding the gittrius hwrf qlxyF hey re represented in QhEmp in pigure 4.16F hph qlxies re hrterized y lrge mesured mssEtoElight rtio @S `M/L `IHH for the lssil dph IPQWPA tht ould e ttriuted to the presene of the hrk wtterD s sme s for the norml glxiesF sn prtiulrD the ΛEghw osmologil model predits the formtion of smll stellite hw strutures hosted y lrger hw hlos Y it hs een proposed tht dph qlxies my hve formed within suh suEhlo strutures inluded in the lrger wilky y hw hlo IIQF fy PHIS more thn QH new ultr fint dph glxies @phA were identi(ed with moE dern oservtories nd espeilly with the lon higitl ky urvey ITT nd the hrk inergy urvey IHWD tht my e the key for understnding the very lrge numer of hw hlos in the vol qroup predited y the ΛEghw modelD not explinle with the tul numer of deteted lssil dphF hese ph glxies re n extension of the lssil dph t lower luminosities @ EV mgnitudeA omprle to the luminosity of qloulr glustersD however they disply very lrge mssEtoElight rtios @M/L b IHHA even when underEestimting the veloity dispersions of their str omponents IIHD mking them exellent ndidtes for the serh for the hwF es n exmple γEry exess @b QFUσA hs een reently reported in the study of the etiulum ss ph qlxy with the permiEve dtD onsistent with nnihilting hw for msses elow few hundreds of qe VWF pigure 4.17 shows the distriutions of the mssEtoElight rtio with respet to the E solute mgnitude for ll hwrf qlxies deteted efore PHII @not limited to the spheroidl onesAF hen pigure 4.18 represents the luminosity distriution of these hwrf glxies inluding the most reent deteted phD the nine ltest deteted ph eing shown in red IHWF he seprtion etween hwrf qlxies nd gloulr lusters is lerly visileF

Example of Dark Matter analysis : Sagittarius Dwarf Galaxy with H.E.S.S.I 105

he position of the gittrius hwrf qlxy is lso inditedF prom these plots the most promising fint ndidte for hw serhes would e egue s dphD studied y permiEve THD weqsg PR nd erits PT @not oservle with rFiFFFAD while gittrius hwrf is rther loted t modest mssEtoElight rtioF he mssEtoElight rtio of grh is not fully onstrined yet ut reent rdil veloity disperE sion mesurements report vlue M/L = 9.1 @ggi et lFD PHHR ITUAF his hwEdominted system nonetheless shows high levels of tidl disruption used y its proximity with the wilky y VTF he dph hs een estimted to orit our qlxy within period of less thn illion yers @WWDIRHA @rdil veloity ∼ 140 km.s -1 A nd onsequently should 108 Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection hve pssed through the qlti lne t lest IH times in its historyF rowever over suh long time the oserved high level of tidl fores etween grh nd the wilky y should hve lredy used the omplete disruption of grhF his rings prtiulr interest for indiret hw serhes in this dph @in ddition to mssEtoElight mesurements ITUA s onentrted hw hlo emring grh ould e responsile for its stility nd to mke it hold on for so mny yers IHHF grh hs een regulrly oserved y rFiFFF etween PHHT nd PHIP nd ws the ojet of pulitions in PHHU ISD in PHII IRID in PHIQ IIS nd PHIR TQ with no ri γEry signl foundF gonsequently limits on the γEry )ux nd on the veloityEweighted nnihiltion rossEsetion of the hw prtile were derived for gontinuous hw nnihilting model @see ghpter 1A with msses rnging from PHH qe to IHH eF he work reported in this setion ws done in PHIQ in prllel to the work from qF vmnn et lF IIS for whih s hve een redited s orresponding uthorF he nlysis of ∼ 60 hours of dt tken etween PHHT nd PHIP ws done independently using the risnlysis softwre nd with striter dt qulity seletion utsAF he yxEypp sutrtion method in wole mode @RFIFPA ws used for deling with the osmiEry kgroundF he nlysis steps nd the results of this study re presented in the next setionsF he nlysis of grh ws performed with the wodelCC lgorithm of the risnlysis softwre for the reonstrution of the γEry eventsD with the use of stndrd uts de(ned for the nlysis of pointElike souresF his orresponds to n nlysis region entred on the soure nd of extension θ ROI = 0.1 • F he hw hlo is expeted to extend outside the nlysis region Y nevertheless most of the hw hlo models present n inresing density pro(le when pprohing the entreD nd then pointElike nlysis region entred t the nominl position of grh should ontin most of the density from the host hw hloF he sptil extension of grh @∼ 10 • on the skyA is not importnt here s no γEry strophysil emission is expetedF elso in this senrio frtion of the ypp kground events ould e ttriuted to the hwD however its impt in the lultion of the yxEypp exess signl ws not investigted in the frme of this nlysisF e totl of QIQ runs re villeD tken in severl periods etween PHHT nd PHIP t the position of the grh with the rFiFFFs telesopesF hese runs were tken under vrious oservtion onditions through the di'erent time periodsD eFgF with zenith ngles rnging etween 5 • nd 50 • D vrious tmospheri onditions @humidityD sky tempertureA nd optil e0ienies tht hve degrded y out PH7 etween PHHT nd PHIH @see 2.2.3.2AF his long period of oservtion leds to n inhomogeneous smpleD soure of possile systemti e'ets in the γEry reonstrutionF ht qulity seletion uts were pplied using the risrunqulity softwre @see ghpter 3A in order to get uniform dtsetD rejet suspiious runs nd then ensuring the good reonstrution of the γEry eventsF le 4.4 lists the qulity seletion uts tht were pplied to the grh dtsetF sn prtiulr ll the R telesopes were required in the dt tking to ensure good stereosopi reonstrution of the diretion nd energy of the reonstruted γErysF elso runs with full PV minutes of durtion were onsidered to void prolems tht used the interruption of the oservtionsF uns with men zenith ngles ove 30 • were lso disrded to lower the energy threshold nd serh for hw signl in lrger energy windowF tndrd uts @see ghpter 3A were (nlly pplied on the entrl trigger rteD the PEfold dedtime frtion @4PEfold4 mens γEry events tht hve een seen in t lest P telesopesAD the roken pixel frtion @fulty photomultipliers in the mersA nd the rdiometer temperture @tht indites the temperture of the sky during the dt tkingD orrelted with the trigger rte nd 'eted y loud overge or the humidity levelAF efter qulity seletion uts list of IRP runs ws otined for the nlysis of grhD orresponding to TIFT hours of livetimeF he yx region is irle entred t the nominl position of grh @e X 283.775 • D he X -30.48 • A nd of extension θ ON = 0.1 • F he de(nition of the nominl position is sed on photometri mesurements of grh showing tht the position of the entre oinides with the entre of the gloulr luster wSR IPWF he numer of exess events in the yx region nd ssoited signi(ne were omputed using the wultipleypp kground on(gurtion desried in 4.1.2F xo strophysil signl is expeted ner grh then no exlusion regions were de(ned in the py for the de(nition of the ypp regionsF pinllyD we deided the perform the dt nlysis using set of uts on the )utution of the kground @< 3σAD however there re rguments tht go into fvour of the existene of n strophysil soure or hw hlo X

• he exess is stle with respet to the softwre versionF he present nlysis is done with the ltest version of the rFiFFFs softwre @updtes relted to rFiFFFss re present in di'erent softwre versionAF his version inludes mjor updte on pointing orretions for the oserved souresD s well s improved lirtion of the instrumentF ith the former version of the softwre the sme exess showed up ove QHH qe with signi(ne of 2.3σ nd then rehed 3.5σ ove SHH qeD ut the hotspot ws shifted y out 0.1 • from the nominl position of grhF his is shown on pigure 4.23F ith the new pointing orretions the exess now lies t the ext nominl position of grhD whih goes in fvour of genuine γEry signlF

• he lk of exess events elow QHH qe redues the glol exess signi(ne tht is lulted on the whole rnge in energyD whih ould explin why no exess signl is oserved when no energy ut is ppliedF

• he signi(ne of the exess inreses with the ut in energyD this eing proper to the nlysis of pointElike strophysil soures @the performnes for the reonstrution nd disrimintion etween the γErys nd hdrons improve with respet to the energyAF sn prtiulr this my imply the existene of wek pointElike soure in the pointing diretion of the grh glxyD lthough not prole to elong to grh @unless very old pulsrAF his ould e for instne distnt eqxF he min rguments tht go into fvour of sttistil )utution re the following X

• he evolution of the signi(ne with respet to the livetime does not ompletely folE low its expeted evolution s funtion of √ timeD lthough it inreses with timeF sn prtiulr the signi(ne slightly dereses in the lst PH hours of oservtions @PHIP dtA when utting energies elow QHH qeF

• he signi(ne distriutions over the py re ll well (tted y qussin funtion entred on H nd of width ∼ 1D omptile with pure sttistil )ututions of the kground in the pyF elso the exesses seen in the θ 2 distriutions re not onvining for the existene of signl in the yx regionD exept for energies ove SHH qe where it is seen in Q ins in θ 2 F Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection sn onlusionD new oservtions of grh re required to onlude if the hotspot is (nlly the result of γEry exess or just sttistil )utution of the kground in the reonstruted dtF elso the spetrl nlysis of the yxEypp exess would only eome possile with lrger dtsetD with lerly estlished exess signlF elthough proposl for new oservtions of the dph ws sent to the rFiFFF gollortion in PHIQD no further runs were tken in this region of the sky etween PHIQ nd PHISF he reEnlysis of grh is nywy foreseen in the future with rFiFFFss oservtionsF sn prllel to the work presented in this setionD grh hs een nlysed y qF vmnn et lF IIS using WIFS hours of dt nd di'erent γEry reonstrution lgorithmF xo exess signl ws found @< 1σA t the grh positionF he pper therefore provides limits lultion on the veloity weighted nnihiltion rossEsetion of the hw prtilesF he sme totl run smple ws used ut less strit run qulity seletion uts were ppliedD requesting the presene of t lest Q telesopes in eh run @insted of ll R telesopes in the presented workAF elso the runs were not onstrined to full PV minutes durtion nd no ut ws pplied on the men zenith ngles tht spn here from few degrees to 45 • F his leds to dt smple of 91.5hF he X ef f lgorithm UU ws used for the reonstrution of the γEry eventsD multivrite nlysis method developed to improve the signlEtoEkground disrimintion y exploiting the omplementry disriminting vriles of Q reonstrution methods in use in rFiFFF @inluding rills nd wodel methods disussed in ghpter 2AF he yx region is irle entred t the nominl position of grh nd of extension θ ON = 0.141 • @θ 2 ON = 0.02 •2 AF he yxEypp signi(ne mpD signi(ne distriution nd the ngulr distriution of the events in the py re shown in pigure 4.24F xo signi(nt γEry exess ws found t the position of grh @0.6σAD the θ 2 distriution eing )t nd the signi(ne distriution eing well (tted y qussin funtionF vimits on the veloityEweighted nnihiltion rossEsetion of the hw prtiles @< σv >A were derived for gontinuous hw emission models @see ghpter 1AF pirst n upperElimit on the numer of reonstruted γEry events ws derived t WS7 gv using the peldmn 8 gousins method VQ requiring the numer of yx nd ypp events nd the livetime normliztion ftor αF he result is N 95%CL γ = 123F he lultion proess tht rings to the < σv > limits t WS7 gv will e lter reviewed in 5. Figure RFPS ! enlysis of grh with X ef f @WIFS hours dtsetA X vimits t WS7 gv on the veloityEweighted nnihiltion rossEsetion of the hw prtiles < σv > with respet to the hw prtile mssD for gontinuous γEry emissions nd for two hw hlo pro(les X xp @green dotted lineA nd ssotherml @red lineAF he permiEve limits from the omined study of IS dph with ss V @PHISA is shown in omprison SWF elso WHHH relisti xww dt points re represented in lueD using the pulily ville ode xwwools QFPFR @VIDIQIDQUAF he (gure is pulished in qF vmnn et lF IIS

Conclusions

sn this hpter the yxEypp method ws introdued in the ontext of the reonstrution of γEry exess signl over kground omponentF his method is sed on the de(nition of signl soure region @yxA nd kground regions @yppA tht n e de(ned in the sme py @with wole o'setAD or in di'erent region of the sky @yxGypp pirsA nd tht re used to estimte the kground present in the yx regionF he signi(ne of the yxEypp exess signl is derived using the vi 8 w method IIWF he proedure hs een pplied in Q di'erent nlysis ontextsD ll using the ypp wole on(gurtionD (rst on the unidenti(ed extended soure ri tIURIEQHP in the qE lti gentre region where the yxEypp exess signl ws reonstruted with signi(ne of 7.9σ nd the energy spetrum well represented y powerElw modelF he impt of ri tIURIEQHP in terms of γEry )ux will e further studied in ghpter 6 s the soure oinides with the yx signl serh region for the hw vine nlysisF hen the performnes of the method hve een heked on the extremely vrile nd pointElike extrglti soure u PISSEQHRF his soure is studied y the γEry strophysil ommunity nd serves s lirtion soure for improving the performnes of the rFiFFF γEry reonstrution lgorithmsF he yxEypp exess ws well reonstruted ove IHH qe with the S telesopes of rFiFFFss @tereoA nd lso using the new ig telesope lone @wonoAD with signi(nes of 40.4σ nd 24.3σD respetivelyF elso the energy spetrum ws reonstruted with powerElw modelD the results eing omptile with former rFiFFF pulitionsF he nlysis of u PISSEQHR ws performed severl times in the lst P yers for ensuring the good performnes of the reonstrution of the γEry events t low energies nd t eh mjor step of the development of the rFiFFFss nlysis softwreF yn the other hnd the ypp kground events round the pointElike soure were lso onsidered s possile senrio for the modelling of the kground omponent in the vine serh nlysis t the qg presented in ghpter 6F pinlly the yxEypp method hs een pplied to serh for hw signl from the gittrius hwrf qlxyD dwrf spheroidl glxy oriting the wilky y tht is expeted to ontin lrge hw hlo ontriutionD nd whih is privileged trget for hw nlyses with rFiFFF sine it is lose to us nd no strophysil emission is expeted from this soureF he nlysis with the R telesopes of rFiFFFs showed potentil yxEypp exess t the nominl position of the hwrf qlxyD however not enough signi(nt @∼ 3σA for setting onlusions on the nture of this emissionF he reEnlysis of the soure is expeted in the future with rFiFFFss oservtionsF hile the yxEypp nlysis method desried in ghpter 4 is extensively used in rFiFFF for strophysil soure oservtions with glol estimtion of the exessD the following hpter presents the vikelihood methods proposed y prtile physis nd pplied in the ontext of hw serhes in order to ess more informtion out its ntureF en optimized proedure sed on the wximum vikelihood formlism hs een onsideredF his nlysis methodD lled pull vikelihoodD merges stndrd kground suppression proedure with spetrl shpe ssumptions for the signl nd the kground omponentsF his inreses kground disrimintion potentil nd gives indition out the hw prtile hypothesisF he generl formlism of the wximum vikelihood is introdued in setion 5.1D then developments of the pull vikelihood method in the spei( se of the serh for hw he ove generl vikelihood expression 5.1 is unEinnedD s it tkes individul ounts one y one into the lultionF por lrge mount of ounts ndGor for lrge numer of mesured vriles ssoited with eh ount it is often more onvenient to in the vriles in the orresponding rngesD typilly time or energy ins @in prtile physis experimentsA when mesuring the individul rrivl time nd energy of prtiles in the detetorF sf the totl numer of ounts n is onsidered s rndom vrile then n follows oisson distriution in eh in he proility to oserve n i events in in i is X

P (n i ) = λ n i i n i ! e -λ i @SFPA
where λ i is the verge vlue of the oisson distriutionD prmeter of the model θF he inned wximum vikelihood funtion is then X

L(n| θ) = n bins i λ n i i n i ! e -λ i @SFQA
nd the totl expeted numer of events n is suh tht λ tot = i λ i e prtiulr pproh to the wximum vikelihood method in gherenkov experiments onsists in the reonstrution of the numer of signlGexess events s in the yx nlysis regionD with the numer of yx events N ON nd ypp events N OF F whih re mesured quntitiesF foth N ON nd N OF F re sujet to sttistil )ututions tht oey oisson sttistis X N ON follows oisson distriution of prmeter λ = s + b with s nd the numer of signl nd kground events in the yx regionD while N OF F follows n independnt oisson distriution of prmeter λ = b nd serves s n estimtion of the numer of kground events in the yx regionF he est (t of the numer of signl nd kground events in the yx region is then otined y mximising vikelihood funtion with respet to s nd D lso lled olke formul IRP X

L(N ON , N OF F |s, b) = (s + b) N ON N ON ! e -(s+b) × (αb) N OF F N OF F ! e -αb @SFRA
α is the normliztion ftor etween the yx nd ypp regions @see 4.1AF

his pproh n e used for spetrl (t of mesured energy distriutionF sn prE tie the numer of yx nd ypp events N ON i nd N OF F i in eh in re onsideredD leding to reonstrution of s nd bF rere inned oisson vikelihood funtion n e written X

L(N ON , N OF F |s, b) = n bins i L i (N ON i , N OF F i |s i , b i ) @SFSA
where L i (N ON i , N OF F i |s i , b i ) refers to eqution 5.4 pplied to the single in iF

Binned Poisson Maximum Likelihood with energy side-bands

e inned oisson wximum vikelihood method hs een developed in rFiFFF @tokholm groupA in the ontext of hw vine serhes to lulte the sensitivity to hw vine signls in the qg regionD tking the remining signl ontriution from strophysil glti di'use emission into ountF st ws used to ompre with the results tht will e presented in ghpter 6 with the pull vikelihood methodF st lso served for optimizing the size of the region of interest @ysA in use for this nlysisF his pproh mkes use of yxEypp sutrtion method @see 4.1A nd oisson wximum vikelihood inned in energy X the numer of kground events in the ypp regions is (rst sutrted inEyEin to the yx events F he remining ontriutions from strophysil signls nd residul osmiEry kground re estimted from the yxEypp energy distriE ution onsidering sideEnds in energy on either side of the vine signl serh region then extrpolting the kground estimtion in the serh regionF he result is (nlly ompred to the tul numer of events in the serh region y performing oisson wximum vikelihood (tF sf su0ient lever rm in energy is otined for oth the 4left4 nd 4right4 sideEnds @vineElike signl fetures re shrpD hrteristi of the energy resolution of the detetorA the method provides ompetitive resultsF 122 Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

Un-binned Maximum Likelihood

he unEinned wximum vikelihood pproh provides potentilly more sensitive results is se of limited sttistisF st is lso not sujet to systemtis due to the inningF eduing the in size or inresing the numer of ins n redue the unertintiesD ut in the idel se of n in(nitely smll in size it would led symptotilly to n unEinned wximum vikelihood methodF roweverD inned wximum vikelihood method n e more pproprite when deling with lrge numer of events or lrge numer of mesured vriles per event Y then inned proedure will e preferred for gining lultion timeF sn the se of dt nlysis with rFiFFF typil numer of events @yx C yppA is of the order of 10 3 to 10 5 for round PHh to SHh of oservtion timeD depending on the oservtion mode @rFiFFFsD rFiFFFss wono or tereoAF e vikelihood (t with ID P or Q vriles n esily e performed with n unEinned pproh leding to spei( developments for hrk wtter serhesF 5.1.6 Towards an extended un-binned "Full" Likelihood method for Dark Matter searches es presented in 5.1.1 the vikelihood formlism is generl nd n e pplied to (t ny prmeter of model given the mesured dt villeF he se of n unEinned oisson vikelihood (t is sometimes performed in rFiFFF for the reonstrution of the numer of exess eventsF rowever this onventionl pprohD s sme s the stndrd yxEypp nlysis presented in hpter 4D does not diretly llow proing the nture of the exessD for exmple looking for exoti spetrl fetures tht would give informtion on the strophysil nture of soureF por hrk wtter indiret serhesD looking for exoti spetrl fetures in the energy distriution of the events is essentil to identify nd hrterize potentil hrk wtter ontriutionF st hs een deided to investigte nd develop n extended method for hw signl exE trtionD tht omines the dvntges of n unEinned oisson vikelihood method with dditionl signl hrteriztion power otined with ssumptions on the expeted signl nd kground spetrl shpesF his methodD lled 4pull vikelihood4D is investigted in the next setion 5.2F 5.2. Full Likelihood method 123 5.2 Full Likelihood method he serh for n exoti gmmEry signl from the nnihiltion of hrk wtter @hwA prtiles is prtiulrly omplex for the following resons X 1) redited γEry )uxes from hw nnihiltion @from the lultion of the strophyE sil nd prtile physis ftorsA re low ompred to the )ux from stndrd strophysil soures or osmi ry kgroundF por instne the γEry )ux oming from the qlti hw hlo should e of the order of 10 -12 γ.cm -2 .s -1 t I e nd in region of interest of 0.25 • entred on the hw hloD for n iinsto pro(le nd ssuming tht hw is therml reli with generi nnihiltion rossEsetion < σv >= 3.10 -26 cm 3 .s -1 F rowever in the prtiulr se of hw γEry vines the nnihiltion proess is loopEsuppressed nd the generi nnihiltion rossEsetion is expeted to e lower y t lest ftor of IHF sn omprison the )ux for the osmiErys RH is of the order of 1.8 * 10 -9 γ.cm -2 .s -1 t I e in the 0.25 • regionD while ∼ 3.8 * 10 -11 γ.cm -2 .s -1 for the )ux oming from the gr xeul T nd etween 1 * 10 -12 to 2 * 10 -11 γ.cm -2 .s -1 for vrile soure u PISSEQHR TUF

2) por lind serhD γEry spetrl signtures should e oserved t energies lose to the hw prtile mssF his mss is not onstrined yet @see ghpter 1A nd for most generi models lies etween I qe nd I eF his lrge rnge n only e overed y omining results from the present gmmEry experiments s rFiFFFD weqsgD erits nd permiF

3) ixoti γEry signls like hw gontinuum with utEo' in the spetrum n lso e relted to strophysil glti or extrglti soures like pulsrs nd eqxsF ossile vine signls with signi(ne t the few sigm level ould lso rise from lol sttistil )ututionF sn order to fe those hllengesD we n work on two ftors X E heep oservtions of the hw trget @for 1 nd 3A E roviding n optimized method for signl extrtion with improved sensitivityD dedited to the serh for hw signl @for 1D 2 nd 3A his ghpter fouses on the development of n unEinned pull vikelihood method in the ontext of hw serhesF rere one spei( hw neutrlino nnihiltion hnnel is onsideredD the nnihiltion into two gmmErys χχ → γγ tht produes spetrl vines with energy E line equl to the hw prtile mss m χ F he proedure hs een oded in gGgCCGroot s n independent progrmF he method priniple nd extended developments re introdued in setions 5. where n extr hp term is dded in the vikelihood funtionF st hs een deided to develop the proedure s unEinnedF he numer of signl nd kground events in the nlysis region re free prmeters of the modelD while dditionl informtion on the signl nd kground spetrl shpes is dded in the (tF wodel prmeters suh s the powerElw index of n strophysil signl or kground omponentD utEo' vlue or vine position in energy relted to the hw prtile mss n e dded s dditionl prmeters of the (tF his results in higher sensitivity of the method for signl reonstrution with spetrl hrteriztion of the exess in the proessF wesured vriles re the oserved numer of yx nd ypp eventsD plus vriles ssoited with individul events suh s the energyD time of rrivl or reonstruted diretionF elso kground spetrl properties n e derived from the mesured ypp event distriutionF 5.2.1.2 General formula he proility of oserving N ON events in the yx nlysis region with individul oserE vles x nd N OF F events in the ypp region given tht these numers follow oisson distriE utions of respetive prmeters @verge vlueA s + b nd b nd given tht they depend on spei( wodel M ( θ) for the signl @strophysil or hwA nd the kground omponentsD is desried y the unEinned vikelihood funtion X L(N ON , N OF F , x|s, b, M ( θ))

= (s + b) N ON N ON ! e -(s+b) × (αb) N OF F N OF F ! e -αb × N ON i P DF (x i |M ( θ)) @SFTA P DF (x i |M ( θ))
is the roility hensity puntion of the event i with mesured quntities x i F α is the normliztion ftor etween yx nd ypp regionsF wximizing this pull vikelihood funtion with respet to sD nd the model prmeters θ gives the omined est (t of these prmetersF sn the most generl se the roility hensity puntion of the event i depends on the onsidered signl nd kground models M ( θ) nd on the following mesured quntiE ties X

• he energy E i of the event iF he hp is relted to the ssumed energy distriutions of the γEry soure nd the kground modelsF • he rrivl time t i of the event iF he hp is relted to the ssumed temporl vriility of the γEry soure nd the kground modelsF • he sptil diretion (φ x , φ y ) i of the event i in the frme of the pointing position of the telesopesF he hp is relted to the ssumed sptil morphology of the γEry soure nd the kground modelsF st lso depends on the eptne of the experiment Acc(E i , t i , φ x i , φ y i , φ z i ) tht is funtion of ll the ove prmetersD plus the oservtion enith engle φ z i of the event iF roweverD in the oservtion of pointElike γEry soures of extension smller or ompE rle to the ngulr resolution of the sFeFgFFs @∼ 0.1 • for rFiFFFsA nd tht re supposed to e temporlly stedyD the hp only depends on the mesured energy E i of the individul events iF his is for exmple the se of eqxs @like u PISSEQHRA in nonE)ring sttesD tht re onsidered s stedy pointElike souresF por hw hlo where most of the mss lies t the entre inside the nlysis region the nonEdependeny on the diretion of the events @then the lowEextension of the soureA is usully mde s n pproximtionF yn the other hnd hw hlos re temporlly stedy t humn oservtion time slesD s well s their γEry emission from hw prtile nnihiltionF e lso suppose tht ll the oservtion runs re tken with similr enith englesF sn the following setions temporlly stedy nd sptilly lowEextended γEry signls re onsideredF he roility hensity puntion of the individul events i only depends on the individul mesured energies E i nd on the onsidered signl nd kground models M ( θ)F his pproximtion will e mintined for the hw nlysis performed in the qlti gentre region @hpter 6AF

Development of the formula

ih individul event i in the nlysis region hs ertin proility to e signl event nd ertin proility to e kground eventF he hp of the event i P DF (E i |M ( θ)) n e written s the sum of signl hp nd kground hp X

P DF (E i |M ( θ)) = η × P DF S (E i |S( θ S )) + (1 -η) × P DF B (E i |B( θ B )) @SFUA
where P DF S is the signl hp with ssoited signl model S( θ S )D P DF B is the kground hp with ssoited kground model

B( θ B )F η is the signl frtion X η = s s + b @SFVA nd is lso model prmeter X M ( θ) = η, S( θ S ), B( θ B ) F
por more simpliity in eqution writingD the signl nd kground models S( θ S ) nd B( θ B ) will not e expliitly written in equtions nymore ut remin impliitF prom equtions 5.6 nd 5.7 the pull vikelihood formul eomes X

L(N ON , N OF F , E|s, b, M ( θ)) = (s + b) N ON N ON ! e -(s+b)
Poisson term for ON

× (αb) N OF F N OF F ! e -αb
Poisson term for OFF

× N ON i η × P DF S (E i ) + (1 -η) × P DF B (E i )
Shape term @SFWA Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

wximizing the likelihood funtion L is equivlent to minimizing the logElikelihood funtion -2lnLD tht is relted to the χ 2 de(nition nd is more onvenient for the de(nition of on(dene intervls @see 5.2.3AF sn prtiulr the ftor -2 is introdued suh tht the minimum of -2lnL follows χ 2 distriutionF he expression for the logEvikelihood formul eomes X

-2ln(L) = 2b 1 -η -2N ON .ln( b 1 -η ) + 2αb -2N OF F .ln(αb) - 2
N ON i ln η × P DF S (E i ) + (1 -η) × P DF B (E i ) @SFIHA
where s hs een expressed in funtion of η in the oisson term for yxD nd onstnt terms removed s they do not 'et the (tting proedure nd on(dene intervls lultionF e smller vlue of -2lnL orresponds to etter greement etween the dt nd the modelF he minimiztion of this funtion llows to reonstrut X • ηD the signl frtion in the yx nlysis region • bD the numer of kground events in the yx nlysis region • edditionl prmeters θ from the onsidered soure @signlA nd kground models S( θ S ) nd B( θ B ) relted to P DF S nd P DF B suh s the hw prtile mss nd the kground spetrl powerElw index or utEo' energyF 5.2.1.4 Physics justication he hoie of suh n unEinned pull vikelihood pproh for hw signl serhes is motivted y the following rguments X

• e vikelihood method is nonEsutrtiveD while undesirle prtil sutrtion of the exoti signl is possile with stndrd yxEypp nlysisF

• ith pull vikelihood method it is possile to reonstrut the γEry signl frtion nd spetrl fetures tht re hrteristi of the hw model like the hw prtile mssF e n then (gure out if the exess signl is onsistent with hw signlD or in se of no signl set lower ndGor upper limits on the hw model prmetersF

• he presene of the prmeter η in oth oisson nd hpe terms of the pull vikeE lihood funtion in eqution 5.9 leds in gin in sensitivity for the reonstrution of tht prmeterD s seen in eleksi et lF PQF

• en unEinned method is more urte thn inned method s it hs een exE plined in setion 5.1.5F e inned pproh would e used in se of lrge sttistisD for spei( studiesF rere with sttistis of out 10 3 to 10 5 for PHh to SHh of dtD vikelihood (t with ID P or Q prmeters n esily e performed unEinnedF

Development of the method

his setion fouses on the tehnil developments of the method from the de(nition of the inputs @eFgF instrument responseD proility density funtionsD region of interest nd energy rnge for the (tA to the reonstrution of the model prmeters nd the lultion of on(dene intervlsF 5.2.2.1 Instrument Response Functions he snstrument esponse puntions @spsA hrterise the response of the detetor to inE ident γErys nd osmiEry kground eventsF st onsists in the eeptne @or e'etive reA for gmmsD hdrons nd eletronsD the inergy isD the inergy resolution nd the enE gulr resolution of the detetorD whih depend on the telesope on(gurtion nd γ seletion utsF sFFpFs n e represented s funtion of the energy nd of the rdil oordintes with respet to the pointing position of the telesopes @tht lst e'et is not onsidered hereAF he sps re essentil in the de(nition of the signl hp s it will e shown in 5.2.2.2F pigure 5.1 displys the sps of rFiFFF for gmmErys for the stndrd rFiFFFs tereo @R telesopesA nd the rFiFFFss wono @gS onlyA nd tereo @ll S telesopesA telesope on(gurtionsF hey re derived from full wg simultions of the detetor nd of γEry shoE wers under the pointElike soure hypothesisD with oservtion onditions onsistent with the performed vine nlysis in ghpter 6 X • enith nglea18 eeptne @m 2 A 1.5 × 10 5 7.0 × 10 4 1.5 × 10 5 inergy is @%A -0.6 -0.5 -3 inergy resolution @%A 9.5 25.0 10.5 engulr resolution @ • A 0.065 0.155 0.064 • eonstruted hp X it onsists in deonvoluting the dt events y the sps to derive the initil spetrum of the orresponding gmmEry omponentF e spetrl model @eFgF powerElwA n e (tted on top of tht reonstruted spetrumF • wesured hp X the hp shpe represents diretly the mesured energy distriuE tionsF he hp funtion n e derived from wonteEgrlo @wgA simultions with the onvolution of given spetrl model y the spsD or diretly (tted on mesured dt orE responding to spei( signl or kground omponent @ontrol smpleAF his is explined on pigure 5.2F st hs een hosen to work with mesured hp for the dt nlysis presentedF Measured PDF from MC data :

he wg events re generted ording to given spetrl model nd re then onvoluted with sps to mth the shpe of mesured dt distriutionsF he generl nlytil expresE sion for the mesured hp is funtion of di'erentil )ux of the signl or kground omponentD the sps @eptneD energy is nd energy resolutionA nd the energy X

P DF measured (E) = 1 N ∞ 0 dΦ(E ) dE IRF (E; E )dE @SFIIA
where Φ is the di'erentil )ux relted to the spetrl modelF IRF refers to the instrument response to γErysF E is the true energy nd E the mesured energy tht hs een 'eted y the spsF x is the hp normliztion ftor suh tht Emax E min P DF (E)dE = 1 on the onsidered energy rngeF prom prtil point of view the wg hp for given signl or kground omponent is generted from n histogrm in energy with 10 6 events rndomly produed from the expeted di'erentil )ux dΦ(E ) E F ih individul wg event of true energy E is onverted into mesured event of energy E with smering y the sps with rndom drwing on qussin entred on (E + E bias ) nd of width E res where E bias nd E res re the energy tionF sn this exmple the dt events re supposed to e osmiEry kground events onlyD without ny strophysil or hw ontriutionsF he hp funtion n e otined from wg dt ssuming spetrl model for the kground tht is onvoluted with sps to mth the shpe of mesured dt events distriutionsF he seond option is to (t the hp funtion diretly on the kground dt present in ontrol regionsD for exmple ypp regions in the sme (eld of viewF is nd resolution respetivelyD nd weighted y the eptne vlue t the true energy i9F he resulting hp distriution is (tted with funtion tht is then normlized to I on the onsidered (tting energy rngeF por the hw signl hp the di'erentil )ux depends on the hw prtile mss m χ tht is (tE ted prmeter of the modelF gonsequently wg signl hp is generted for eh step in m χ F Measured PDF from control data he hp of spei( gmmEry ontriution n lso e derived diretly from ontrol dtset tht presents the sme hrteristis s the dt events in the ysD for exmple ypp regions in the sme (eld of viewF his mostly pplies to the osmiEry kground omponent tht is present in every dt nlysis nd its remining ontriution @fter disriminting vrile utsD see ghpter 2A n e isolted from strophysil or exoti γEry ontriutions y oserving ypp regions where no other signl is expetedF his pproh is prtiulrly interesting sine ypp dt is genuine representtion of the kground present in the nlysis regionF por keeping oservtion onditions s stedy s possile the more nturl wy is to tke the kground energy distriution from ypp regions in wole modeD or n ypp run from yxGypp pirs @see 4.1AF st is lso possile to use di'erent ontrol smple with similr oservtion onditionsD like kground from wellEknown lirtion souresF Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

sn the ontext of the hw nlysis presented we rely on hps from oth wg nd ontrol dtsets X the generl performnes of the pull vikelihood method for vine signl reonstrution re investigted in setion 5.2.4 with pure wg dt for oth the signl nd the kground hpF yn the other hnd for the vine nlysis performed in ghpter 6 the kground P DF B @osmiErys nd strophysil di'use emissionA is derived from ypp kground ontrol dt while the expeted hw signl P DF S relies on wg dt generted ording to the model prmeter m χ F

Example of signal and background PDFs ypil exmples of signl nd kground hps in the ontext of hw serhes re represented on pigure 5.3F hese re mesured wonteEgrlo hps generted ording to the wg proedure desried oveD here for the rFiFFFss tereo telesope on(gurtion nd using the sFFpFs for gmms shown on pigure 5.1F he orresponding )ux models @with true energy E A re X

• owerElw estrophysil signl X dΦ(E ) dE = A.E -Γastro with index Γ astro = 2.3 @SFIPA
his hp is used s spetrl representtion of the di'use γEry emission omponent in the qlti gentre regionF

• owerElw osmiEry kground X dΦ(E ) dE = A.E -Γ CR with index Γ CR = 2.7 @SFIQA
his hp is used to model the osmiEry kground omponent in rFiFFF dt

• hw nnihiltion gontinuous signl X dΦ(E ) dE =          p 1 m χ . e -p 2 E mχ E mχ p 3 + p 4 for E ≤ m χ 0 for E > m χ @SFIRA
with utEo' energy orresponding to hw prtile mss m χ = 700GeV F he prmetriE ztion is tken from vF ollnd thesis IRQ X

• hw nnihiltion vine signl X

dΦ(E ) dE = δ(E -m χ ) @SFISA
whih is simple helt funtion t m χ D here UHH qeF efter eing smered y the sps the hp is well desried y n symmetri qussin funtion with width relted to the 5.2. Full Likelihood method 133 energy resolution of the experimentF he symmetry omes from the eptne smering nd liner dependeny in the resolution in energyF he performnes of the pull vikelihood method strongly depend on the di'erenes etween the signl nd kground hp shpesF por instne n exoti vine signl will e muh esier to identify thn onventionl strophysil signl when disriminting with powerElw kground omponentD due to the shrp nture of the vine signl tht lerly ontrsts with the ontinuous nture of powerElwF he systemtis on the signl nd kground hp hve to e onsidered whih impt the qulity of the reonstrution of the model prmeters Y deep investigtion of these systemtis will e done in ghpter 6 efore pplying the method on the dt smplesD y introduing nuisne ftors in the signl nd kground hp prmetriztionsF

Region Of Interest (ROI)

he hoie of the egion yf snterest @ysAD iFeF the yx nlysis regionD is determinnt for rehing optiml sensitivity to hw signlsF he de(nition of the ys is relted to the omplexity of the nlysis Y expeted position nd size of the hw hloD presene of strophysil soures or γEry di'use emissions in the (eld of viewD nd sptil limits due to the limited (eld of view of the instrumentF hw hlos re sptilly extended with extension depending on the onsidered hlo pro(le @see ghpter 1AF por extrglti soures @eFgF eqxsA the γEry emission from the soure is pointElike nd is expeted to oinide with the entre of the hw hloF sn this sitution the yx region for hw nlysis my onsist in n extended irulr region θ >> P SF nd msking out the entrl soure RF por hwrf pheroidl qlxies no strophysil signl is expeted nd the hw hlo is supposed to e entred on the grvittionl ryentre of the hwrf qlxyF he size of the ys n e optimized in order to inrese the signlEtoEkground rtioD in prtiulr smllEextension ys my e onsidered sine the entrl region of the hwrf qlxy is not exluded @ontrry to rFiFFF with extrglti souresA nd the ys would then ontin the possile usp of the hw hloF elso exessively inresing the ys size would result in drop in sensitivity s the numer of kground events would strt to dominte over the hw signl omponentF pinlly for the qlti gentre regionD ompromise hs to e found etween the hw hlo extension nd the vrious exlusion regions tht re usully de(ned on the entrl soure nd long the qlti lneF e frtionl ys omposed of severl setions of the py from either side of the exluded qlti plne @hlfEirles of 1 • rdiusA ws onsidered in previous rFiFFF hw pulitions TPF por the hw vine serh tht is presented in ghpter 6 the ys size will e optimized using wg simultionsF por the generl wg performne studies in setion 5.2.4 the ys is not optimized in ny prtiulr nlysis ontextD ut onsists in irulr region of extension θ = 0.25 • tht ompromises etween the situtions presented oveD nd is su0iently lrge to ontin most of the hw signl in uspy hlo pro(leF 5.2.2.4 Energy range for the Full Likelihood t he energy rnge for the (t of the model prmeters hs lso mjor in)uene on the performnes of the methodF yn one sideD it my e wise to hoose n energy rnge tht is su0iently lrge to inlude most of the hrteristi di'erenes etween the signl nd the kground hpF por exmple hw γEry gontinuous nnihiltion signl with utEo' energy E cut-of f = m χ is similr to owerEvw osmiEry kground for energies `Ecut-off ut strongly di'erent for energies b E cut-of f Y in tht se n energy rnge going eyond E cut-of f my ring more disrimintion power to the methodF yn the other sideD nrrow energy rnge tht omprises most of the expeted hw signl provides lrger signlEtoEkground rtioF his sitution is prtiulrly relevnt for hw vine signls where the spetrl extension σ line is relted to the energy resolution of the instrumentF ine the ext position of the hw vine is prmeter of the (tD onventionl pproh with sliding window in energy my e used suh tht the rnge omprises most of the hw vine signl t eh step in m χ F sul sliding windows rnge from m χ ± 1σ line to m χ ± 3σ line F rowever this pproh my lso loose in sensitivity from the lk of su0ient lever rm in energy for the kground hpF por the following wg performne studies in 5.2.4 lrge (xed energy rnge of PHH qe Y Q e is onsidered tht gives su0ient lever rm with P DF S nd P DF B nd llows reonstruting m χ on omfortle mss rngeF sn this hpter the energy region PHH qe is ignored s the distriution of the events is degrded y the eptne t the energy thresholdD s seen in the hp exmples of (gure 5.3F o perform n nlysis ner the threshold of the instrument requires speil ttention sine systemtis my strongly 'et the reonstrution of the γEry eventsF his sitution is treted in ghpter 6 s the nlysis fouses on the serh for hw vine t IQH qeF

Statistical estimators

Condence Intervals

he on(dene intervl @gsA for the reonstrution of model prmeter θ re)ets the sttistil preision of the mesurement of θF st is de(ned s n oserved intervl round the (tted vlue θ best tht frequently inludes the true vlue of the prmeter θ true if the experiment is repetedF gon(dene sntervls re ssoited with orresponding gon(dene vevels @gvA in perentF por exmple de(ning gon(dene sntervl t 95% gon(dene vevel round θ best mens tht if the experiment is repeted N times under the sme onditions nd with N di'erent dtsets 95% of the N ssoited gon(dene sntervls inlude θ true F sn our se gs re derived from the vritions of the logEvikelihood funtion @eqF5.10A on either side of the est (t vlueD fter sutrting the minimum of the vikelihood X -2∆ln(L) = -2ln(L) -ln(L(est)) @SFITA sullyD prmeter α is hosen suh tht the proilities exluded eyond lower nd upper ounds (θ 1 , θ 2 ) re eh α/2 where (1 -α) refers to the gvF he gs is onsequently de(ned requiring the proility P (θ

1 < θ best < θ 2 ) ≥ (1 -α)F
pigure 5.7 shows the priniple of on(dene intervls lultion from the -2∆ln(L) funtionD for the single (t prmeter θF

Figure SFU ! houleEsided versus ingleEsided gon(dene sntervls t gon(dene vevel

(1 -α)@7A for the (t of single model prmeter θF houleEsided gs re used when it is relevnt to onstrin oth the lower nd upper ounds of the prmeter θF hen only the upper limit is of interest it is more onvenient to lulte singleEsided gs Y this hppens for instne when reonstruting very low positivelyEde(ned signl frtion η 0 for whih the lower ound of the gs would e negtiveF hen removing the onstrint on the lower ound of the prmeter θD the douleEsided gs t (1 -α)% gv eomes singleEsided gs t (1 -α/2)% gv for the sme logEvikelihood vlueF por exmple singleEsided gs t 95% gv orresponds to the sme logEvikelihood vlue s douleEsided gs t 90% gvF he reltionship etween gon(dene vevels nd logEvikelihood vlues is presented in le 5.2 @tken from the hq fooklet of rtile hysisA orresponding to douleEsided gs nd for the reonstrution of m model prmetersF he sttistil preision of the mesurement degrdes with the numer of (tted prmeters resulting in lrger logElikelihood vlues t given gvF por PEdimensionl (t @eFgF the hw signl frtion η nd mss m χ A gs re intervls in P dimensionsD rther lled 4regions4 or 4ontours4 in the PEdimensionl phseEplne of (η, m χ )D s shown on pigure 5.8F por the present hw studiesD in se of reonstruted signl douleEsided gs re omputed t WS7 gv orresponding to logEvikelihood vlue of SFWWF

(1 -α) (%) m = 1 m = 2 m =
X N σ = √ T S @SFIVA
sn the onventionl se of oisson wximum vikelihood method @see 5.1.3A were only the numer of signl nd kground events in the nlysis region re prmeters of the (t the estimtor refers to the stndrd vi8w exess signi(ne from eqution 4.7F

rere for the Ph (t of (η, m χ ) we de(ne glol estimtor tht hrterizes oth the signl exess nd the signl position in energy X

T S = -2ln L(η = 0, m χ (0)) L(η, m χ ) best @SFIWA
where m χ (0) is the est (t vlue of m χ under the null hypothesis η = 0F etully the wximum vikelihood vlue for the null hypothesis L(η = 0, m χ (0)) is independent of m χ s the ssumption η = 0 in eqution 5.10 removes the dependeny in the signl hpF elsoD s the null hypothesis is here de(ned y ondition on single prmeter η the signi(ne of the reonstruted vine signl follows eqution 5.18F

Sensitivity limits in case of no reconstructed signal

sf there is no hint for signl detetionD or if the reonstruted signl lies under P sigm we ompute the sensitivity limits of the method for the detetion of hw signlF ensitivity limits re onventionlly de(ned s the lowest γEry )ux tht n e reonstruted y the experiment t given on(dene levelD nd for given spetrl model @here hw signlAF sn the present sitution it is not useful to ompute the PEprmeter pull vikelihood (t of (η, m χ ) sine the (t of m χ is not relevnt if there is no reonstruted exessF rowever for given mss it is possile to lulte n upper limit on the numer of reonstruted signl events N γ F rere the orresponding on(dene level is hosen to e 95% so the upper limit is N 95%CL γ F pigure 5.9 shows how to ompute N 95%CL γ from the normlized pull vikelihood -2∆lnL pro(le in η t given m χ F he upper limit on the signl frtion η 95%CL is derived from the singleEsided gs t 95% gvD orresponding to logEvikelihood vlue of PFUIF

N 95%CL γ = b. η 95%CL 1 -η 95%CL @SFPHA
where b is the numer of kground events in the ys estimted from the ypp regionsF he γEry )ux limit t 95% gv n e written s follows X

Φ 95%CL γ = N 95%CL γ × Emax E min dΦ dE (E, m χ )dE T OBS Emax E min Acc(E) dΦ dE (E, m χ )dE @SFPIA
where dΦ dE (E) is the onsidered di'erentil )uxGspetrl modelD Acc(E) the eeptne for gmmsD T OBS the oservtion time nd [E min , E max ] the onsidered energy rngeF por hw nnihiltion into two gmms χχ -→ γγ the di'erentil )ux is dΦ

(E) dE = 2 * δ(E -E line )F
sn the ontext of hw serhesD it is lso relevnt to plot the limits on the hw γEry veloityEweighted nnihiltion rossEsetion < σv > @cm -3 .s -1 A tht is relted to the ove γEry )ux limit nd the strophysil ftor Φ astro @iFeF the morphology of the onsidered Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

hw hloD see hpter 1A X

< σv > 95%CL = 8πN 95%CL γ T OBS × Φ astro . m 2 χ Emax E min Acc(E). dΦ dE (E, m χ )dE @SFPPA
he plot of < σv > 95%CL with respet to m χ nd with ssoited sttistil nd systemti error is the referene sensitivity plot of n experiment for indiret hw serhes onsidering the nnihiltion of neutrlinos into γErysF he reson is tht the physil quntity < σ.v > origintes from the prtile physis ftor nd not from the hw hlo morphology nd then provides referene vlue when ompred with other indiret hw γEry experiments like rFiFFFD permiD weqsgD erits @nd ge in futureA in the oservtion of ny potentil hw regionF qenerlly the nonil vlue < σv > can = 3.10 -26 cm -3 .s -1 tht orresponds to the hw osmologil reli density serves s omprisonD sine n experiment sensitive to tht < σv > can would e le to rule out the hw hypothesisF rowever for hw vine serhes the nnihiltion proess is loopEsuppressed lowering the nonil vlue y I to P orders of mgnitudeF sn the hw vine nlysis of the qg region presented in ghpter 6D the pull vikeliE hood (t is performed IEdimensionl s funtion of η for the lultion of upper limits on Φ nd < σv >D sine no exess signl is oserved in the onsidered dt smpleF rowever for the following wg studies @5.2.4A performnes of the method re lso tested for (xed hw signl frtions thus llowing the PhEreonstrution of the model prmeters @η, m χ AF 5.2.4 Performances of the method with Monte-Carlo simulations sn this setion the performnes of the pull vikelihood method re evluted in the ontext of hw vine serhes for wide rnge of input signl frtions nd vine energiesD using wg dt smplesF por eh ouple of input vlues (η, m χ ) true vine signl events re simulted on top of wg kground distriution tht inludes osmiEry hdrons nd ontriution from strophyE sil di'use emissionF he numer of kground events is hosen to mth the kground level seen in the qlti gentre regionD ssuming low zenith ngles nd wole o'sets of out 0.5 • -1 • F he ys is de(ned s irulr region of rdius θ = 0.25 • dpted for the nlysis of extended soures in the py nd tht is su0iently lrge to ontin most of the hw density in uspy hlo pro(leF he wg experiment is repeted SHH times for sttistil lirtion of the errors on the reE onstrution of the model prmeters (η, m χ )F erformnes with oth rFiFFFss wono nd tereo telesope on(gurtions re ompred ove PHH qe where the present nlysis softE wre is est opertingF hese wg studies pve the wy to the vine dt nlysis performed in ghpter 6F

Working with MC simulations -Statistics Calibrated errors

sn the nlysis of rel dtset the pull vikelihood (t of the model prmeters η nd m χ is performed y minimizing the Ph logEvikelihood funtion in (η, m χ ) @or minimizing the Ih logEvikelihood funtion in η t given m χ for limits lultionAD nd omputing gon(dene sntervls round the est (t vluesF his hs een desried in setion 5.2F rowever the true vlues of the model prmeters re unknown nd the omputed gs is de(ned s region tht overs the true prmeters with ertin proility if the experiment is repeted ertin mount of timesF wg simultions o'er the possiility to lirte the gs y the repetition of N experimentsF he result is gon(dene sntervl lirted in sttistil wyF elso some systemtis inherent to the method n e evluted in the proessF he numer of wg simultions is hosen to e N = 500D required for hving good evlution of the gsF por eh of the SHH wg experiments the est (t vlues (η, m χ ) best re (lled into Ph histogrmF irrors with respet to the true vlues re derived diretly from this est (t distriutionD s shown on pigure 5.10 for the exmple of single (t prmeter m χ F he systemti error is de(ned s the devition of < m χ best > with respet to m χ true while the sttistil error is relted to the sigm of the qussin distriution round < m χ best >F sn the present sitution the distriution is Ph qussin entred on the est (t vlues < (η, m χ ) best > verged over the SHH simultions F glirted errors re de(ned suh tht 95% of the SHH simultion results lie inside the mrgin of errorF

Inputs of the MC procedure

por the wg performne studies the following inputs re onsidered X

• Region Of Interest : irulr region ROI = 0.25 • orresponding to solid ngle ∆Ω = 5.98 * 10 -5 srF he pointed region of the sky is not importnt s the numer of vine signl events is de(ned s frtion of the kground eventsF

• Observation time : T OBS = 50hF st orresponds to referene oservtion time for stndrd soure nlysis in rFiFFF

• Background events : he numer of osmiEry kground events is hosen to mth the kground level seen in the qlti gentre regionF prom the nlysis of PHIR ontrol dt with low zenith ngles @< 20 • A nd wole o'sets of ∼ 0.5 • -1 • it orresponds to n verge of ∼ 17050 events in wono telesope on(gurtion nd ∼ 8905 events in tereo in the hosen ysD for SHh of oservtion time nd efore energy utsF e frtion of γ-ry qlti di'use emission is lso inluded in the kgroundF uF wor @tokholm niversityA extrpolted the numer of di'use events from the rFiFFFs spetrum pulished in PHHT TVF st orresponds to TFI7 ontriution resulting in 1120 events in wono nd 585 in tereoF he totl numer of wg kground events is then 18170 in wono nd 9490 in tereoF hese numers re summrized in le 5.3F

wg Table SFQ ! snput numer of simulted events in the ys for the osmiEry kground nd the glti di'use emission omponentsD efore energy uts nd for SHh of oservtion time fkground sttistil )ututions re tken into ount in the oisson vikelihood term @see 5.9AD with N OF F eing rndomly simulted round the men vlue α * N background for eh of the SHH simultionsF sn the present ys nd wole o'set on(gurtion @0.5 • -1 • A the numer of ypp regions is α = 8F

• MC Dark Matter signal events : these wg studies do not fous on spei( hw hlo with n expeted γEry )uxF snstedD the pull vikelihood proedure is tested for di'erent input vlues of the signl frtion η with respet to N background in the hosen energy windowF e hose to work with the following input vlues X η input a 5%D 10%D 20%D 30% nd 50%F he orresponding numer of signl events is then given y the eqution X • DM Line signal PDF : he signl hp is delt funtion δ(E -m χ ) smered y the spsF he performnes of the pull vikelihood method re evluted for T vlues of the hw prtile mss X m χ a 250GeV D 300GeV D 500GeV D 700GeV D 1T eV nd 2T eV F pigure 5.13 shows the wg event distriution for one experiment in tereo modeD with S7 vine signl t QHH qe simulted on top of the kground omponentF he fkE ground hp is lso represented y the lk solid line in the energy window [200GeV ; 3T eV ] @here resled to dtAF

N signal = η 1 -η * N background @SFPQA • Instrument

MC results

he performnes of the pull vikelihood method with wg dt re presented on pigure 5.14F ell the relted numers re given in le 5.4F

por eh ouple of input prmeters (η, m χ ) true the method is pplied over SHH wg dt smples nd the glol est (t vlues (η, m χ ) best re reonstruted with ontours orresponding to WS7 ontinment frtion of the resultsD for oth rFiFFFss wono @in blackA nd tereo @in blueA telesope on(gurtionsF glirtion plots re representing the evolution of the reonstruted prmeters with respet to the true prmetersD shown s IhEprojetions of the Ph results for presenttion purposesF sn prtiulr the (gures η reco = f (η true ) @A re presented for the two extreme ses m χ = 250GeV nd m χ = 2T eV D nd sme for m χ reco = f (m χ true ) @A with η = 5% nd η = 50%F his llows proing overll performnes of the method for vine signl reonstrutionF ixmples of Ph (ts re lso given in @A nd ompred on sme sle in η nd m χ oordintesF he results re very promisingF por the onsidered inputs in 5.2.4.2 the method is le to reonstrut vine signls frtions ≥ 5% nd msses ≥ 250GeV with less thn QH7 unertinty t WS7 ontinment on η @wono nd tereoAD nd less thn PH7 @wonoA nd IH7 @tereoA error on m χ F sn prtiulr these unertinties re ll t few perent level when deling with signl frtions ove IH7 nd msses ove PSH qeD nd improve when reonstruting lrger msses s the lol numer of kground events dereses following powerElw funtionF fis on the reonstruted vlue of η is lso oserved t the lowEend of the energy window when reonstruting PSH qe vine in tereo @IH7 e'etA nd PSHqeEQHHqe vines in wono @PH7 e'etA Y this is simply explined y the energy resolution of the instrument tht spreds the vine events distriution elow PHH qeD resulting in lower vlues of the η prmeter tht tully mth the frtion inluded inside the energy windowF gonerning the ompred performnes of the wono nd tereo reonstrutionsD desE pite the lowEend e'et desried oveD the tereo reonstrution is est performing t low signl frtions @smller errorsA due to the improved energy resolution of the instrument tht mkes vine signls more distinguishle from the powerElw kground distriutionF rowever when reonstruting oth lrge frtions nd msses the two reonstrutions re lmost equl with unertinties `I7 on the reonstruted prmeters t WS7 ontinmentF pinlly the onditions for rehing detetion t 5σ signi(ne level hve een determined from distriutionsF sn wono n input frtion of t lest S7 is required in omintion with msses over QHH qeF sn tereo the signi(ne is lredy rehing 5σ with frtion of S7 nd for ny onsidered mssesF hese results don9t tke systemtis of the method into ount nd we should not forget tht they orrespond to SHh of oservtion timeF ine the method is well performing down to S7 vine frtions it is interesting to inE Table SFS ! ummry tle X wg sensitivity limits with respet to m χ when no hw signl is generted @η input = 0AD in wono nd tereo telesope on(gurtionsF esults t WS7 gv re shown on the reonstruted line signl rte η 95%CL nd on the γEry )ux per sterdin unit Φ 95%CL /∆ΩF

η true m χ true η reco m χ reco η reco m χ reco is σ 95%CL is σ 95%CL is σ 95%CL is σ 95%CL @eA @7A @7A @7A @7A @7A @7A @7A @7A
m χ η 95%CL Φ 95%CL /∆Ω η 95%CL Φ 95%CL /∆Ω @eA @7A 10 -4 γ.m -2 .s -1 .sr -1 @7A 10 -4 γ.m -2 .s -1 .

Conclusions

en unEinned pull vikelihood proedure hs een developed in the ontext of hw serhes with rFiFFF sn this hpterD ll importnt steps of the method nd the developments relted to the spei( se of the reonstrution of hw neutrlino nnihiltion γEry vine signl were disussedF he extension of the stndrd pprohes with shpe term sed on signl nd kground roility hensity puntions for individul events enles to reonstrut the hw prtile mss in ddition to the signl frtion in the egion yf snterest nd on the onsidered energy rngeD nd ssoited on(dene intervls nd signi(nesF erformnes of the method hve een investigted with wg dt smples for relisE ti oservtion nd nlysis onditions with kground level hrteristi of the level seen in the qlti gentre regionF he method is le to reonstrut vine signls down to IFS7 frtion t WS7 on(dene levelD with possile 5σ detetion for frtions exeeding S7F glirted errors t WS7 gv hve een lulted with SHH wg experiments for ouples of input prmeters (η, m χ ) true nd re t mximum level of 20 -30% in wono nd tereo telesope on(gurtions with signl frtions rnging from S7 to SH7 nd msses rnging from PSH qe to P eF his pull vikelihood proedure will e used with similr sheme on rel dt smples in ghpter 6 in the qlti gentre regionD with totl smple of out PHh of oservtion time nd with dditionl omplexity in onsidering the energy region elow PHH qe were systemtis t the threshold will e studiedF gomplete optimiztion of the method nd systemtis lultion will e done with mesured kground distriutions in the pyD with the im to on(rm or exlude the hotspot feture t IQH qe reported in permiEve dt in PHIP ITPD nd to produe limits on the hw nnihiltion rossEsetion on omplete mss rnge etween IHH qe nd P e tht omplements the former pulished rFiFFFs results RF

Introduction

he generl ontext of the serh for hrk wtter nnihiltion signls hs een set up in ghpter 1F ghpter 5 introdued the pull vikelihood nlysis proedure tht is onsidered for produing the min results on the serh for exoti gmmEry signls with rFiFFFssF sn this hpter we fous on hw vine serhes in the qlti gentre @qgA regionF vine spetrl fetures hs the dvntge of eing very simple to modelD qussinElike @in logIH of the energyA when smered y the energy resolution of the instrument Y those exoti spetrl ontriutions re esier to disriminte from power lw kground @ompred to hw gontinuum signlA nd the hw prtile mss is diretly relted to the energy of the deteted vine signlF yn the other hnd hw vine signls re loopEsuppressed in neutrlino models nd the numer of γEry vine events re expeted to e I to P orders of mgnitude less thn with hw gontinuumF he potentil for the detetion of given low vine signl frtion ws shown to e promising in ghpter 5F

HESS-I and Fermi Line search results

erhes for hw vine signls hve lredy een performed in the lst dedeD nd very reE ently with rFiFFFs @PHIQD RA nd permiEve @PHIQD IHAF he permiEve pper onsists in the nlysis of QFU yers of dt with set of (ve FyFsF deE (ned round the qgD eh optimized for (ve di'erent hw hlo pro(lesF he regions |b| < 5 • nd |l| > 6 • were msked Y this exludes the qlti lne tht is dominted y the presene of strong strophysil soures nd of the glti di'use emission ut does not exlude the entrl soure sine etter sensitivities n e hieved y inluding the dense prt of the hw hloF he rFiFFFs pper omprises IIPh of oservtions t the qgD exluding the qlti lne |b| > 0.3 • nd the entrl soure y tking two hlf irles of 1 • rdius on either side of the qlti lne s the FyFsF foth permiEve nd rFiFFFs nlyses hve een performed using stndrd innedE vikelihood pproh with energy ins nd onsidering kground regions in the (eld of viewF he permi gollortion performed the vine sn in the S qe Y QHH qe energy rngeD while SHH qe Y PH e ws onsidered with rFiFFFsF for the omputtion of sensitivity limits on the hw gmmEry vine )ux nd nnihiltion rossEsetionD setting onstrints on nnihilting hw prtile modelsF pigure 6.1 shows 95% gv limits on the hw nnihiltion rossEsetion < σv > (cm -3 .s -1 ) for these two pulitionsD for n iinsto hw hlo pro(le Figure TFI ! ulished limits on the hw γEry vine nnihiltion ross setionD otined from nlysis t the qg with permiEve @lk dt pointsA nd rFiFFFI @red dt pointsA nd onsidering n iinsto hw hlo pro(le with prmeters α = 0.17D r S = 20kpc nd ρ = 0.39 -0.4GeV.cm -3 t 8.5kpc from the qg @lol hw density t the unAF he presene of gp in energy @no dt pointsA is oserved etween QHH qe nd SHH qeD the energy rnges of those two experiments eing not fully omplementryF 6.1.2 130 GeV Line spectral feature observed in Fermi-LAT data -Fermi Hotspot sn epril PHIP gF eniger reported QFPσ detetion of vine signl t IQH qe in the qg region with permiEve dtD providing plusile hint for the detetion of n exoti γEry signl nd whih ould e ttriuted to nnihilting hw ITPF RQ months of permiEve puli dt were nlysed @independent workD not relted to the permi gollortionA in the qg regionD with energies etween PH qe nd QHH qeD nd found RFTσ indition for the presene of gmmEry vine t IQH qeF king into ount the lookEelsewhere e'etD the signi(ne is QFPσF st orresponds to n exess of out SH gmmF everl FyFs hve een onsidered nd optimized for hndling di'erent hw hlo pro(lesF pigure 6.2 shows the dt events ounts in the VH qe to PHH qe energy rnge with the signl exess t IQH qeD for the hw iinsto pro(leF sn terms of nnihilting hw this IQH qe vine signl orresponds to n nnihiltion rossEsetion of < σv >= (1.27 ± 0.32 +0.18 -0.28 ) × 10 -27 cm -3 .s -1 for n iinsto pro(leD nd < σv >= (2.27 ± 0.57 +0.32 -0.51 ) × 10 -27 cm -3 .s -1 for xp pro(leF region with H.E.S.S.II e following externl permiEve dt pulition hs een sumitted in tune PHIP y hF pinkeiner nd wF u ISQ nd on(rmed the results from gF eniger out the presene of IQH qe vine feture with QFU yers of dt t the qgF e signi(ne of Sσ ws found for IPW qe vine signlD whih trnsltes to QFUσ with trils ftorF ith set of optimized FyFsFs they hve lso found tht etter (t is otined when onsidering sptil o'set of the entre of the hw hlo with respet to the qgF sn prtiulr signi(ne of SFSσ is rehed when onsidering hw hlo o'set of -1.5 • longitude from the qg @in qlti oordintesAD orresponding to distne of PHH p from the qgF fut this est (t result is lso ontminted y lrger tril ftorF he possiility of qlti hw hlo tht would e o'set from the qg is not expeted from ommon hw hlo models in spirl glxyD nd remined n open question t tht time Y prom tht time this IQH qe vine signl hs lso een extensively investigted y the permi gollortion itself whih reported rossEhek results in vine sn pulition in PHIQ IHF hey hve used the sme QFU yers of permiEve dt s hF pinkeinerD ut hve not onsidered ny (t with hw hlo o'set from the qgF he est (t for vine serh hs een otined for IQQ qe vine with lol signi(ne of QFQσD whih orresponds to only IFSσ with tril ftorF he di'erene of Q qe with respet to the IQH qe vine n e explined y the use of n improved lirtion for the permiEve dtF pinllyD the evolution of this IQH qe vine with more oservtion time hve lso een onsidered in the pper Y the signi(ne dereses y IH% when going from QFU yers of dt tking to RFR yersF sn onlusionD the IQH qe vine feture hs een deteted y externl uthors nd y the permi gollortion with the highest glol signi(ne of QFUσ for hw hlo o'set of EIFS • from the qgF fut ll those pulished exesses IQH qe were found using the sme permiEve puli dtD nd re t the present time disproved y the use of lrger sttistisF wost reent studies reported in PHIR pulitions ttriute tht exess to n unfortunte sum of sttistil nd systemti unertintiesF elso the vine feture seem to hve rther smller resolution thn the energy resolution of the instrumentD this eing onsistent with sttistilGsystemti )ututionF yn the other sideD over the yers gF eniger hs lso produed results with more permiEve dt nd stiking to the sme nlysis onditions @nd sme lirtionA s for its initil IQH qe vine detetion in PHIPF sn tht frmeD (gure 6.3 shows the evolution of the lol signi(ne of the IQH qe vine with more umulted sttistisD showing tht the lol signi(ne vried from RFTσ to QFTσ etween PHIP @gF eniger detetionA nd PHIRD nd now follows n evolution omptile with sttistil )ututionsF roweverD the hypothesis tht this vine feture ould e signl is t the present time exluded t > 3σ only nd ler nd de(nitive rejetion of tht γEry vine in the qg region would only e hieved y rossEhek nlysis from n independent experimentF end rFiFFFss is the one @nd onlyA present experiment tht ould on(rm or in(rm the IQH qe vine signl oming from the qg regionF 6.1.3 General strategy with H.E.S.S.II ine the vine feture t IQH qe hs een of very high interest in the pst yers in the hw serh ommunityD it lso rised interest within the rFiFFF gollortion s IQH qe signl is essile t the lowEend of the energy rngeF permiEve nd rFiFFF shre omplementry energy rnges for very high energy gmmEry serhes nd re oth le to nlyse the qg regionF his is not the se for other groundEsed gmmEry gherenkov experiments like weqsg nd erits tht re loted in the xorthern hemisphereF gonsequentlyD there re no other gmmEry experiments to dte tht n serh for vine feture t IQH qe in the qg regionF he ide of rossEhek nlysis with rFiFFF would llow to on(rm or exlude tht vine signl de(nitively with Sσ on(dene levelF his nlysis is however di0ult sine the vine feture lies t the lowEend of the energy rnge overed y rFiFFFD de(ned t ∼ VH qe for low zenith oservtionsF e stndrd rFiFFFs dt nlysis my require to set sfe energy threshold tht is ove VH qe for stndrd soures in order to void eing dominted y systemtis in the events reonstrution t low energiesF es stted in 6.1 the rFiFFFs vine nlysis pper pulished in PHIP relesed hw limits for vines > 500 GeV onlyF ell the interest for IQH qe vine serh with rFiFFF omes then with the 5 th telesope 4gS4 dded in PHIP with expettion of lowering the physil energy threshold down to SH qeF ith rFiFFFss it is now possile to extend the lowEend of the nlysis rngeD llowing vine serhes down to IHH qe nd investigte the spei( se of the IQH qe fetureF he generl ims for vine serhes with rFiFFFss re then the following X

• Produce complementary DM limits with published Fermi and H.E.S.S.I papers in the 100 GeV to 500 GeV energy range using H.E.S.S.II (with CT5), covering the existing gap in energy (see Figure 6.1). Limits for a wider Line scan up to 2 TeV will also be considered

• Investigate the specic case of the reported 130 GeV Line signal, leading to conrmation or rejection of the Line feature. For this purpose H.E.S.S. data were taken in 2014 in a scan conguration along the Galactic Plane and covering the best t position of the reported excess

• Since the best t results for that 130 GeV Line feature has been obtained by D. Finkbeiner for a DM halo shifted by -1.5 • longitude from the GC (l = -1.5 • ; b = 0 • ) it has been decided to focus the DM Line searches in the region of the "Fermi Hotspot" as called in the whole chapter. Limits for the large Line scan [100 GeV ; 2 TeV] as well as a deeper investigation of the 130 GeV Line feature is then considered for a DM halo centred at the position of the Fermi Hotspot (l = -1.5

• ; b = 0 • )
• The Line analysis is performed with the Full Likelihood method that has been fully described in chapter 5. First the procedure is applied on MC data. Here the background event distribution is generated according to the PDF shape extracted from OFF regions around the Fermi Hotspot position, instead of considering the pure MC background PDF that was used in Chapter 4 for studying the general performances of the method. The analysis is then performed on H.E.S.S.II data taken in 2014.

6.1.4 Challenges for a 130 GeV Line-like spectral feature detection with H.E.S.S.II Astrophysical environment he hoie of vine serh t the permi rotspot position ene(ts from eing very exoti se in the serh for new physisD nd in the mentime simpli(es the nlysis sine we don9t hve to del with the entrl soure gittrius eB @gr eBA s n strophysil γEry kground ontriutionF rowever n nlysis lose to the qg remins very omplex s qlti di'use emission is present long the whole qlti lneF he di'use γEry ontriution nd the osmiEry kground omponent s well will e hndled together onsidering kground regions round the permi rotspot with some of them lying in the qlti lneD nd unertinties on the ontriution of the di'use omponent will e derivedF he presene of the nery extended soure ri tIURIEQHP @studied in ghpter 4A in the permi rotspot region is lso triky issue sine it is di0ult to estimte its ontriution in terms of γEry emissionF he other known strophysil soure ner the region with H.E.S.S.II Table TFI ! vist of exlusion regions in the qg region for the permi rotspot vine nlysis permi rotspot is ri tIURSEQHQ ITF st will e exluded from the nlysis using irulr exlusion region round tht soureD s sme s for the entrl soure gr eBF pigure 6.4 shows rFiFFFs mp of the qg region in glti oordintes with the position of the permi rotspot nd nery strophysil soures gr eBD ri tIURIEQHP nd ri tIURSEQHQF elso exlusion regions re set round known supernov remnnts @xA qHFWCHFI nd qHFQCHFH tht re loted long the qlti lne in positive glti longitudesF hese two x re su0iently fr from the permi rotspot position to not interfere with the FyFsF ut re exluded s they my interfere with the ypp wole regionsF le 6.1 lists ll the onsidered exlusion regions with respetive positions in glti oordintes nd rdil extensions in degreesF yther possile strophysil ontriutions my not hve signi(nt impt on the vine nlysis sine they re under the level of the glti di'use emission @he di'use emission omponent will e hndled within the pull vikelihood methodAF Analysis energy range purthermoreD the ility to produe nlysis results t sfe energy threshold of IHH qe with rFiFFFss is more omplited thn expeted sine it strongly relies on the progresses of the frenh rFiFFF softwre for lirtion nd reonstrution of gmmEry eventsF ehing the expeted SH qe energy threshold with rFiFFFss tkes time sine it requires huge e'orts from the whole rFiFFF gollortion to get the new 5 th telesope opertionl t its est performnesF sn prtiulr the nlysis performnes re optimized on known lirtion soures (rst @eFgF gr xeuleD u PISSEQHRA nd getting lower nd lower in energy threshold through nlysis softwre versionsF et tht time 4sfe4 energy threshold of ∼ISH qe n e hieved for low zenith ngle soures with stndrd nlysis utsD ove whih systemtis on the reonstrution of the γErys re under ontrolD while events strt to show up t ∼ VH qeF he IQH qe vine feture is then loted etween the physil nd the sfe energy thresholds of rFiFFFss where systemtis hve to e hndled very refullyF his onstitutes the min di0ulty for investigting the IQH qe vine feture t the permi rotspotF region with H.E.S.S.II 6.2 R.O.I. optimization he hoie of the region of interest @FyFsFA or 4yx4 region is primordil for the vine nlysisD nd orresponds to the nlysis region tht ontin most of the γEry events from the studied soureF por stndrd pointElike strophysil soure the FyFsF should point t the entre of the soure nd hve irulr extension orresponding to the ngulr resolution of the instrumentF his on(gurtion o'ers the highest signi(ne for the exess signl sine lrger FyFsF would just ontin more kground eventsF por n extended soure the hoie of the FyFsF requires dditionl studiesF sn the se of serh for hrk wtter the expeted signl is extended nd the hoie of the FyFsF will depend on the hrk wtter hlo pro(le Y the FyFsF should point t the supposed entre of the hw hlo nd its irulr extension n e optimized suh tht highest signi(nes re rehed for the hw signl omponent nd dditionl ontriutions minimizedF por the present nlysis there is no strong strophysil soure t the ext position of the permi rotspotD only ontriution from the γEry di'use emissionF he qg nd the extended soure ri tIURSEQHQ re fr enough so tht irulr region up to 0.5 • n e esily de(ned round the permi rotspot for the vine nlysis without interfering with the exlusion regionsD nd tht would ontin most of the hw densityF Optimization of the R.O.I. size :

he pull vikelihood proedure ws used on wg dt smples tht inlude ontriutions from line signlD osmiEry kground nd di'use emissionF his llowed setting the optiml FyFsF size for the vine serh t the permi rotspot positionF he signl nd kground events were produed ording to wg signl nd kground hp shpes s in ghpter 5 @only for this FyFsF studyD s ypp dt will e used in the following dt nlysis setionsAF he optimiztion is mde on IQH qe vine for SH hours of oservtion timeD nd vikelihood (t is perfomed on VH qe Y I e energy rnge he wg proedure is repeted SHH timesF he rFiFFFss tereo on(gurtion @t lest P triggering telesopesA is used with stndrd uts for reonstruting the γEry eventsD in prtiulr the ssoited response funtions re lso used for setting the expeted vine signl hp shpeF he input numer of vine signl events were derived from the eniger vine nnihiltion rossEsetionD nd onsidering xvrroEprenkEhite @xpA hrk wtter hlo pro(leF he numer of hdroni kground events were otined from the nlysis of ypp kground regions round pointElike soure u PISSEQHRD nd dding orretion ftor to ount for the higher xf level present in the qg regionF he numer of di'use emission kground events oming from the qlti lne is evluted y extrpoltion of the di'use emission level in rFiFFFs Y this numer hs een provided y uF worå t the tokholm niversityF he fkground hp @hdrons C di'useA spetrl shpe is set from wg simultions smered y sFFpFsF Finally, the signicance of the reconstructed 130 GeV Line signal is computed with the Full Likelihood procedure for a set of R.O.I. angular extensions ranging from 0.1 • to 0.5 • D s well s performnes on the reonstrution of the vine signl frtion nd energy @is with respet to input vlues nd unertinty t TV7 gv lirted on the SHH simultionsAF e rossEhek of the FyFsF optimiztion is lso performed y uF worå with n lterntive inned likelihood pprohF Figure TFS ! FyFsF optimiztion X xumer of wg input events for the signl nd kground omponents @A nd ssoited vine frtion @A for set of FyFsF ngulr extensions vrying from 0.1 • to 0.5 • pigure 6.5 shows the evolution of the numer of signl nd kground events with respet to the FyFsF ngulr extension @on the leftAD nd the evolution of the orresponding vine signl frtion tht is going to e reonstruted @on the rightAF pigure 6.6 displys the energy distriutions of the events in 0.1 • @left plotA nd 0.5 • @right plotA FyFsF respetivelyD with the IQH qe vine signl exess oloured in redF pigure 6.7 shows the resulting performnes for the vine signl reonstrution with inresing FyFsF he vlues re summrized in le 6.2F hile the input vine frtion dereses from out S% to QFS% when inresing the FyFsF extensionD the signi(ne of the reonstruted vine frtion inreses from P to RFV nd seems to stilize just under S sigms for even lrger FyFsFsF elso performnes on the reonstrution of the line frtion nd energy @is nd resolutionA re improved for the lrgest FyFsF extensionsF e turning point is expeted to e oserved in the evolution of the signl signi(ne for FyFsF sizes elow 0.5 • D due to the hw density tht is mostly on(ned t the entre of the hloF rowever the present results n e explined y the glol event sttistis ville for the pull vikelihood method X the method n e0iently identify signl omponent in the dt if nd only if there is minimum numer of signl nd kground ounts in the dt so they n e sttistilly ttriuted to their respetive signl nd kground hpF sn the present se FyFsF of 0.1 • only ontins ∼IHH vine signl events nd PHHH kground @hdrons C di'useA events for SHh or oservtion time whih is then sujet to higher sttistil )ututions in the energy distriution of the events ompred to FyFsF of 0.5 • s seen on (gure 6.6F sn onlusionD for suh n nlysis with very low input signl frtions @only few perentA the dominnt riteri for improving the performnes of the pull vikelihood method is the glol event sttistisF The largest R.O.I. is then privileged for this analysisD ut we should not forget tht the FyFsF size is lso limited y tehnil onstrintsD overed in the next prgrphF Figure TFT ! FyFsF optimiztion X inergy distriutions of the wg input events @signl C kgroundA for FyFsF ngulr extension of 0.1 • @A nd 0.5 • @A Figure TFU ! FyFsF optimiztion results X vine signl signi(ne @A nd is nd resolution on the reonstrution of the input vine frtion nd energy @A for set of FyFsF ngulr extensions vrying from 0.1 • to 0.5 • F esults re produed for IQH qe vine nd for SHh of oservtion time with the tereo telesope on(gurtionF he is is the shift etween the true nd the reonstruted vlues of the prmetersD while the resolution is the unertinty t TV7 gv on the reonstruted prmetersF esults re lirted on SHH simultions vine frtion reoF vine energy reoF FyFsF @ • A η input @7A is @7A res @7A is @7A res @7A igni ( Technical limitations for the R.O.I. size :

he FyFsF optimiztion is limited y the following tehnil onstrints X • he FyFsF nnot exeed the limits of the (eld of view whih is of out ±2 • for rFiFFFss nlysisF • he PhEeeptne for gmms strts deresing rpidly for ngles > 1 • resulting in lrger systemtis t those ngulr extensions when ounting for the eptne orretion ftor • he ngulr resolution of the instrument @or the FFpFA de(nes the lower ound for the FyFsF sizeF st orresponds to ∼ 0.17 • for rFiFFFss wono nd ∼ 0.1 • for rFiFFFss tereo onsidering stndrd uts for the reonstrution of the γElike eventsF • he exlusion region round ri tIURSEQHQ limits the mximum size of the FyFsF to ∼ 0.5 • if we stik to irulr region • e too lrge FyFsF ngulr extension limits the numer of ypp kground regions tht n e de(nedF e studied the impt of the FyFsF size on the numer of ypp wole regions reted in the (eld of view of single run for n nlysis t the permi rotspot positionF es n exmple pigure 6.8 shows the evolution of the numer of ypp regions for run WRQIH from the vine n dt ontrol smple @see setion 6.5A pointing t gr eB for set of FyFsF ngulr extensions vrying from 0.1 • to 0.6 • F his lso ounts for the exlusion regions de(ned y red irlesF et lest RES ypp regions were required for getting su0ient kground sttistisD neessry for the omputtion of the kground hp in the pull vikelihood method @see 6.8AF his orresponds to mximum FyFsF extension of 0.4 • F Cross-check study :

ixtended studies for the FyFsF optimiztion were mde y uF wor @tokholm niversityA using the inned oisson likelihood method with side nds in energy desried in ghpter 5 @5. he strophysil soure ri tIURIEQHP hs een introdued in ghpter 4 in the ontext of spetrl rossEhek nlysis performed for iF yF engunerF his extended strophysil soure is very lose to the permi rotspot position nd lies within the 0.4 • FyFsF sts )ux ontriution in omprison to the glti di'use emission nd the eniger IQH qe vine hs een investigted y extrpolting the rFiFFFs spetrum on pigure 4.8 @in ghpter 4A to lower energiesF he )ux t IQH qe for the di'use emission omponent is extrpolted from the pulished spetrum in TVF he )ux for the hw vine signl is derived from the eniger nnihiltion rossEsetion for n iinsto hw hlo pro(leF rere )uxes for the vine nd for the di'use emission re oth lulted for Q referene FyFsF in order to study the evolution of the ri tIURIEQHP omponent with respet to the size of the signl regionF 0.1 • nd 0.17 • orrespond to the stndrd energy resolutions for the rFiFFFss wono nd tereo telesope on(gurtionsD respetivelyD nd 0.4 • orresponds to the optimized FyFsF disussed in setion 6.2F he results re summrized in le 6.3F pluxes from the gr xeul serve s referene vlues for omprisonsD the vlues t IQH qe eing extrpolted from the pulished rFiFFF spetrum in PIF prom tht tle the )ux ontriution from ri tIURIEQHP is omprle to the level of the IQH qe vine signl for 0.1-0.17 • FyFsFD ut is ftor S less importnt for the optimized 0.4 • FyFsF elso its ontriution is lmost I order of mgnitude less importnt thn the di'use emission for lrge FyFsF

In conclusion the impact of HESS J1741-302 is small for the 130 GeV Line analysis for a large R.O.I. such as 0.4 0.56% qlti di'use emission @ysa0.1 • A 1.77e -11 0.36% 1.66e -13 0.44% qlti di'use emission @ysa0.17 • A 5.12e -11 1.04% 4.78e -13 1.27% qlti di'use emission @ysa0.4 • A 2.83e -10 5.74% 2.65e -12 7.05% IQH qe vine @gF enigerA @ysa0.1 • A 1.33e -11 0.27% IQH qe vine @gF enigerA @ysa0.17 • A 3.14e -11 0.64% IQH qe vine @gF enigerA @ysa0.4 ri tIURSEQHQ strophysil soure hs een studied y the rFiFFF gollortion @IWD IUAF e 0.35 • irulr exlusion region hs een de(ned round tht soure X this rejets most of the ssoited strophysil gmm events from the nlysisF rowever the soure is very extended @ sfe exlusion region of 0.9 • ws set for stndrd rFiFFFs nlysisA nd then smll frtion of the events my ontriute to the gmm events in the signl regionF e dedited study hs een performed y uF wor who investigted the numer of strophysil γEry events from tIURSEQHQ tht re polluting the permi rotspot nlysisF he )ux from tht soure is derived from the pulitions nd extrpolted t low energies for totl energy rnge of UH qe Y I eF IQV gmm events from ri tIURSEQHQ nd for SHh of oservtion time were otinedD ompred to VPS events for the IQH qe vine from gF enigerF

In conclusion the impact of HESS J1745-303 is small for the 130 GeV Line analysis when using a 0.4 • R.O.I., and represent ∼ 0.6% of the total number of reconstructed gamma events in the R.O.I. (hadronic background included). 6.5 Line scan Data Sample 6.5.1 Observations of the Line Scan elmost IHHh of dt tken in PHIQ nd PHIR with rFiFFFss nd pointing t the qg @with wole o'sets etween 0.5 • nd 1.1 • A re ville for nlysisD ut suh pointing positions do not llow n optiml nlysis t the permi rotspot whih is too fr from the qgF sn this sitution systemtis from eptne in the pFyFF ould e importntD espeilly for the reonstrution of possile fint hw signlF st is then preferle to hve set of runs with optiml wole o'sets round the permi rotspot positionF his dt hs een tken in pring PHIR nd will e nmed 4vine n4F he pointing strtegy for the sn is represented on (gure 6.9F he sn is performed with 0.7 • steps in longitude nd with ±0.8 • ltitudeF hose IH pointing positions were orgnized in two distint groupsD tht re lled 4left4 nd 4right4F he 4left4 dt smple onsists in R pointings @U to IHA tht re entred on the qgF he 4left4 dt is used s ontrol smple for dt qulity nd lirtion heksF he 4right4 dt smple onsists in the T other pointings @I to TA tht hve glol PhEeptne entred on the permi rotspotF hose runs re the min dt smple for vine nlysis t the permi rotspotD nd will e used for produing results t IQH qe nd lso for wider rnge of vine energiesF he vine n dt hs een tken through Q oservtion periodsD epril @eriod RAD tune @eriod TA nd tuly @eriod UA of PHIRF hese dt smples re nmed 4vine n RD T nd U smples4F et lest R telesopes were requested for ensuring good reonstrution of the γEry eventsD nd inluding gS s well s low zenith ngles @`PH • A for low energy threshold lose to possile IQH qe vine fetureF he totl oservtion time efore dt qulity heks is RI hours whih orresponds to WS runs @t lest SHh of oservtions were requested for the vine n in PHIRAF he numer of runs in eh of the Q periods of oservtions is detiled in le 6.4F he numer of runs tht pssed run qulity seletion uts @see 6.5.2A re lso represented with its distriution within the 4left4 nd 4right4 dt smplesF eriod @PHIRA fefore seletion efter seletion Table TFS ! un qulity seletion uts for the vine n dt smple he glol run nd telesope informtion tht orrespond to the most relevnt qulity seletion riteri for the vine n dt smples R @PP runsAD T @QI runsA nd U @RP runsA re shown on pigures 6.10D 6.11 nd 6.12 respetively @the histogrms re extrted from the risrunqulity softwreAF his inludes in prtiulr the distriution of the numer of triggering telesopesD the run durtionD the men zenith ngle over the runD the entrl nd telesope trigger rte informtion or the roken pixel frtion in the mersF he rejeted runs re shown with red res or irlesF he only exeption to these qulity uts is run WRSQW @period RA tht displys too lrge w of trigger rte vlues @round PH%A on Q telesopes ut shows overll good qulity for ny of the other riteriF his run is useful sine the R dt smple lks of su0ient run sttistisD nd ws not rejeted @R will e used for tests of the pull vikelihood methodAF region with H.E.S.S.II • requestedF pollowing to this vetD PQ runs @IQ t the permi rotspotA my not e usle for the vine nlysis t IQH qe diretlyD ut re onsidered nywy for the generl vine sn t higher energiesF he use of T dt would require di'erent sFFpF vlues in the simultion proedureF sn onlusionD on totl of WS runsD UT re pssing dt qulity seletion utsD iFeF QH runs @IQFUhA in the 4left4 dt smple for dt qulity nd lirtion heks nd RT runs @IWFWhA in the 4right4 dt smple for the vine nlysis t the permi rotspotF he dt qulity proedure leds to PH7 run loss in the vine n dtsetF 6.5.2.2 Additional selection from background maps en dditionl hek on the individul run kground mps hs een performed on the whole vine n dt smpleF Q runs tht hve weird strutures in their kground mps were identi(edF hey elong to the R dt smple X WRPIVD WRQSU nd WRQSVF pigure 6.13 displys the ssoited kground mpsD in omprison with 4norml4 kground mpF hese unusul strutures use holes in the PhEeeptne mps nd then must e removed from the nlysis dtsetF hose Q runs were lredy exluded from run qulity seletion euse of too high roken pixel frtion in gS @> 10%AF T nd U dt smples do not show suh strutures in the kground mpsF 6.5.3 Un-blinding of the Line Scan P4 dataset qiven the im to disover new signl with the vine nlysis in the qg regionD it hs een deided in greement with the gollortion to set up linding proedure for the vine n dt smpleF his ws motivted to keep the numer of trils s low s possileF roweverD due to the omplexity of the foreseen nlysisD the R dt smple orresponding to QFIh of oservtion time t the permi rotspot ws urned nd extensively used for evluting the generl qulity of the gmm events reonstrution nd for tests nd optimiztions of the pull vikelihood method for the vine serhD espeilly t the lowest rnge of energiesF T nd U dt smples @ITFVh t the permi rotspotA styed linded until ll heks nd optimiztions Conclusions on the nature of the bias he exess seen elow PHH qe in the vine n R dt t the permi rotspot position is systemti is oming from the rFiFFFss reonstrution of the gmm eventsD prior to the pplition of ny nlysis method @yxEyppD vikelihoodD pull vikelihoodFFFA he sme ises re oserved in lnk (elds where no exess is expeted nd in sptil sideEnds round the permi rotspotF st is present in oth wono nd tereo reonstrutionsD ut less pronouned in tereo @signi(ne redued y ftor ∼ 2A s the impt of the gS telesope is more limitedF purther studies hve shown tht the is is rdillyEdependent nd n show up s n exess or hole in the energy distriutions depending on the FyFsF position within the (eld of viewF he prolem is inherent to the reonstrution lgorithm for the γEry events nd uses eptne grdients in the py tht re responsile for wrong normliztion etween the signl nd the kground regionsD leding to unexpetedly lrge ises ner the energy thresholdF Impact for the Line analysis rFiFFFss lirtion nd reonstrution softwres were t this moment only optimized on known strophysil soures nd still require developments for hndling low energy issuesF rFiFFFss is still in softwreEdevelopment phse for mking use of the 5 th telesopeD nd huge e'orts from the rFiFFF gollortion re still set for improvements of the low energy side nd for rehing (xed initil gol of SH qe energy thresholdF his ojetive will e rehed step y step nd in timeEsle whih did not ful(l ompletely the sope of this thesisF et this stte of the rFiFFF softwreD the lowEenergy is hs to e inluded in the vine nlysisF

The Line-like systematic eect at ∼130 GeV has been observed in the P4 dataset and in other control samples as well, where no excess was expected ; this contribution corresponds to 5 to 10% of the data events and dominates over the possible existing DM signal that should contribute at the order of 1 to 2% according to the Weniger annihilation cross-section. In this context it has been decided to consider the null hypothesis for the DM signal at 130 GeV and to make use of the Full Likelihood method to derive conservative upper limits on the Line ux and annihilation cross-section that are intrinsically worsen by the bias.

Hopefully, the extended scan with Lines at higher masses is not limited by that bias and the analysis can be performed safely. Here no excess is observed above 200 GeV in the P4 dataset then upper-limits will be derived for an extended range of DM particle masses. he reonstrution method hs een seleted on the sis of its response funtionsD of the expeted frtions for the potentil hw signl t IQH qe nd of the present sttus of the reonstrution hinsD leding to the est sensitivities for the vine serhF • Background level : he numer of kground events from the vine n R dtset in the optimized 0.4 • FyFsF orresponds to ∼ 22820 events in tereo when resling to SHh of oservtions nd ∼ 42660 events in wonoD ftor of P higher sine only one telesope @gSA is required in the trigger nd lrger ontriution of night sky kground events is reonstruted @see 6.8.2.1AF

• Acceptance for gamma : he eptnes derived from the snstrument esponse puntions @see pigure 5.1A re ∼ 2.1 * 10 4 m 2 in wono nd ∼ 1.5 * 10 4 m 2 in tereo t n energy of IQH qeF he expeted numers of permi vine events hve een lulted from the eniger nnihiltion rossEsetion onsidering hw iinsto pro(le nd from the ove eptne vluesF hey orrespond to ∼ 405 events in tereo nd ∼ 555 in wono in the FyFsF for SHh of oservtion timeD tht trnslte into vine signl frtions η = 1.7% nd η = 1.3%D respetivelyF he wg sensitivity limits produed in ghpter 5 gve onlusions on the minimum frtion required for the reonstrution of vine signls down to PSH qe with WS7 gvD nd is IFS7 in tereo nd IFQ7 in wonoF upposing similr sensitivity limits t IQH qeD the eniger vine signl should just e detetle t WS7 gv with oth reonstrutionsD with slight dvntge for tereoF gonerning lrger mssesD the tereo on(gurtion is preferred s the eptne for gmm eomes muh lrger thn wono @up to ftor of PFSA • Energy bias and resolution : he more telesopes re used to trigger the eventsD the est the stereosopi reonstrution performs nd the lowest the energy resolution isF prom the sFFpFs the energy resolution for the wono reonstrution is worse y ftor ∼ 2 ompred with tereoF he e'et of suh n inrese in the energy resolution ws studied with wg dtsets for the reonstrution of IQH qe vine signl t S7 frtion in tereo telesope on(gurtion @with the inputs further disussed in 6.12A Y when douling the energy resolution the is etween the input nd the reonstruted vlues of the signl frtion η inreses from IFS7 to T7D while the unertinty on η t TV7 gv inreses from SFT7 to TFR7F

• Systematic bias < 200 GeV : prom pigure 6.14 the numer of exess γ events ttriuted to the systemti is @6.5.4A nd to sttistil )ututions re VUFT in tereo nd PRIFS in wono for the vine n R dtsetD supposing no ontriution from the hwF his orresponds to frtions of TFR7 nd VFR7D respetivelyF he ontriution from the systemti is is then less importnt in tereoF hen onsidering lnk (elds round lirtion soure u PISSEQHR @see pigure 6.16A this gp is muh more redued with ontriutions of SFR7 nd SFS7 respetivelyF rowever results with u PISSEQHR nd with the vine n dt re not omprle due to di'erent night sky kground levels nd oservtion onditionsF he pull vikelihood method is performed for severl vine energies rnging from IHH qe to P eF hen n ssoited signl hps is required for eh of the onsidered vinesF et given energy E line the vine spetrl signture is the result of disrete energy smered y the response funtions of the instrument @eptneD energy is nd energy resolutionAF 10 6 events re simulted on qussin entred on (E line + E bias ) nd of width E resolution F hen n histogrm is (lled with these smered energies weighted y the eptne t the true energy E line F he inning is optimized on the kground hpD disussed in 6.8.2F yne (lled this histogrm is (tted y n symmetri qussin funtion normlized to I on the energy rnge of the vikelihood (t @see 6. 1) wg simulted events following powerElw spetrum with omined ontriutions from the di'use @Γ = 2.3A nd hdroni @Γ = 2.7A omponentsD nd smered y the rFiFFFss sFFpFsF his hp ws used in ghpter 5 for the wg performne studies of the methodF

2) fkground events from ontrol smple u PISSEQHRF e dtset of SI rFiFFFss runs tht pssed stndrd tereo qulity seletion uts ws usedD nd ypp wole regions were tken round the pointElike soure @with n ypp region size of 0.4 • A s the representE tive kground events for hp genertionF

3) fkground events from the vine n dt smpleF his hoie seems ovious ut the di0ulty is to evlute the numer of kground events in this omplex region of the sky @see 6. Impact of the Azimuth Angle he impt of the ezimuth engle on the energy threshold hs lso een investigtedF he zimuth ngle of the telesopes is orrelted with the mgneti (eld of the irth tht impts the shower developmentF he impt for the reonstrution of the gmm events is reported to e ∼ 10% on the eptne t the trigger level in rFiFFFs @UQDRIAF pull rFiFFF wg simultions of shower developments re only ville with two vlues for the zimuth ngle X 0 • nd 180 • F his is simply due to storge limittions on the inPpQ serverD those simultions eing memoryEonsumingF e investigted its impt on the rFiFFFss energy threshold y plotting the wg eptnes in wono nd tereo for zimuth ngles 0 • nd 180 • @nd for stndrd xf level of IHH wrzAF his is shown on pigure 6.22F he e'et on the eptne is of out 65% @ftor IFSA in wono nd out 60% @ftor IFUA in tereo t IQH qeF he zimuth ngle hs signi(nt impt on the energy thresholdF he zimuth ngles for the vine n dt re etween 150 • nd 180 • while the wg eptnes nd hps seen on (gures 6.19D 6.20 nd 6.21 were generted with n zimuth ngle of 180 • F he impt of the zimuth ngle is then redued when ompring wg nd vine n hps X quntittive impt nnot e estimted preisely ut the zimuth ngle should still ontriute slightly to the di'erenes seen in the energy thresholds of the di'erent kground hpsF region with H.E.S.S.II 6.10 Systematics ystemtis relted to the pull vikelihood method hve een evluted with wg simulE tions y introduing nuisnes on severl vriles in the vikelihood funtion lultionF e omprison of the di'erent systemtis of the method hs een hieved y onsidering the error on the reonstrution of the vine signl frtion η for input vine energies of IQHD SHH nd VHH qeD for n input frtion η input = 5%D for the tereo telesope on(gurtion nd T OBS = 20h nd pplying the di'erent nuisne ftors individully on eh of the relevnt vrilesF por eh studied systemtisD the error on the reonstrution of η is lirted on SHH simultionsF 6.10.1 Systematics on the I.R.F.s hue to sps unertintiesD shifts were introdued on the input vine energy nd on the vine width in the expression of the signl hpF es wg vine events re still generted t the true energy the resulting errors on the reonstrution of η re evlutedF his wy the systemtis oming from the unertinty on the sFFpFsD iFeF the energy is nd the energy resolutionD were estimtedF he nuisne on the vine energy position is hosen to e reltive vrition of ±5%D while ±20% on the energy resolutionF esults re shown on le 6.7F he systemtis on the sFFpFs re of the order of ±10 -15% in the reonstrution of η nd re lmost stle for the whole rnge of onsidered vine energiesF he systemtis oming from the eeptne were not onsidered here ut re strongly relted to the systemtis on the kground hp desried in the next prgrphF 130 GeV 500 GeV 800 GeV Nuisance range low up low up low up Line energy (GeV) E line ± 5% -6.3% -0.3% -3.7% -11.4% -12.0% -3.8%

Energy resolution (%) E res ± 20% -9.6% +7.5% -14.1% +3.1% -13.9% +1.7% round the input vlue D input = 6% @the numer of di'use events is extrpolted from the rFiFFFs glti di'use emission pperD TVA so tht we vry the di'use frtion etween H7 nd IP7F yn the other hnd nuisne of ±0.2 is introdued on the di'use powerElw index round the input vlue Γ = 2.3D whih resonly overs the possile rnge of unertinties on the spetrl indexF esults re shown in le 6.9 where the unertinties on the knowledge of the di'use omponent re of the order of ±7 -8% on the vine frtion reonstrutionD region with H.E.S.S.II nd re lmost stle for the whole rnge of onsidered vine energiesF hese systemtis re less importnt thn the systemtis on the sFFpFs nd hve moderte impt on the performnes of the pull vikelihood methodF prom le 6.9 we lso notie tht nuisne of -0.2 on the spetrl index hs more importnt e'et thn nuisne of +0.2 X this is due to the ft tht the spetrl index for the hdroni kground is softer @∼ PFUA thn for the di'use emission @∼ PFQAF e negtive vlue of the nuisne ftor rings the di'use index frther from the hdroni index nd the glol kground hp shpe @hdrons C di'useA is then muh more 'eted resulting in lrger systemti e'etF sn onlusionD the modelling of the lowEend of the kground hp is the dominnt soure of systemtis for vines ner the energy threshold of the experiment @`QHH qeAF st is losely relted to the eptne of the instrument t low energiesD however the di0ulty here doesn9t ome from unertinties on the eptne funtion ut reltes to the hoie of kground hp tht is good representtion of the kground omponent in the hosen FyFsFD most importntly t low energiesF his rgument strongly motivted the ide of onsidering kground regions in the sme (eld of view s the permi rotspot for the nlysisD s it hs een explined in setion 6.8F 6.10. Systematics 201 he unertinties on the sFFpFs @energy is nd energy resolutionA lso ontriute signi(ntly to the systemtis of the method nd espeilly dominte over the kground hp systemtis t energies ove QHH qeF rowever the sFFpFs re derived from full wg simultions of the ir showers nd of the telesopes nd n e onsidered s relile s soon s we re slightly ove the energy threshold of the instrumentF he hoie of tking ±5% nuisne on the energy is nd ±20% on the energy resolution for SHH nd VHH qe vines is then sfe estimtion nd relted systemtis on the reonstrution of η re expeted to e less importnt thn presented in this studyF pinlly the modelling of the di'use emission omponent is still very omplex issue nd hs not een overed yet with the seond phse of rFiFFF he hoie of resonly lrge rnge of vlues for the nuisnes introdued on the di'use frtion nd spetrl index is then justi(ed nd its ontriution to the systemtis s presented in le e new version of the rFiFFF softwre hs een relesed in tune PHIS nd proposes new developments suh s n improved eptne grdient orretion module for hndling systemti ises disussed in 6.5.4D nd improved uts on disriminnt vriles for the reonstrution of the gmm eventsF e lot of e'orts were lso put into the hievement of orret ypp event normliztion nd its stility with respet to seletion utsF et presentD Q di'erent sets of uts nd seletions re ville for the reonstrution of the γEry events @tndrdD voose nd pintAD optimized on known lirtion soures eFgF the gr xeulD u PISSEQHR nd q ISSQCIIQ to improve the exess signi(ne nd the signlEtoEkground rtioF tndrd uts were onsidered for the vine nlysis under the previous softwre version @vFPVAF hese uts di'er in the minimum numer of photoEeletrons produed in the mer pixelsD in the gmmExf event seprtion @xf qoodness disriminting vrileA nd in the optiml FyFsF size for the nlysis of pointElike souresF voose @relxedA uts re provided for the nlysis of wek γEry soures when highest possile numer of γEry events is expeted t low energiesD while pint @striterA uts re often used in se of very wek ut pointElike strophysil signlF por the present vine nlysis the FyFsF size stys (xed t the vlue of 0. he pull vikelihood proedure hs een performed on wg dt smples in order to investigte the sensitivity of the method for vine signl detetionF sn ghpter 5 the generl performnes of the method were studied for the reonstrution of vine signls over PSH qe with frtions η input ≥ 5% nd upperElimits on the )ux were lso derived for η input = 0F sn prtiulr the FyFsF ws irulr region of extension 0.25 • D the kground hp ws otined from pure wg dt nd the results were produed for referene oservtion time of SHhF

Here MC studies are done for a large mass scan between 100 GeV and 2 TeV with a R.O.I. centred at the Fermi Hotspot position, considering all optimizations described in the previous sections and an observation time in accordance with the available Line Scan data. In particular the background PDF is derived from OFF regions in the FOV and follows the parametrization given in Table 6.11. Since no signicant excess has been observed in the Line Scan P4 data, only upperlimits on the Line signal fraction are computed, on the Flux and on the velocityweighted annihilation cross-section of the DM particles into two gammas. The particular case of a 130 GeV Line is also investigated with upper-limits compared to the reported excess in Fermi-LAT data.

6.12.1 MC simulation conditions e onsider region of interest of 0.4 • round the permi rotspot (l = -1.5 • ; b = 0 • )F he ltest version of the rFiFFF softwre @see 6.11A is used to estimte the numer of simulted kground events in the permi rotspot regionD onsidering the tereo telesE ope on(gurtion nd voose uts for the reonstrution of the gmmElike eventsF he vine signl hp is derived from the orresponding rFiFFFss sFFpFsF he kground hp is otined from ypp wole regions round the permi rotspot with exlusion reE gions set on gr eBD x qHFWCHFI nd qHFQCHFH nd on the nery soure ri tIURSEQHQF ell wonteEgrlo studies re performed with SHH simultions for sttistil lirtion of the results nd for determintion of the systemtis in the upperElimits lultionF xo vine signl events re simulted @η true = 0A for the limits lultionF he wg events in the FyFsF re generted diretly from the kground hp funtion nd for T OBS = 20h orresponding roughly to the totl oservtion time ville for the vine n dt smple in PHIR pssing qulity seletion utsF he orresponding numer is derived from the stndrd nlysis of the vine n R dt smple y extrpolting the numer of yx events to PHh X it orresponds to N ON = 24280 efore energy utsF his inludes oth the osmiEry nd the di'use emission omponentsF he totl numer of kground events in ypp regions is lso required s n input for the oisson term lultion X here the verge numer is tken s α * N ON where α = 4.65 @normliztion ftor etween yx nd ypp regions in the R dtsetA nd onsidering sttistil )ututions round tht verge vlue for eh of the SHH simultionsF ell input numers re summrized in le 6.12F Table TFIP ! ummry tle X wg simultion onditions for the pull vikelihood performne studies 6.12.2 DM sensitivity limits for the mass scan : 100 GeV → 2 TeV ensitivity limits re lulted for wide rnge of hw prtile msses @iFeF vine energiesA etween IHH qe nd P eF he following msses re onsidered @in eA X HFID HFIQHD HFPD HFQD HFRD HFSD HFTD HFVD ID nd P eF por eh mss the 95% gv limit on the reonstruted vine frtion η in the FyFsF is lulted s result of the pull vikelihood (tF he energy rnge hs een optimised in 6.6 nd is set to VH qe Y I e for vines ≤ SHH qe nd PHH qe Y Q e for vines > SHH qeF por given mss the 95% gv limit on the vine signl frtion η 95%CL is onverted into limit on the numer of gmm exess events N 95%CL γ using the formul X

N 95%CL γ = N background × η 95%CL 1 -η 95%CL @TFRA
where N background is the numer of kground events in the FyFsF he proedure is repeted with SHH simultions nd then the medin limit is tken s the 95% gv limit on the numer of gmm exess events s shown on pigure 6.28F prom N 95%CL γ the orresponding limit on the γEry )ux is derived with the formul X

Φ 95%CL = N 95%CL γ T OBS × Emax E min dN dEγ (E γ )dE γ Emax E min A ef f (E γ ) dN dEγ (E γ )dE γ @TFSA
where T OBS is the oservtion time @in seondsAD A ef f the e'etive re @in m 2 A nd dN dE the di'erentil energy spetrum of the expeted γEry signlF region with H.E.S.S.II Figure TFPV ! glultion of 95% gv limits on the reonstruted numer of vine signl events with the pull vikelihood methodF veft (gure X herivtion of oneEsided 95% gv limit on the vine frtion for one simultionD whih onverts into numer of reonstruted vine signl eventsF ight (gure X gomputtion of the 95% gv limit on the numer of vine signl events y tking the medin vlue over SHH simultions por monohromti γEry vines χχ → γγ X

dN dE γ (E γ ) = 2 × δ(E γ -m χ ) @TFTA
where the ftor P results from the nnihiltion of hw prtiles into two gmmsF he expression of the )ux is then simpli(ed X

Φ 95%CL = N 95%CL γ T OBS × A ef f (m χ ) @TFUA
he limits on the )ux per solid ngle unit re shown on pigure 6.29F hey re divided y ∆Ω = 2π(1 -cos(θ ROI )) = 1.531 * 10 -4 sr in order to e FyFsF independent nd to llow omprison with former rFiFFFs limits R whih were derived with muh lrger FyFsF @1 • extensionAF he lue dt points orrespond to the omputed wg limits with PHh of oservtion timeF hese limits re resled to PFVh @mgent solid lineA nd IHHh @yellow solid lineA orresponding to the eptneEorreted livetime of the vine n R dtset nd to the referene oservtion time for omprisons with rFiFFFs limitsD respetivelyF i'ets on the limits due to systemti unertinties on the kground hp re represented y dshed lue lineF es omprison the red dt points represent the )ux limits pulished with rFiFFFs R strting from SHH qeD for IIPh of oservtions t the qgF he otined limits re ompleting the rFiFFFs sn t energies under SHH qe for omprle livetime of ∼ 100hF 6.12. Monte-Carlo studies & performances of the Full Likelihood method 209

Figure TFPW ! pull vikelihood results X wg plux limits t 95% gv for the mss sn etE ween IHH qe nd P eF he )ux is expressed in γ.m -2 .s -1 nd per sterdinF he lue dt points represent the omputed limits with PHh of oservtion time nd tking the meE din vlue on SHH simultionsF i'ets on the limits due to systemti unertinties on the kground hp re represented y dshed lue lineF hese limits re resled to IHHh of oservtion time @yellow solid lineA nd PFVh @mgent solid lineA for respetive omprisons with the rFiFFFs pulition nd the vine n R eptneEorreted oservtion timeF esults from the rFiFFFs pulition R re lso inluded in the (gure X vimits for the qg nlysis @IIPh of dtA re shown with red dt pointsD nd the lk solid lines represent the expeted limits from wg simultions with 68% gv regions s grey res Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II por T OBS = 20h orresponding to the totl ville livetime in the vine n dtset the wg )ux limit t IQH qe nd SHH qe re X Φ 95%CL (130GeV ) = (3.73 + 1.39syst) × 10 -4 γ.m -2 .s -1 .sr -1 Φ 95%CL (500GeV ) = (0.52 + 0.12syst) × 10 -4 γ.m -2 .s -1 .sr -1

he vlues for the omplete mss sn re summrized in le 6.13F vimits on the veloityEweighted hw nnihiltion rossEsetion hve een derived with the formul X

< σv > 95%CL = 8πN 95%CL γ Φ astro T OBS × m 2 χ Emax E min A ef f (E γ ). dN dEγ (E γ )dE γ @TFVA
where Φ astro is the strophysil ftor for the onsidered FyFsF nd hw hlo pro(leF he priniple of the strophysil ftor lultion hs een introdued in ghpter 1F sn order to set omprle limits with permi IH nd rFiFFFs R ppers hw iinsto hlo pro(le ws used X

ρ Einasto (r) = ρ s . exp - 2 α E r r s α E -1 @TFWA
with α E = 0.17 nd r s = 20kpcD normlized to ρ(r = r 0 ) = 0.39GeV.cm -3 t the position of the un resulting in ρ s = 0.079GeV.cm -3 F he distne from the un to the entre of the hw hlo is r 0 = 8.5kpcF prom the hlo pro(le we derived the strophysil ftor integrted on the 0.4 • FyFsD whih leds to the vlue of Φ astro = 2.46 * 10 21 GeV 2 .cm -5 F es omprison the strophysil ftor for the 1 • FyFsF proposed in the rFiFFFs pper is 4.43 * 10 21 GeV 2 .cm -5 F por the line serh the formul (6.8) simpli(es to X

< σv > 95%CL = 8π × m 2 χ × N 95%CL γ 2 × Φ astro × T OBS × A ef f (m χ ) @TFIHA
pinlly s disussed in setion 6.9 frtion of the expeted hw γEry events is lso present in the ypp regions @tht re used for the kground hp lultionA nd represents ∼ 25% of the hw γEry events in the FyFsF he < σv > limits hve een worsen y PS7 to ount for tht e'etF For T OBS = 20h the Monte-Carlo < σv > limits at 130 GeV and 500 GeV are :

< σv > 95%CL (130GeV) = (0.62 + 0.23syst) × 10 -27 cm 3 .s -1 < σv > 95%CL (500GeV) = (1.25 + 0.29syst) × 10 -27 cm 3 .s -1
The values for the complete mass scan are summarized in Table 6.13. The limit at 130 GeV is lower than the C. Weniger annihilation cross-section (< σv > Weniger (130GeV) = (1.27 ± 0.32 +0.18 -0.28 ) × 10 -27 cm 3 .s -1 ) by a factor of 2, and a factor of 1.5 when including systematics on the background PDF. With the Full Likelihood method and the available 20h Line Scan dataset it is then possible to exclude the 130 GeV Line feature with more than 95% condence level. elso the omprison with former rFiFFFs limits is not ovious s the present nlyE sis is sed on hw hlo o'Eentred from the qgF his prtiulr on(gurtion gets rid of the prolems used y the entrl soureD while gr eB ws exluded in the rFiFFFs pper msking the entre of the hw hlo in the mentimeF rowever the hw hlo pro(les re identil in oth nlyses nd re lwys entred on the de(ned FyFsF sn tht ontext the < σv > limits re omprle ut di'erent results re expeted in the future with foreseen rFiFFFss vine nlysis pulitions t the qgF Figure TFQH ! pull vikelihood results X wg < σv > limits t 95% gv for mss sn etween IHH qe nd P eF he limits re expressed in cm 3 .s -1 F he lue dt points represent the omputed limits with PHh of oservtion time nd tking the medin vlue on SHH simultionsF i'ets on the limits due to systemti unertinties on the kground hp re represented y dshed lue lineF hese limits re resled to IHHh of oservtion time @yellow solid lineA nd PFVh @mgent solid lineA for respetive omprisons with the rFiFFFs pulition nd the vine n R eptneEorreted oservtion timeF esults from rFiFFFs R re represented y red dt pointsD nd results from permiEve IH re shown with lk dt pointsF he vlue orresponding to the IQH qe vine from gF eniger ITP is represented y green squre dt point with error rs 6.12. Monte-Carlo studies & performances of the Full Likelihood method 213 rere the results with the pull vikelihood method re given for the vine n R dt smple on whih the method hs een optimizedD s preliminry step efore the unlinding of the whole vine n dtsetF he signi(ne mpD signi(ne distriution nd the thet 2 plot for the stndrd nlysis of the R dtset reported in 6.11 re relled on pigure 6.31F hese plots show no hint for vine signl exess t the permi rotspot positionF sn onsequeneD limits on the plux nd on the nnihiltion rossEsetion < σv > re derived for lrge mss sn etween IHH qe nd P e following the proedure disussed in the previous setion 6.12 ut this time using the yx events from the vine n R dtset in the pull vikelihood (tF rtiulr ttention is rought on the < σv > limit for the IQH qe vine tht is ompred to the reported vlue in the permiEve dtF he yx events tht enter into the pull vikelihood (t re tken from the R dtsetD in the 0.4 • FyFsF he orresponding energy distriution is shown on pigure 6.32F he totl por eh mss of the sn etween IHH qe nd P eD the pull vikelihood funtion is lulted nd the 95% gv limit on the reonstruted vine frtion η 95%CL is determinedF pigures 6.33 nd 6.34 show the IEdimensionl vikelihood pro(les for the oisson termD hp shpe term nd the omined pull vikelihood for eh mssF por given (tting energy window @VH qe Y I e or PHH qe Y Q eA the oisson term is stle with respet to the mss s it doesn9t depend on the signl nd kground hpsF yn the left olumn the yx event distriution from pigure 6.32 is represented with the vine signl hp t the region with H.E.S.S.II onsidered mssF he vlue of η 95%CL is presented in red in the right olumnF por some msses @IQHD PHHD RHHD SHH qeA the pull vikelihood funtion @the omintion of the oisson nd hpe termsA reonstruts slightly negtive vlues for η Y s the limit vlues should e b H the orresponding pull vikelihood funtions hve een shifted suh tht minim re set to HD resulting in orret limitsF prom η 95%CL the limits on the numer of reonstruted gmm eventsD the plux @in γ.m -2 .s -1 .sr -1 A nd < σv > @in cm 3 .s -1 A hve een omputed from equtions 6.4D 6.7 nd 6.10D respetivelyF hese re not ounting for systemti unertintiesF he vlues re summrized in le 6.15F he plux nd < σv > limits re lso presented on pigures 6.35 nd 6.36 respetivelyD with violet squre dt pointsD in omprison to the wg sensitivity limits disussed in 6.12.2 resled to PFVh of oservtion time @mgent solid lineAF he vine n R results show good omptiility with the wg studies down to IQH qe nd up to VHH qeF et IHH qe the )ux nd < σv > limits re worsened y ftor of 2.3 with respet to the wg preditions sine the eptne for gmms is poorly onstrined ner the energy thresholdD resulting in lrge sttistil or systemti unertinties in the reonstrution of the γEry eventsF yn the other side the R limits re not omptile with the wg results ove VHH qe Y this is explined y hnge in the spetrl index of the R dt event distriutions in yx nd ypp regions when looking t pigures 6.27 nd 6.32D more pronouned with the updted version of the rFiFFF softwre @vFQHAF he hosen kground hp prmetriztion @eqF6.2A ws restrited to single powerElw (t ove PHH qe resulting in n imperfet desription of the kground y the wg hp over VHH qeF he hnge in the spetrl index ould e relted to the ontriution from the di'use emission omponentD or to gmm reonstrution issues tht re not overed in this studyF he otined results with the vine n R dtset present very good omptiility with the wg simultions preditionsD when extrpolted to PFVh of oservtion timeF sn prtiulr the lowest limit vlues re rehed t IQH qe where X Φ 95%CL (130GeV ) = 9.95 × 10 -4 γ.m -2 .s -1 .sr -1

E line N 95%CL line Φ 95%CL < σv > 95%CL (T eV ) (×10 -4 γ.m -2 .s -1 .sr -1 ) (×10
E line η 95%CL N 95%CL line Φ 95%CL < σv > 95%CL < σv > 95%CL (T eV ) (%) (×10 -4 γ.m -2 .s -1 .sr -1 ) (×10
< σv > 95%CL (130GeV) = 1.64 × 10 -27 cm 3 .s -1 he < σv > limit orresponds to ∼ 1.3 times the vlue reported in the permiEve pulition from gF eniger ITP @1.27 × 10 -27 cm 3 .s -1 AD omptile with our wg limits extrpolted to PFVh of oservtion timeF he use of lrger dtset is primordil to hieve etter vlues more ompetitive with rFiFFFs nd permiEve pulitionsD following to the wg preditionsF his is foreseen with the forthoming unlinding of the vine n T nd U dtsets @∼IUh of oservtion timeAD with IIh of oservtion time usle down to IHH qeF sn this sitution it will e possile to exlude the IQH vine feture with t lest WS7 of on(dene levelD inluding systemti unertinties on the kground hpF region with H.E.S.S.II 6.14 Conclusions he nlysis of PFV hours of dt t the permi rotspot position (l = -1.5 • ; b = 0 • ) hs een performed with the pull vikelihood methodD using the omplete potentil of the seond phse of rFiFFF with SEtelesope tereo on(gurtionF he region of interestD the exlusion regionsD the energy rnge for the (t nd the proility density funtions hve een studied nd optimized with tht dt smple to ring the est sensitivities to hrk wtter vine signls in the qg regionF wonteEgrlo simultions were performed to derive lirted sensitivity limits on the plux nd on the nnihiltion rossEsetion of the expeted hw signlsD nd to study the ontriutions from vrious systemti e'ets suh s errors on the kground hp shpe nd on the di'use emission omponent in the qlti lneF hese wg simultions show n exellent potentil for line reonstrution ove IHH qe nd elow few eD onsidering t lest PH hours of oservtion time nd yielded limits on gmmEry plux nd < σv > whih e0iently (ll the gp etween rFiFFFs nd permiEve pulitionsF he nlysis of tht limited PFVh dtset shows no hint of n exess t IQH qe t 95% gv in the region of the permi hotspot nd the derived < σv > limits is of the order of 1.64 * 10 -27 cm 3 .s -1 t WS7 gvD slightly ove the nnihiltion rossEsetion reported in permiEve dt @1.27 * 10 -27 cm 3 .s -1 A tht ws omputed with QFU yers of dtF elso the otined results with the vine n R dtset show very good omptiility with the results with wg simultionsF es the performnes of the method strongly depend on the event sttistis it is neessry to nlyse muh lrger dtset to eome ompetitive with the former rFiFFF nd permiEve pulitionsF he unlinding of the vine n T nd U dtsets @∼ IUh of oservtion time with IIh usle t IQH qeA is primordil to hieve tht golF sn prtiulr the nlysis of the vine n U dtset will possily llow to exlude the IQH qe permi rotspot with t lest 95% of on(dene level inluding systemti unertinties on the kground hpF here is lso room for improvement with the present developments of the rFiFFF reonstrution softwre where the rFiFFF performnes with the (fth telesope re supposed to reh the expeted low energy threshold of SH qe in futureF hi0ulties relted to nlysis t low energies @espeilly t IQH qeA should dispper s the energy threshold of the experiment is deresingD the idel sitution eing to get the position of the IQH qe vine signl in the high energy @powerElwA prt of the kground event distriutionF he omintion of lrger run sttistis ner the permi rotspot position nd the softwre developments will ertinly led to b S sigm exlusion of the IQH qe permi vine rotspot nd will open window for new disoveriesF Conclusion he presene of the hrk wtter @hwA in the oservle niverse hs een lrgely demonstrted through its grvittionl in)uene on visile ojets t strophysil nd osmologil slesD nd nturlly enters s omponent into the ΛEghw modelF roweverD its nture remins unknownD despite the extensive e'orts rised y the interntionl sienti( ommunity in im to detet its nnihiltion or dey into w prtiles with strophysil oservtions or intertions with norml mtter in groundEsed detetorsD or its prodution in prtile elertors s the vrgF emong the list of possile prtile ndidtesD ekly snterting wssive rtiles @swsA re urrently one of the most populr hypotheses to nswer the question of the nture of the hrk wtterF ixoti gmmEry signtures produed from the selfEnnihiltions of the sws n e deteted t very high energies @riA with speEorne telesopes or with groundEsed γEry oservtories pointing t spei( regions of the sky suh s the qlti gentre @qgA regionD hwrf pheroidl qlxies @dphAD qlxy glusters or extrglti soures tht re inluded into the dense hw hlo struturesF sn this thesisD results on the indiret detetion of the hw with the groundEsed rFiFFF γEry oservtory hve een providedD serhing for exoti γEry spetrl signtures in the gittrius hwrf qlxy @grhA nd in the qlti gentre regionF he rFiFFF experimentD onsisting in n rry of S smging etmospheri gherenkov elesopes loted in xmii nd designed to reonstrut the diretion nd energy of the ri γErys entering nd interting with the tmosphereD hs een desriedF he priniple of the rFiFFF instrument lirtionD the reonstrution of the priE mry γEry events nd their disrimintion with the osmiEry kground hs een overed in ghpter 2F un qulity seletions hve een disussed in ghpter 3D whih re used to produe seletion of good qulity runs for o0il physis nlyses in rFiFFF sn this work the ParisRunQuality run seletion softwreD initilly setEup for rFiFFFsD hs reeived mjor upgrde nd now provides independent qulity seletions on the gS telesopeD s well s new onvenient fetures suh s defult run seletion pro(les tht depend on the telesope rry on(gurtionF his tsk hs een of high ommon interest nd the upgrded version of the softwre is now urrently used in rFiFFF he ommissioning of the iggest gherenkov telesope in the world @gSA in PHIP t the entre of the rry hs lowered the rFiFFF energy threshold down to ∼VH qe t the nlysis levelF he kground to hw signl essentilly onsists in di'use osmiEry hdronsD di'use γErys nd known strophysil emissions tht rise in the hw regions of interestF sn ghpter 4 the priniple of stndrd rFiFFF nlyses hve een presentedD tht mke use of the sutrtion from the numer of reonstruted events in the signl @yxA nd kground @yppA regions to extrt the exess γEry signl from soureF he method 224 Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II hs een pplied on two known strophysil soures tht re of interest for the further hw nlysesD with spetrl reonstrution of the exesses Y the extended glti soure ri tIURIEQHP @lose to the qgA nd the extrglti lirtion soure u PISSEQHR @the ypp dt were studied to e used s templte for kground modelling in the qg regionAF he results re omptile with previous pulitionsF hen this yxEypp proedure hs een pplied on the nery grh qlxyD looking for potentil hw ontinuous nnihiltion signlF e ∼Qσ exess hs een oserved t the nominl position of the dphD tht ould possily e ttriuted to the hw or to n old pulsrF rowever this low signi(ne does not yet rule out the hypothesis of sttistil )utution of the kgroundD nd onsequently limits hve een lulted on the nnihiltion rossEsetion of the hw prtilesD lthough not ompetitive with permiEve limits nd with expettions from xww modelsF he reEnlysis of the soure with more dt is expeted in future with potentil on(rmtion of the exess signlF he most importnt prt of the thesis is devoted to the serh for γEry line signlD reported in ghpters 5 nd 6F e new unEinned pull vikelihood method hs een developedD lirted @with wonteEgrlo simultionsA nd pplied to the qg region dt smples quired y rFiFFF in PHIRF he qg region hs een privileged trget during the (rst phse of rFiFFFD s it is expeted to e the entre of very high density hw hloF yn the other hnd the detetion of line signtures in γErys would e smoking gun for proving the existene of sws s they re esily distinguishle from the stndrd strophysil nd osmiEry kground spetrF he results of the work onsist in the estimtion of the hw lineEsignl frtion nd its position in the energy spetrum with the developed method pplied on wg nd rel dt smplesF sn (rst stepD the size of the nlysis region of interest hs een optimized with wg simultions pointing t the est (t position of the IQH qe γEry line exess reported in the permiEve dt in PHIPD o'set y -1.5 • longitude from the qgF his line feture is however urrently eing disproved y the permi gollortion nd rFiFFF is the only γEry experiment tht is le to provide rossEhek nlysisF eondlyD the use of ∼PHh of dedited PHIR oservtions with ll the S telesopes llowed to go down in energy to VH qe nd up to Q e in testing the potentil of the line signl extrtionF es dt smples re onernedD only smll frtion of the totl dtset hs een o0illy nlyzed until nowD orresponding to PFVh of livetimeF xo exess signl ws found with the stndrd yxEypp methodF vimits t WS7 gv hve een derived on the γEry )ux nd on the nnihiltion rossEsetion of the hw prtiles with respet to the hw prtile mssD using the pull vikelihood methodF he results for lrge mss sn IHH qe Y P e provided with wg simultions nd with the PFVh dtset hve shown very good potentil of the method for line signl detetion nd provide omplementry nd lso more ompetitive limits with respet to the older rFiFFFs nd permiEve pulitions in the IHH E QHH qe rngeF he nlysis of the full PHh dtset is foreseen in eptemer PHIS nd is expeted to rule out the IQH qe permi line feture with etter thn WS7 gvD nd to provide the most onstrining hw nnihiltion limits upEto dte on γEry line emission in the ri rngeF 6.14. Conclusions 225 hese results will improve in future with further developments in the rFiFFFss gmmEry reonstrution elow IHH qe nd with more dedited oservtionsF he nlysis t the qg position is foreseen with more thn IHHh of oservtion time lredy ville with rFiFFFssF sn more distnt futureD the rekEthrough in hw serhes will ome with the gherenkov elesope erry @geA projet tht is expeted to strt operting y the end of this dedeD nd would possily llow to solve the hw nture puzzleF Bibliographie I wq ertsenD esiD sser edouD w ekermnnD t edmsD te eguilrD w ehlersD h eltmnnD t eu'energD fiD et lF seue serh for drk mtter nnihiltion in nery glxies nd glxy lustersF Physical Review DD VV@IPA XIPPHHID PHIQF @gited on pge IUFA P wq ertsenD u erhmD w ekermnnD t edmsD te eguilrD w ehlersD w ehrensD h eltmnnD endersonD w erhingerD et lF erh for drk mtter nnihiltion in the glti enter with ieueEUWF arXiv preprint arXiv :1505.07259D PHISF @gited on pges IT nd IUFA Q eous e edoD w ekermnnD w ejelloD f etwoodD w exelssonD v fldiniD t flletD q frielliniD h fstieriD wiln fttelinoD et lF wesurement of the osmi ry eCC eE spetrum from PH gev to I tev with the fermi lrge re telesopeF Physical Review LettersD IHP@IVA XIVIIHID PHHWF @gited on pge ISFA R e ermowskiD p eeroD p ehroninD eq ekhperjninD q entonD flendernD e flzerD e frnkD vonne feheriniD t feker jusD et lF erh for photonE linelike signtures from drk mtter nnihiltions with hessF Physical review lettersD IIH@RA XHRIQHID PHIQF @gited on pges IQRD ISSD ISVD PHVD PHWD PIH nd PIPFA S e ermowskiD p eeroD p ehroninD eq ekhperjninD q entonD e frnkD frres he elmeidD e fzerEfhiD vonne feheriniD t fekerD et lF erh for drk mtter nnihiltion signl from the glti enter hlo with hessF Physical Review LettersD IHT@ITA XITIQHID PHIIF @gited on pge PQFA T e ermowskiD p ehroninD p eit fenkhliD eq ekhperjninD i engünerD q entonD flendernD e flzerD e frnkD feheriniD et lF ress oservtions of the r during its mrh PHIQ gev gmmEry )reF Astronomy & AstrophysicsD STP XvRD PHIRF @gited on pge IPQFA U ettil ermowskiD p eeroD p ehroninD eq ekhperjninD q entonD frres he elmeidD e fzerEfhiD vonne feheriniD f feherD fenowD et lF he γEry for the milliseond pulsr origin of the glti enter gev exessF arXiv preprint arXiv :1506.05104D PHISF @gited on pge PRFA QR q feriD w fellzziniD p prternliD q fttgliD erinD e ollimD e yosterlooD estD nd qlletiF he extended struture of the dwrf irregulr glxy sgittriusF

Astronomy & AstrophysicsD SUH XeUVD PHIRF @gited on pge IHUFA QS uq fegemnD er froeilsD nd r ndersF ixtended rottion urves of spirl glxies X hrk hloes nd modi(ed dynmisF Monthly Notices of the Royal Astronomical SocietyD PRW@QA XSPQ!SQUD IWWIF @gited on pges P nd QFA QT to h fekensteinF eltivisti grvittion theory for the modi(ed newtonin dynE mis prdigmF Physical Review DD UH@VA XHVQSHWD PHHRF @gited on pge IHFA QU q felngerD f humontD illwngerD tp qunionD nd urmlF qlol (t to higgs signl strengths nd ouplings nd implitions for extended higgs setorsF Physical Review DD VV@UA XHUSHHVD PHIQF @gited on pge IITFA PHHV@HIA XHRWD PHHVF @gited on pge PQFA SH wtthew fukley nd hn rooperF hrk mtter suhlos in the fermi (rst soure tlogF Physical Review DD VP@TA XHTQSHID PHIHF @gited on pge PSFA SI endres furkertF he struture of drk mtter hloes in dwrf glxiesF Galaxies in the Young UniverseD pges PPH!PPSD IWWSF @gited on pge IWFA SP q grlergD rug eeD v worrisD r vinD i illingsonD h ttonD w wikiD nd g hepherdF he ω M Eω Λ dependene of the pprent luster ωF The Astrophysical JournalD SIT@PA XSSPD IWWWF @gited on pge PFA SQ irdo gten nd iero llioF e novel determintion of the lol drk mtter densityF Journal of Cosmology and Astroparticle PhysicsD PHIH@HVA XHHRD PHIHF @gited on pge PHFA 232 Bibliographie SR w ghdwikD u vyonsD tv wgomD ut yrfordD tv ysorneD w ynerD i hwD ui urverD nd qt iezorekF ery high energy gmm rys from pks PISS!QHRF The Astrophysical JournalD SIQ@IA XITID IWWWF @gited on pge WUFA SS ghlmeEglvetD w de xuroisD tE vernetD et lF wuon e0ieny of the hess telesopeF arXiv preprint arXiv :1403.4550D PHIRF @gited on pge RSFA ST eli r ghmseddineD o ernowittD nd rn xthF volly supersymmetri grnd uni(tionF Physical Review LettersD RW@IRA XWUHD IWVPF @gited on pge WFA SU glifton nd eq vyneF righErdioEfrequeny survey for young nd milliseond pulE srsF NatureD QPH@THSUA XRQ!RSD IWVTF @gited on pges WI nd WPFA SV hougls gloweD wrus frdD enthony r qonzlezD wxim wrkevithD ott ndllD ghristine tonesD nd hennis ritskyF e diret empiril proof of the existene of drk mtterF The Astrophysical Journal LettersD TRV@PA XvIHWD PHHTF @gited on pge QFA SW permiEve gollortionF erhing for drk mtter nnihiltion from milky wy dwrf spheroidl glxies with six yers of fermiElt dtF arXiv preprint arXiv :1503.02641D

PHISF @gited on pges PRD IIS nd IITFA TH permiEve gollortionD w ekermnnD e elertD et lF erhing for drk mtter nnihiltion from milky wy dwrf spheroidl glxies with six yers of fermiElt dtF arXiv preprint arXiv :1503.02641D PHISF @gited on pges IU nd IHSFA TI ri gollortionD e ermowskiD p eeroD p ehroninD eq ekhperjninD q enE tonD flendernD e flzerD e frnkD feheriniD et lF erh for photon lineElike signtures from drk mtter nnihiltions with hessF arXiv preprint arXiv :1301.1173D

PHIQF @gited on pges xviii nd PQFA TP ri gollortionD e ermowskiD p eeroD p ehroninD eq ekhperjninD q enE tonD e frnkD frres de elmeidD e fzerEfhiD feheriniD et lF erh for drk mtter nnihiltion signl from the glti enter hlo with hessF arXiv preprint arXiv :1103.3266D PHIIF @gited on pge IQRFA TQ ri gollortionD e ermowskiD p ehroninD p eit fenkhliD eq ekhperjninD i engünerD w fkesD flendernD e flzerD e frnkD et lF erh for drk mtter nnihiltion signtures in hess oservtions of dwrf spheroidl glxiesF arXiv preprint arXiv :1410.2589D PHIRF @gited on pge IHVFA TR ri gollortion nd p ehroninF ery high energy gmm rys from the diretion of sgittrius BF arXiv preprint astro-ph/0408145D PHHRF @gited on pge RSFA TS ri gollortion nd p ehroninF roing the ti pek in the osmiEry eletron spetrum with hessF arXiv preprint arXiv :0905.0105D PHHWF @gited on pge ISFA TT lnk gollortion et lF lnk PHIS resultsF xiiiF osmologil prmetersF arXiv preprint arXiv :1502.01589D PHISF @gited on pges S nd TFA TU he ri gollortion nd p ehroninF ress oservtions of pks PISSEQHRF arXiv preprint astro-ph/0411582D PHHRF @gited on pge IPQFA TV he ri gollortion nd pe ehroninF hisovery of veryEhighEenergy gmmE rys from the glti entre ridgeF arXiv preprint astro-ph/0603021D PHHTF @gited on pges IRVD IUI nd IWWFA TW q h gost nd i ermndro'F eundnes nd kinemtis of the gloulr luster systems of the glxy nd of the sgittrius dwrfF The Astronomical JournalD IHW XPSQQD IWWSF @gited on pge IHUFA UH nsu hylnD hougls pinkeinerD hn rooperD im vindenD tephen ux ortilloD xihols v oddD nd ry ltyerF he hrteriztion of the gmmEry signl from the entrl milky wy X ompelling se for nnihilting drk mtterF arXiv preprint arXiv :1402.6703D PHIRF @gited on pges IT nd PRFA UI wthieu he xuroisF enlysis methods for tmospheri erenkov telesopesF arXiv preprint astro-ph/0607247D PHHTF @gited on pge SQFA UP wthieu he xuroisF Very High Energy astronomy from HESS to CTA. Opening of a new astronomical window on the non-thermal UniverseF hh thesisD niversité ierre et wrie gurieEris sD PHIPF @gited on pges RI nd RQFA UQ wthieu he xuroisF Very High Energy astronomy from HESS to CTA. Opening of a new astronomical window on the non-thermal UniverseF hh thesisD niversité ierre et wrie gurieEris sD PHIPF @gited on pge IWPFA UR wthieu he xurois nd voï ollndF e high performne likelihood reonstrution of γErys for imging tmospheri herenkov telesopesF Astroparticle PhysicsD QP@SA XPQI! PSPD PHHWF @gited on pges SPD SQ nd SRFA US t hiemndD w uuhlenD wduD w empD f wooreD h otterD nd t tdelF glumps nd strems in the lol drk mtter distriutionF NatureD RSR@UPHSA XUQS!UQVD PHHVF @gited on pge UFA UT ott hodelson nd vwrene w idrowF terile neutrinos s drk mtterF Physical Review LettersD UP@IA XIUD IWWRF @gited on pge IHFA UU p huoisD q vmnnD nd e tholkowskF e multivrite nlysis pproh for the imging tmospheri herenkov telesopes system hessF Astroparticle PhysicsD QP@PA XUQ! VVD PHHWF @gited on pge IIRFA UV tokim idsjoF espets of neutrino detetion of neutrlino drk mtterF arXiv preprint hep-ph/9704384D IWWUF @gited on pge IIFA UW t iinstoF yn the onstrution of omposite model for the glxy nd on the deE termintion of the system of glti prmetersF Trudy Astrozicheskogo Instituta Alma-AtaD S XVU!IHHD IWTSF @gited on pge IWFA VH tohn illisD uelleyD nd himitri xnopoulosF gonstrints from guge oupling uni(tion on the sle of supersymmetry rekingF Physics Letters BD PVU@IA XWS!IHHD IWWPF @gited on pge IHFA VI lrih illwnger nd gyril rugonieF xmhdey PFI X n updted progrm for sprtile mssesD higgs mssesD ouplings nd dey widths in the nmssmF Computer physics communicationsD IUS@RA XPWH!QHQD PHHTF @gited on pge IITFA VP ierre pyetF upersymmetry nd wekD eletromgneti nd strong intertionsF Physics Letters BD TR@PA XISW!ITPD IWUTF @gited on pge WFA VQ qry t peldmn nd oert h gousinsF ni(ed pproh to the lssil sttistil nlysis of smll signlsF Physical Review DD SU@UA XQVUQD IWWVF @gited on pge IIRFA VR wikulski erhive for pe elesopes @weAF qloulr luster messier SRD tken y the hule spe telesope @hstAF PHHTF @gited on pges IHU nd IHVFA VS x pornengoD v ieriD nd opelF xeutrlino nnihiltion into γ rys in the milky wy nd in externl glxiesF Physical Review DD UH@IHA XIHQSPWD PHHRF @gited on pge PIFA VT eter w prinhoyD teven wjewskiD irdo wuñozD hvid vwD iw v oksD illim i uunkelD ihrd t ttersonD nd uthryn tohnstonF e Pmss llEsky view of the sgittrius dwrf glxyF viiF kinemtis of the min ody of the sgittrius dsphF The Astrophysical JournalD UST@IA XURD PHIPF @gited on pge IHUFA VU tefn punkD qermn rermnnD tmes rintonD hvid fergeD uonrd fernlöhrD erner rofmnnD xymnD p oussenelD nd inentF he trigger system of the hess telesope rryF Astroparticle PhysicsD PP@QA XPVS!PWTD PHHRF @gited on pge QUFA VV w roller w enter g qivitto q udk f vernier hjnntiEeti e for the ri gollortion qjdusD w ghretienF ulstions from the vel pulsr down to PH gev with hFeFsFsFiiF Proceedings Of Science, ICRC 2015 The HagueD to e pulishedD PHISF @gited on pge SSFA VW elex qeringerEmethD wtthew q lkerD vvs w uoushippsD ergey i uopoE sovD sily felokurovD qriel orrelD nd x yn ivnsF ividene for gmmE ry emission from the newly disovered dwrf glxy retiulum PF arXiv preprint arXiv :1503.02320D PHISF @gited on pges PR nd IHRFA WH elex qeringerEmethD wtthew q lkerD vvs w uoushippsD ergey i uoposovD sily felokurovD qriel orrelD nd x yn ivnsF sndition of gmmEry emission from the newly disovered dwrf glxy retiulum iiF Physical Review LettersD Physics ReportsD PTU@SA XIWS!QUQD IWWTF @gited on pge WFA IHQ q unhD hv fertshD e pvleD gi pihtelD g rrtmnD rofstdterD if rughesD h runterD f rughlokD he uni'enD et lF he projet egret @energeti gmmEry experiment telesopeA on ns9s gmmEry oservtory groF Space Science ReviewsD RW@IEPA XTW!VRD IWVWF @gited on pge PUFA IHR e ushlinskyF eonstruting the spetrum of the preglti density (eld from stroE nomil dtF The Astrophysical JournalD RWP@IA XID IWWVF @gited on pge PFA IHS w uertzmn nd qr emroskiF gomputer simultion methods for investigting the detetion hrteristis of tev ir herenkov telesopesF Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated EquipmentD QRQ@PA XTPW!TRQD IWWRF @gited on pge RVFA IHT t uildeD etkinsD rw fdrnD q flylokD sr fondD w frduryD tr fukleyD he grterEvewisD y gelikD gu ghowD et lF he whipple oservtory IHm gmmEry telesopeD IWWU!PHHTF Astroparticle PhysicsD PV@PA XIVP!IWSD PHHUF @gited on pge RVFA IHU uzunori uohriD uunihito sokD utk pujitD nd yo mzkiF gn we explin msEHP ntiproton nd positron exesses simultneously y nery supernove without pulsrs nor drk mtter c arXiv preprint arXiv :1505.01236D PHISF @gited on pge ISFA IHV idwrd uol nd wihel tnley urnerF he erly universeF Front. Phys., Vol. 69,D ID IWWHF @gited on pge VFA IHW ergey i uoposovD sily felokurovD qriel orrelD nd x yn ivnsF fests of the southern wild X hisovery of nine ultr fint stellites in the viinity of the mgellni loudsF The Astrophysical JournalD VHS@PA XIQHD PHISF @gited on pges IHR nd IHTFA IIH ergey i uoposovD q qilmoreD wq lkerD felokurovD x yn ivnsD w pellhuerD qierenD h qeislerD v wonoD ti xorrisD et lF eurte stellr kinemtis t fint mgnitudes X pplition to the oötes i dwrf spheroidl glxyF The Astrophysical JournalD UQT@PA XIRTD PHIIF @gited on pge IHRFA III umil uowlskD veszek oszkowskiD nd inrio wri essoloF wo ultimte tests of onstrined supersymmetryF Journal of High Energy PhysicsD PHIQ@TA XI!QQD PHIQF @gited on pge IPFA IIP wrek uowlskiD hvid uinD qreg elderingD t egostinhoD e emdonD emE nullhD g fllndD u frryD q flnD t ghllisD et lF smproved osmologil onstrints from newD oldD nd omined supernov dt setsF The Astrophysical Jour-nalD TVT@PA XURWD PHHVF @gited on pges S nd TFA IIQ endrey urvtsovD yleg qnedinD nd entoly e ulypinF he tumultuous lives of gE lti dwrfs nd the missing stellites prolemF The Astrophysical JournalD THW@PA XRVPD PHHRF @gited on pge IHQFA IIR p uryzelD q wurinD v frunettiD tEw huoisD e pissonD v tournetD q vmnnD ve)ourD f vieunrdD s wonteiroD et lF smproved sensitivity of hessEii through the (fth telesope fous systemF arXiv preprint arXiv :1307.6461D PHIQF @gited on pges RU nd TWFA IIS q vmnnD g prnierD e tholkowskD w uie'erD nd g gollortionF gittrius dwrf spheroidl glxy oserved y hessF arXiv preprint arXiv :1307.4918D PHIQF @gited on pges ixD IHVD IIRD IIS nd IITFA Bibliographie 237 IIT endrew g vyden nd et rjediniF hotometry of the gloulr luster mSR nd the sgittrius dwrf glxy X he geEmetlliity reltionF The Astronomical JournalD IIW@RA XIUTHD PHHHF @gited on pge IHUFA IIU téphne ve foheD f hegrngeD w unhD e frruD fzerEfhiD r gotD vw ghounetD q heiisD t hezlyD e hjnntiEet%D et lF e new nlysis method for very high de(nition imging tmospheri herenkov telesopes s pplied to the ITT honld q orkD t edelmnD tohn i enderson trD ott p endersonD tmes ennisD xet e fhllD te fkkenD oert frkhouserD teven fstinD iileen fermnD et lF he slon digitl sky survey X ehnil summryF The Astronomical JournalD IPH@QA XISUWD PHHHF @gited on pge IHRFA ITU ggiD fonifioD w fellzziniD i g'uD p perrroD q wroniD v wonoD woE niD nd v ordoneF he sgittrius dwrf mssEtoElight rtioF Proceedings of the International Astronomical UnionD I@gIWVA XIHI!IHRD PHHSF @gited on pges IHU nd IHVFA ITV pritz wikyF hie rotvershieung von extrglktishen neelnF Helvetica Physica ActaD T XIIH!IPUD IWQQF @gited on pge PFA Résumé : v9nivers est dominé pr une omposnte invisile ppelée wtière xoire @wxAD de nture inonnue mis dont les e'ets grvittionnels sur l mtière visile sont lirement oservésF sl été proposé que l wx soit onstituée de prtiules mssives et intergissnt filement ve l mtièreD permettnt insi de onilier théorieD oservtions et simultionsF v9nnihiltion de es prtiules dns les régions où l wx est fortement onentrée pourrit produire des ryons γ de très hute énergie dont les signtures spetrles peuvent être déteE tées pr le réseu de télesopes rFiFFF n exès à ∼Qσ est oservé dns l diretion de l qlxie xine du gittireD ve l méthode stndrd d9nlyse yxEyppF lus de données sont néessires pour onlure qunt à son origineF v seonde prtie du trvil onerne l reherhe de ries spetrles en γ dns l région du gentre qltiqueF ne méthode de wxiE mum de risemlne gomplète été développéeD étlonnée et ppliquée à une frtion d9un ensemle de PHh de données prises en PHIRF euun exès de γ n9étnt oservéD des limites sur l setion e0e d9nnihiltion de l wx sont produites pour des msses de IHH qe à P eD l sensiilité de rFiFFF à sse énergie étnt otenue pr l9jout d9un S ème télesope depuis PHIPF ges limites omplètent e0ement les préédents résultts de permiEve et rFiFFF h9utre prt l9nlyse (nle devrit permettre d9exlure un potentiel signl à IQH qe oservé dns les données de permiEve en PHIP et e ve plus de WS7 gvD et de proE poser les limites les plus solides à e jour sur les modèles d9émission de ries spetrles en γ dns le domine d9énergie ouvert pr rFiFFF Mots-clés : Matière Noire, Astronomie gamma, H.E.S.S., Maximum de Vraisemblance, Centre Galactique, Galaxies Naines Sphéroïdes Abstract : he niverse is full of grvittionl evidene of dominnt invisile hrk wtE ter @hwA omponent t the qlti nd osmologil slesF elthough its nture is still one of the mjor puzzles of the PI st genturyD ekly snterting wssive rtiles @swsA re n exellent senrio for mthing theoretil preditions with oservtions nd simultionsF sn prtiulrD their selfEnnihiltions would give rise to hrteristi spetrl signtures in γErysD detetle t ery righ inergies @riA with the rFiFFF telesope rry in regions suh s the qlti gentre @qgA nd hwrf pheroidl qlxies @dphsAF he stndrd yxEypp nlysis method is pplied in the oservtion of the gittrius dph where ∼Qσ hotspot is oserved ove QHH qeD lthough more sttistis is required to onlude on its potentil hw originF he seond prt of the work is foused on the serh for monohromti γEry line signtures in the qg regionF e pull vikelihood method hs een developedD liE rted with wonteEgrlo simultions nd pplied to suEsmple of PHh dtset quired in PHIRF xo exess signl is foundD thus leding to limits on the hw nnihiltion rossEsetion down to IHH qe mss rngeD the sensitivity t the lowest energies eing hieved y the S th rFiFFF telesope dded in PHIPF hese limits e0iently (ll the gp in mss etween results from permiEve nd the (rst phse of rFiFFF yn the other side the nlysis of the omplete dtset is expeted to exlude the IQH qe lineElike feture reently reported in the permiEve dtD with more thn WS7 gvD nd to provide the most onstrining hw limits so fr on γEry line emission in the ri rngeF Keywords : Dark Matter, Gamma-ray astronomy, H.E.S.S., Full Likelihood method, Galactic Centre, Dwarf Spheroidal Galaxies

Figure

  Figure Q ! ve réseu de télesopes rFiFFFD situé en xmiie

Figure S ! v

  Figure S ! v méthode stndrd d9nlyse yxEypp dns rFiFFF ves positions I à R

  PHP TFIP wonteEgrlo studies 8 performnes of the pull vikelihood method F F F F F F PHT TFIPFI wg simultion onditions F F F F F F F F F F F F F F F F F F F F F F F F F PHT TFIPFP hw sensitivity limits for the mss sn X IHH qe → P e F F F F F F PHU TFIQ enlysis of the vine sn R dt smple F F F F F F F F F F F F F F F F F F F F PIR TFIQFI wss sn etween IHH qe nd P e F F F F F F F F F F F F F F F F F PIR TFIQFP hisussion of the IQH qe rotspot results F

1. 1 .

 1 Figure IFI ! ottionl urve for the qlxy xqg TSHQ @QSD IWWIAF he irulr veloity eomes onstnt t lrge distnes from the entre of the qlxyD inomptile with prediE tions from xewtonin mehnis nd with the ssumption tht ll the mss is loted within the luminous omponent

Figure

  Figure IFS ! ivolution of the omoving numer density a(t) 3 .n DM of the hw prtiles following to the expnsion of the niverse @iFeF inresing timeAD showing the freezeEout in the hw density nd the relted therml reli density tht depend on the veloityEweighted nnihiltion rossEsetion of the hw prtilesF pigure dpted from uol nd urner IHV

Figure

  Figure IFII ! rinipl hw hlo pro(les onsidered in the litertureD here orresponding to the wilky y hloF he pro(les re normlized ording to the lol hw density t the un X ρ (r 0 = 8.5kp) = 0.39 GeV.cm -3

Figure

  Figure IFIP ! rinipl γEry emission proesses from sw nnihiltionD nd their resE

Figure

  Figure PFI ! smging eir gherenkov elesopes urrently in opertion

Figure

  Figure PFQ ! ypil gherenkov light signtures in the rFiFFF mers for @A γEryD @A osmiEry hdron nd @A muon

  Figure PFS ! ixmple of longitudinl nd lterl pro(les for ir showers seen y segsF @veftA iletromgneti shower initite y γEry t QHH qeF @ightA rdroni shower initited y osmiEry proton of I eF he (gure is tken from ehronin et lF @PHHVA IV

Figure

  Figure PFII ! smpt of the xf level on the high gin pedestl P HG D in the rFiFFFs mersF et ∼ IHH wrz @verge xf level in rFiFFF oservtionsA the pedestl distriution is similr to the photoEeletron spetrumF pigure tken from UP

Figure

  Figure PFIS ! ixmple of simulted shower imge in the gS merD orresponding to zenith oservtions of PHH qe γEry t di'erent fous distnes for the merF pigure tken from IIR

Figure

  Figure PFIU ! @A he(nition of the rills prmetersD illustrted here for the stereosopi reE onstrution of γEry event with P telesopesF he importnt prmeters re the length nd width of the ellipses nd the distne etween the ryentre of the imges nd the mer entreF he shower imges re shown in ommon referentilD suh tht the reonstruted diE retion of the primry γEry orresponds to the intersetion of the mjor xes of the di'erent ellipsesF Θ is the ngle etween the reonstruted nd the expeted position of the soureF @A histriution of the men sled width prmeter from wg γEry nd proton simultionsD nd tul kground dt in rFiFFF he pplied uts re shown y the vertil linesF he (gures re tken from PH Reconstruction of the energy he energy of the primry prtile is the weighted verge of the reonstruted energies in eh of the individul telesopes X E reco = 1 N tel ×

Figure

  Figure PFIV ! gomprison of the energy resolutionD the energy is nd the ngulr resolution

Figure

  Figure QFI ! he min qs window of the risunulity softwreF st n e suEdivided into R regionsF veft pnel X ontrol pnel with tion uttons for lodingG(lteringGsving the runs from the dtseF op pnel X disply of the generl informtion on the seleted runsF widdle pnnel X ontrol plots showing the distriution of the qulity vriles for the seleted runsF fottom pnel X min pnel for (ltering the run dtseD presented in suEmodules for eh lss of seletion riteri

3. 4 .

 4 Figure QFP ! he generl struture of risunulity

  Figure QFR ! he trigger seletion pnel with relted ontrol plots for gSF hefult uts re shown in red he defult trigger uts tht re pplied in rFiFFFs seletions re relted to the enE trlGsystem rteD not to the individul gIER telesopesF por rFiFFFss nlyses it hs een deided to detivte the entrl trigger uts nd to rther rely on individul telesope trigger utsD for gIER nd gSD independentlyF his hoie is motivted y the di0ulty to set (xed entrl trigger uts when produing omined rFiFFFsGrFiFFFss run listD or omined rFiFFFss wonoGtereo run listF sn prtiulr the trigger rte of gS is out one order of mgnitude higher thn for gIER resulting in vrious entrl trigger rte vlues depending on the telesope on(gurtionD with two min popultions s shown in pigure 3.5F

Figure

  Figure QFU ! he gS utofous seletion pnel with relted ontrol plotsF he defult uts re shown in red he utofous @epA system of the gS telesope hs een presented in 2.2.4D nd llows imE proving the osmiEry rejetion pilities nd the ury of the reonstruted diretion

Figure

  Figure QFIH ! histriution of the g vlues over the runsF @A uns tken with the R telesopes of rFiFFFsF @A uns tken with ll the S telesopes sn risunulity it is now possile to ut on < T C > nd lso on the w of the g distriution in eh runF eout TS7 of the runs disply < T C > vlues etween HFW nd IFID hrteristi of n idel tmosphere nd reommended s stndrd uts in risunulityD lthough g uts re not set in defult seletionsF sn prtiulr the γEry )ux normliztion of soure is orrelted with the gD nd then utting on the g llows reduing systemti errors in the spetrl reonstrution of γEry souresF pinlly pigure 3.11 shows the timeEevolution of the g from the ommissioning of rFiFFFs lte PHHQ up to the end of PHIRD showing tht the vlues re stle from one yer to nother nd re well lirted to I for n idel tmosphereF elso the degrde in g vlues etween eugust nd ytoer is lerly oservedD nd is ttriuted to lnd (res tht re very ommon in the xorth of the rFiFFF site during this period of the yerF

Figure

  Figure QFIS ! gomprison of the telesope ded time nd roken pixel frtions on the gIER telesopesD for runs tken in the (rst phse of rFiFFF nd in the seond phse of rFiFFF @with gSA etween HIGPHIR nd HTGPHISF hese distriutions hve een shifted y out CS7 fter the ommissioning of gSF he defult uts in risunulity re shown in red

1 . 3 4. 1 . 2

 1312 Figure RFI ! wo di'erent wys to de(ne ypp kground regions in the py from wole oservtions

Figure

  Figure RFP ! yxEypp wole nlysis with exlusion regionsAngular direction of the wobble oset he lst importnt onsidertion in wole oservtion mode is the ngulr diretion of the o'set for given runF por wole o'set introdued in given ngulr diretion in the pyD the yx nd ypp regions re symmetril with respet to the pointing position @to get sme oservtion onditionsA ut re not symmetril with respet to the yx region 3 ine the sptil distriution of the kground events is vrying ross the skyD the kground nnot e perfetly homogeneous in ll diretions round the studied soureF por tking kground inhomogeneities round the soure into ountD the solution is to set di'erent ngulr direE tions for the wole o'set from one run to nother in the dt tkingF his on(gurtion is shown on pigure 4.3F ih individul run hs its own wole o'set diretion in eGhe or in glti oordintes nd its own ypp regionsD ut they ll hve ommon yx region for the yxEypp sutrE tionF e run list lso generlly mixes di'erent wole o'set vlues from one run to notherD typil vlues for rFiFFF lie etween HFS • nd IFS • F pigure 4.4 shows n exmple of yx nd ypp event mp for the nlysis of lirtion soure u PISSEQHR in tereo telesope on(gurtionD using run list of PH runs tht psses stndrd risrunqulity seletion uts nd onsidering 0.1 • irulr yx region entred on the pointElike soureF he ingfkE ground on(gurtion hve een used in the de(nition of the ypp regionsD mixing di'erent o'set vlues nd ngulr diretionsF sn this exmple the distriution of the wole o'sets is not ompletely homogeneous over the PH runsD whih explins the symmetry in the event mp long the e xisF et the (nl point of the yxEypp proedureD the numers of ypp events in eh run re summed together nd then sutrted from the sum of the yx events using the vlue of α for eh individul runD s n extension of eqution 4.1 X N excess =

Figure

  Figure RFS ! yxEypp nlysis with yxGypp pirs from di'erent dt smples

4. 2 . 2

 22 Figure RFT ! he very high energy gmmEry sky in the qlti gentre region over RHH qe with rFiFFFsD using the qermn rFiFFF softwre @reA with hrd nlysis utsF he position of ri tIURIEQHP is represented t the entreD with lso the lotion of the qlti gentre nd of the nery strophysil soure ri tIURSEQHQF he position of the pulsr fIUQUEQH @tht ould e responsile for the very high energy emission seen t the position of ri IURIEQHPA is lso shownF

Figure

  Figure RFW ! ixess mpD igni(ne mp nd signi(ne distriution in the py for the nlysis of ri tIURIEQHP with wodelCC pint uts @risnlysisA

Figure

  Figure RFIH ! rFiFFF exlusion regions in the qlti gentre regionD de(ned round referened γEry strophysil soures

Figure

  Figure RFIQ ! ixess mpD igni(ne mp nd signi(ne distriution in the py for the nlysis of uPISSEQHR with rFiFFFss wono nd tereo telesope on(gurtionsF he signi(ne distriutions for the estimted kground @the red insA re well (tted y qussin funtion entred t zero nd of width lose to I for oth reonstrutionsD s expeted from sttistil )ututions of the kground

Figure

  Figure RFIS ! petrl nlysis of u PISSEQHR with risnlysisEwodelCC in rFiFFFss wono telesope on(gurtionD using powerElw model

104

  Figure RFIT ! higrm showing the losest 4lssil4 hwrf qlxies oriting the wilky y @soure X IQVD PHHTA

Figure

  Figure RFIU ! histriution of the mssEtoElight rtio @in solr unitsD lulted within the hlfElight rdiusA of ll hwrf qlxies for whih the dt exist @`PHIIAD s funtion of their solute visul mgnitudeF his plot inlude ll types of hwrf qlxies deteted in the vol qroup @eFgF lso elliptil nd irregulrAF @soure X IPRD PHIPA

Figure

  Figure RFPH ! veft X the gloulr luster wessier SRD supposed to e t the entre of grh @photogrphed y the rule pe elesope VRAF ight X lotion of grh in equtoril oordintesD the pprent position of the dph eing loted ner the qlti gentre region

Figure

  Figure RFPI ! ixess mpD igni(ne mp nd signi(ne distriution in the py for the nlysis of grh with rFiFFFsD nd using di'erent uts on the reonstruted energy of the events

  Figure RFPR ! igni(ne mpD signi(ne distriution nd ngulr distriution of the events in the pyD reonstruted in qF vmnn et lF IIS with the X ef f method

5. 1 .

 1 Maximum Likelihood formalism 121 5.1.3 Modied Poisson Maximum Likelihood with ON and OFF regions (Rolke)

Figure

  Figure SFP ! hetermintion of the mesured hp relted to spei( gmmEry ontriuE

Figure

  Figure SFQ ! ixmple of wg roility hensity puntions s funtion of the mesured energyF he se of owerEvw strophysil signlD owerEvw hdroni kgroundD gontinuous hw nnihiltion signl nd hw nnihiltion vine re representedF ell hps re onvoluted with rFiFFFss sps for gmms in tereo telesope on(gurtion nd normlized to I on the energy rnge VHqe Y Qe

Figure

  Figure SFR ! qenerl struture of the pull vikelihood methodD showing the intertion etE ween the di'erent inputs nd the steps of the (tting proess of the model prmeters (η, m χ )F

Figure

  Figure SFS ! gomintion of the vikelihood pro(les for the oisson nd hpe terms in the reonstrution of η t given mss of the Ph (tting proessF his results in nrrower vikelihood in η nd then more urte reonstrution of tht model prmeterF sn this exmple 5% hw vine signl with mss m χ = 700GeV is reonstruted in tereo telesope on(gurtionD with Ih pro(les extrted t (xed m χ = 700GeV F he vertil oordintes re ssoited with the pull vikelihood pro(le onlyD the oisson nd hpe pro(les eing resled for presenttion purposesF

Figure

  Figure SFV ! riniple of the Ph on(dene region lultion t (1 -α)% gv for the reonstrution of the two model prmeters (η, m χ )

Figure

  Figure SFW ! gomputtion of the numer of reonstruted γEry signl events t 95% gv under the no signl hypothesisF he singleEsided gs t 95% gv on the reonstruted signl frtion η is shownF e simple lultion gives the ssoited numer of gmms N 95%CLγ

Figure

  Figure SFII ! ixmple of est ttistis distriution over SHH wg experimentsD here for the reonstrution of QHH qe vine signl with frtion η = 5% in rFiFFFss tereo telesope on(gurtionF he lirted signl signi(ne is derived from the medin vlue of the distriution

Figure

  Figure SFIQ ! histriution of the wg dt events for one experimentD in tereo telesope on(gurtionF he kground hp sled to the dt distriution is shown with lk solid line on the (tting energy window [200GeV ; 3T eV ]F e vine signl exess t QHH qe nd frtion S7 is represented in redF

Figure

  Figure SFIR ! esults X performnes of the pull vikelihood method for the reonstrution of vine signl (η, m χ ) using wg dtD for oth rFiFFFss wono nd tereo telesope on(gurtionsF ih dt point represents lirted vlue on SHH experimentsD with error rsGontours orresponding to WS7 ontinment frtionF

Figure

  Figure TFP ! ht events ounts in the VH qe to PHH qe energy rnge from gF eniger pperF Upper sub-panel : the mesured events with sttistil errors re plotted in lkF he horizontl rs show the estE(t models with @redA nd without hw @greenAD the lue dotted line indites the orresponding line )ux omponent loneF he lower sub-panel show residuls fter sutrting the model with vine ontriution

Figure

  Figure TFR ! rFiFFFs mp of the qg region in glti oordintesF he permi rotspot position (l = -1.5 • ; b = 0 • ) is represented y yellow rossD while nery strophysil soures re pointed y white irles nd rrowsF he extension of the hrk wtter hlo entred t the permi rotspot is represented y yellow re for visul representtion purposes only Y it is not representtive of the rel hw hlo ngulr extension whih depends on the onsidered hlo model oure nme l( • ) b(• ) rdius ( • ) gr eB H H HFPS qHFWCHFI HFVU HFHR HFPS qHFQCHFH HFQV H HFPS ri tIURSEQHQ EIFPUS EHFTS HFQS

1 .

 1 Figure TFV ! fkground mps of single run with pointing position t the qgD showing the evolution of the numer of ypp regions for n inresing FyFsF ngulr extensionF ixlusion regions re represented y red irles on the upperEleft plot

Figure

  Figure TFIH ! ht qulity for the vine n R dt smpleF he histogrms re extrted from the risrunqulity softwre nd disply the glol run nd telesope informtion for the most relevnt qulity seletion riteriF ed res or irles show the rejeted runs

Figure

  Figure TFIR ! ixess mpsD igni(ne mpsD θ 2 distriutionsD eeptne mps nd inergy distriutions from the nlysis of the vine n R dt for oth rFiFFFss wono nd tereo telesope on(gurtions

Figure

  Figure TFIS ! yxEypp energy distriutions using vine n R dt nd sptil sideEnds in the region round the permi rotspotF en exess is systemtilly oserved elow PHH qe t ll those pointing positions

Figure

  Figure TFIU ! tudy of the is on the reonstruted vine energy for simulted vines etween IHH qe nd PSH qeF por eh dt point the verge is on SHH simultions hs een tken t tht given vine energyF eonstrution is performed with the pull vikelihood method onsidering the wono telesope on(gurtion nd n energy rnge of IHH qe Y I eF en edge e'et is oserved t the lowEend of the rnge

  Figure TFIV ! vine signl hps for the pull vikelihood method X exmples t IQHD QHHD SHH nd VHH qeF essoited histogrms re lso represented

1 .

 1 Figure TFIW ! fkground FhFpFs in tereo on(gurtion for the pull vikelihood method derived from Q di'erent ontrol smples X wg simultionsD u PISSEQHR ypp wole dt nd vine n R ypp wole dtF he FhFpFs re normlized to I on the energy rnge VH qe Y I e

Figure

  Figure TFPP ! i'et of the zimuth ngle on the energy thresholdF he eptnes re omputed from pull wg simultions with zimuth ngles of 0 • nd 180 • in wono nd tereo telesope on(gurtions

  Figure TFPS ! histriution of the yx events in the vine n R dtset with the new softwre relese @vFQHAD for the tndrdD voose nd pint γEry seletion utsF he FyFsF stys (xed to θ ROI = 0.4 •

6. 12 .

 12 Monte-Carlo studies & performances of the Full Likelihood method 207 wg simultion onditions gentre of the FyFsF nd of the hw hlo @l = -1.5 • ; b = 0 • A FyFsF size θ ROI = 0.4 • estrophysil ftor @iinstoA Φ astro = 2.46 * 10 21 GeV 2 .cm -5 yservtion time T OBS = 20h xumer of vine signl events in the FyFsF N signal = 0 xumer of kground events in the FyFsF N background = N ON = 24280 xormliztion ftor etween yx nd ypp regions α = 4.65 xumer of simultions for eh mss N simu = 500

Figure

  Figure TFQI ! igni(ne mpD signi(ne distriution in the py nd thet 2 plot for the vine n R dtsetF he ys is represented with white irle entred on the permi hotspot (-1.5 • ; 0 • )

Figure

  Figure TFQP ! inergy distriution of the yx events @FyFsFA for the vine n R dtset

Figure 220 Chapitre 6 .

 2206 Figure TFQQ ! pull vikelihood (t of η performed on the vine n R dt smple @PFVhA in tereo telesope on(gurtion for msses etween IHH qe nd SHH qeF he energy distriution of the yx events nd the vine signl hp shpe is shown in the left olumn for eh step in m χ F he orresponding energy rnge for the (t is VH qe Y I eF he seondD thirdD nd lst olumn show the IEdimensionl vikelihood pro(les in η for the oisson termD shpe termD nd the omintion of oth @pull vikelihoodA respetivelyF he pull vikelihood limit on η t 95% gv is mentioned in red

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@gited on pges xviiiD ISVD ITHD PIHD PII nd PIPFA II edriánEwrtínezD e elertD w endréD q entonD w erdidD tEt euertD f fretD t frriosEwrtíD fsD fertinD et lF erh of drk mtter nnihiltion in the glti entre using the ntres neutrino telesopeF arXiv preprint arXiv :1505.04866DPHISF @gited on pges IT nd IUFA IP ysr edriniD qg frrinoD qe fzilevskyD fellottiD wirko foezioD ie fogoE molovD v fonehiD w fongiD lter fonviiniD fottiD et lF en nomlous positron undne in osmi rys with energies IFS!IHH gevF NatureD RSV@UPQVA XTHU!THWD PHHWF @gited on pge ISFA IQ p ehroninD eq ekhperjninD uEw eyeD e fzerEfhiD w feilikeD fenowD h fergeD ferghusD u fernlöhrD y folzD et lF glirtion of mers of the hess detetorF Astroparticle PhysicsD PP@PA XIHW!IPSD PHHRF @gited on pge QWFA IR p ehroninD eq ekhperjninD e fzerEfhiD w feilikeD fenowD h fergeD u fernlöhrD g foissonD y folzD forrelD et lF wultiEwvelength oservtions of pks PISSEQHR with hessF Astronomy & AstrophysicsD RRP@QA XVWS!WHUD PHHSF @gited on pges WU nd 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HTPHHI @PHIPAF Physical Review DD WI@IPA XIPWWHQD PHISF @gited on pges PR nd IHSFA PU hinihiro endo nd iiihiro uomtsuF gonstrints on the nnihiltion ross setion of drk mtter prtiles from nisotropies in the di'use gmmEry kground mesured with fermiEltF Physical Review DD VU@IPA XIPQSQWD PHIQF @gited on pge PSFA PV qrry engusD entonldo hiferioD fenoit pmeyD nd uurt t vn der reydenF gosmologil simultions in mond X the luster sle hlo mss funtion with light sterile neutrinosF Monthly Notices of the Royal Astronomical SocietyD RQT@IA XPHP!PIID PHIQF @gited on pge IHFA PW i eprileD w elfonsiD u eriskD p erneodoD g flnD v fudisD f fuermeisterD e fehE rensD feltrmeD u fokelohD et lF hrk mtter results from PPS live dys of xenonIHH dtF Physical review lettersD IHW@IVA XIVIQHID PHIPF @gited on pge IRFA QH rowrd ferD ernon frgerD endre vessD nd erxes tF usy disovery potentil of lhIR with HFQEQ£ ¢{EI} X e snowmss whitepperF arXiv preprint arXiv :1306.5343D PHIQF @gited on pge IQFA QI xet e fhll nd iohui pnF he most mssive distnt lusters X hetermining ω nd σVF The Astrophysical JournalD SHR@IA XID IWWVF @gited on pge PFA QP g fixersD h fstieriD g figongiriD y flnhD q flnhotD fokD fretzD e ghiE lingrinD te gorsD i golomoD et lF gommissioning nd (rst tests of the mgi telesopeF Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated EquipmentD SIV@IA XIVV!IWPD PHHRF @gited on pge PUFA QQ ihrd frtelsD urj urishnmurthyD nd ghristoph enigerF trong support

  QV vrs fergström nd iero llioF pull oneEloop lultion of neutrlino nnihiltion into two photonsF Nuclear Physics BD SHR@IA XPU!RRD IWWUF @gited on pge PQFA QW vrs fergströmD iero llioD nd tmes r fukleyF yservility of γ rys from drk mtter neutrlino nnihiltions in the milky wy hloF Astroparticle PhysicsD W@PA XIQU! ITPD IWWVF @gited on pge PIFA RH tuerg feringer et lF rtile dt groupF Phys. Rev. DD VT@HIHHHIAD PHIPF @gited on pge IPQFA RI u fernlöhrF qeomgneti e'ets on showers relevnt for the hess experimentF HESS internal noteD SQ XSVD PHHSF @gited on pge IWPFA RP qinfrno fertoneD ilfried fuhmüllerD vur goviD nd elejndro srrF qmmE rys from deying drk mtterF Journal of Cosmology and Astroparticle PhysicsD PHHU@IIA XHHQD PHHUF @gited on pge IVFA RQ qinfrno fertoneD hn rooperD nd toseph ilkF rtile drk mtter X ivideneD ndidtes nd onstrintsF Physics ReportsD RHS@SA XPUW!QWHD PHHSF @gited on pges IH nd ISFA RR qinfrno fertone nd hvid werrittF hrk mtter dynmis nd indiret detetionF Modern Physics Letters AD PH@IRA XIHPI!IHQTD PHHSF @gited on pge WFA RS hilip fettD inent ikeD grlos prenkD edrin tenkinsD tohn rellyD nd tulio xE vrroF he spin nd shpe of drk mtter hloes in the millennium simultion of λ old drk mtter universeF Monthly Notices of the Royal Astronomical SocietyD QUT@IA XPIS!PQPD PHHUF @gited on pge UFA RT yliver folzF Absolute Energiekalibration der abbildenden Cherenkov-Teleskope des HESS Experiments und Ergebnisse erster Beobachtungen des Supernova-Überrests RX J1713. 7-3946F hh thesisD hisserttionD uprehtEurlsEniversität reidelergD PHHRF @gited on pge TPFA RU ennmri forriello nd olo luiF he drk mtter distriution in dis glxiesF Monthly Notices of the Royal Astronomical SocietyD QPQ@PA XPVS!PWPD PHHIF @gited on pge PFA RV wrus frdD hougls gloweD enthony r qonzlezD hil wrshllD illim pormnD ghristine tonesD wxim wrkevithD ott ndllD im hrkD nd hennis E ritskyF trong nd wek lensing unitedF iiiF mesuring the mss distriution of the merging glxy luster Ies HTSU!SSVF The Astrophysical JournalD TSP@PA XWQUD PHHTF @gited on pge QFA RW orsten fringmnnD vrs fergströmD nd tokim idsjöF xew gmmEry ontriuE tions to supersymmetri drk mtter nnihiltionF Journal of High Energy PhysicsD

  IIS@VA XHVIIHID PHISF @gited on pge ITFA WI ferrie qieelsF Contribution á la reconversion d'une centrale solaire en un vaste détecteur pour l'astronomie gammaF hh thesisD IWWVF @gited on pge PVFA Bibliographie 235 WP qerrd qilmoreD wrk s ilkinsonD osemry pq yseD tn uleynD endres uohD x yn ivnsD nd iv u qreelF he oserved properties of drk mtter on smll sptil slesF The Astrophysical JournalD TTQ@PA XWRVD PHHUF @gited on pge IHQFA WQ tulien quyF Premiers résultats de l'expérience HESS et étude du potentiel de détection de matière noire supersymétriqueF hh thesisD niversité ierre et wrie gurieEris sD PHHQF @gited on pges RV nd SHFA WR uoihi rmguhiD keo woroiD nd uzunori xkymF emsEHP ntiprotons from nnihilting or deying drk mtterF arXiv preprint arXiv :1504.05937D PHISF @gited on pges IS nd ITFA WS h rnnD h fhtthryD vw fooneD wg ghntellD gonnerD gi govultD w hrgoE vnD portinD h qregorihD te rintonD et lF he steeEQP ground sed gmmEry detetorF Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated EquipmentD RWI@IA XIPT!ISID PHHPF @gited on pge PVFA WT endi rektorD wrtti idlD nd ilmo empelF ividene for indiret detetion of drk mtter from glxy lusters in fermi γEry dtF The Astrophysical Journal LettersD UTP@PA XvPPD PHIQF @gited on pge PRFA WU e wihel rillsF gerenkov light imges of es produed y primry gmmF sn International Cosmic Ray ConferenceD volume QD pges RRS!RRVD IWVSF @gited on pge SHFA WV erner rofmnnD ri gollortionD et lF ttus of the hess projetF sn International Cosmic Ray ConferenceD volume UD pge PUVSD PHHIF @gited on pge PUFA WW e stD q qilmoreD nd wt srwinF e dwrf stellite glxy in sgittriusF IWWRF @gited on pge IHUFA IHH odrigo stD osemry yseD qerrd qilmoreD wihel srwinD nd xihols untze'F he kinemtisD oritD nd survivl of the sgittrius dwrf spheroidl glxyF arXiv preprint astro-ph/9612025D IWWTF @gited on pge IHVFA IHI wt srwinD n funlrkD w fridgelndD nd q wwhonF e new stellite glxy of the milky wy in the onstelltion of sextnsF Monthly Notices of the Royal Astronomical SocietyD PRR XIT!IWD IWWHF @gited on pge IHQFA IHP qerrd tungmnD wr umionkowskiD nd uim qriestF upersymmetri drk mtterF

t

  telesopeF Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated EquipmentD RIT@PA XRPS!RQUD IWWVF @gited on pge SPFA IIV i for the ri gollortion vefrnD woulinF hrk mtter serh in the inner glti hlo with hFeFsFsF i nd hFeFsFsF iiF Proceedings Of Science, ICRC 2015 The HagueD to e pulishedD PHISF @gited on pges IU nd PQFA IIW E vi nd E wF enlysis methods for results in gmmEry stronomyF The Astrophysical JournalD PUP XQIU!QPRD IWVQF @gited on pges VVD IIU nd IRPFA IPH teven wjewskiD wp krutskieD wrtin h einergD nd tmes g ystheimerF e two miron ll sky survey view of the sgittrius dwrf glxyF iF morphology of the sgittrius ore nd tidl rmsF The Astrophysical JournalD SWW@PA XIHVPD PHHQF @gited on pge IHUFA IPI eter wrleuD ulo efonsoD wxwell ghertokD tun vizrzoD ho wruymD tohn tilleyD nd wni ripthiF sntermedite energy oservtions with tusF Proceedings of CHERENKOV05, Paris, April 2005D PHHSF @gited on pge PVFA IPP ihrd wsseyD homs uithingD nd tohn ihrdF he drk mtter of grvittioE nl lensingF Reports on Progress in PhysicsD UQ@VA XHVTWHID PHIHF @gited on pge RFA IPQ wrio wteoD idwrd ylszewskiD nd rether v worrisonF ring the outer struE ture of the sgittrius dwrf glxy X hetetions t ngulr distnes etween IH nd QRF The Astrophysical Journal LettersD SHV@IA XvSSD IWWVF @gited on pge IHQFA IPR eln wgonnhieF he oserved properties of dwrf glxies in nd round the lol groupF The Astronomical JournalD IRR@IA XRD PHIPF @gited on pge IHSFA IPS toseph wgulloughF ttus of the milgro gmm ry oservtoryF sn International Cosmic Ray ConferenceD volume PD pge QTWD IWWWF @gited on pge PVFA IPT trik wedeD wihele puiD elessndro trumiD nd omer olnskyF hrk mtE ter interprettions of the e±exesses fter fermiF Nuclear Physics BD VQI@IA XIUV!PHQD PHIHF @gited on pge IUFA IPU hvid werrittD elister qrhmD fen wooreD türg hiemndD nd fl² erzi¢F imE piril models for drk mtter hlosF iF nonprmetri onstrution of density pro(les nd omprison with prmetri modelsF The Astronomical JournalD IQP@TA XPTVSD PHHTF @gited on pge IWFA 238 Bibliographie IPV wordehi wilgromF e modi(tion of the newtonin dynmis s possile lterntive to the hidden mss hypothesisF The Astrophysical JournalD PUH XQTS!QUHD IWVQF @gited on pge IHFA IPW v wonoD w fellzziniD p perrroD nd i ninoF he entrl density usp of the sgittrius dwrf spheroidl glxyF Monthly Notices of the Royal Astronomical SocietyD QST@RA XIQWT!IRHPD PHHSF @gited on pges IHU nd IHWFA IQH fen wooreD pio qoverntoD om uinnD tohim tdelD nd qeorge vkeF esolving the struture of old drk mtter hlosF The Astrophysical Journal LettersD RWW@IA XvSD IWWVF @gited on pge IWFA IQI w wühlleitnerD e hjoudiD nd wmriniF dey X e fortrn ode for the deE ys of the supersymmetri prtiles in the mssmF Computer physics communicationsD ITV@IA XRT!UHD PHHSF @gited on pge IITFA IQP tulio p xvrroD grlos prenkD nd imon hw hiteF e universl density pro(le from hierrhil lusteringF The Astrophysical JournalD RWH@PA XRWQD IWWUF @gited on pges IW nd IISFA IQQ tn r yortF he fore exerted y the stellr system in the diretion perpendiulr to the glti plne nd some relted prolemsF Bulletin of the Astronomical Institutes of the NetherlandsD T XPRWD IWQPF @gited on pge PFA IQR irnst ypikF en estimte of the distne of the ndromed neulF The Astrophysical JournalD SS XRHT!RIHD IWPPF @gited on pge PFA IQS oerto h eei nd relen uinnF gp onservtion in the presene of pseudoprE tilesF Physical Review LettersD QV@PSA XIRRHD IWUUF @gited on pge IHFA IQT torge eñrruiD sily felokurovD x yn ivnsD hvid wrtínezEhelgdoD qerrd qilmoreD wike srwinD wrtin xiedersteEystholtD nd hniel f ukerF s the progeniE tor of the sgittrius strem dis glxy c Monthly Notices of the Royal Astronomical Society : LettersD RHV@IA XvPT!vQHD PHIHF @gited on pge IISFA IQU vidi ieriD tulien vvlleD qinfrno fertoneD nd inzo frnhiniF smplitions of highEresolution simultions on indiret drk mtter serhesF Physical Review DD VQ@PA XHPQSIVD PHIIF @gited on pge PHFA IQV ihrd owellF etls of the universeD mps nd digrmsF PHHTF @gited on pge IHRFA IQW toel rimkF htever hppened to hot drk mtter c arXiv preprint astroph/0112336D PHHIF @gited on pge UFA IRH ghris urellD tmes fullokD irik t ollerudD wiguel ohD nd ukny ghE krrtiF he sgittrius impt s n rhitet of spirlity nd outer rings in the milky wyF NatureD RUU@UQTRA XQHI!QHQD PHIIF @gited on pge IHUFA Bibliographie 239 IRI tohim ipkenD tn gonrdD nd t ottF smplitions for onstrined supersymmeE try of omined hess oservtions of dwrf glxiesD the glti hlo nd the glti entreF Journal of Cosmology and Astroparticle PhysicsD PHII@IIA XHHRD PHIIF @gited on pge IHVFA IRP olfgng e olkeD engel w vopezD nd tn gonrdF vimits nd on(dene intervls in the presene of nuisne prmetersF Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated EquipmentD SSI@PA XRWQ!SHQD PHHSF @gited on pge IPIFA IRQ voï ollndF Etalonnage des cameras de l'experience d'astronomie gamma HESS et observations du Centre Galactique au-dela de 100 GeVF hh thesisD niversité ierre et wrie gurieEris sD PHHSF @gited on pges PI nd IQPFA IRR voï ollndF Etalonnage des cameras de l'experience d'astronomie gamma HESS et observations du Centre Galactique au-dela de 100 GeVF hh thesisD niversité ierre et wrie gurieEris sD PHHSF @gited on pges QT nd RRFA IRS veszek oszkowskiD inrio wri essoloD nd endrew t illimsF ht next for the mssm nd the nuhm X smproved prospets for superprtner nd drk mtter detetionF Preparing for submission to Journal of High Energy PhysicsD riv XIRHSFRPVWvQD PHISF @gited on pge IQFA IRT enny h kett nd vind prkeF he drk hlo of the polrEring glxy ng RTSHFThe Astrophysical JournalD QTI XRHV!RIVD IWWHF @gited on pge IWFA IRU he nhezD f qieelsD h orovD h rsonD qw wdejskiD e xueD et lF wulE tiwvelength mpign on the hl pks£ PISSEQHR X e new insight on its spetrl energy distriutionF arXiv preprint arXiv :1502.02915D PHISF @gited on pge WUFA IRV he nhezD f qieelsD h orovD h rsonD qw wdejskiD e xueD et lF wulE tiwvelength mpign on the hl pks£ PISSEQHR X e new insight on its spetrl energy distriutionF arXiv preprint arXiv :1502.02915D PHISF @gited on pge IHHFA IRW rmish ilverwoodD ghristoph enigerD t ottD nd qinfrno fertoneF e relisti ssessment of the t sensitivity to drk mtter nnihiltionF Journal of Cosmology and Astroparticle PhysicsD PHIS@HQA XHSSD PHISF @gited on pge IISFA ISH pringelD t ngD w ogelsergerD e vudlowD e tenkinsD e relmiD tp xvrroD g prenkD nd hw hiteF he qurius projet X the suhloes of glti hloesD mnrs QWI @deFD PHHVA ITVS!IUIIF arXiv preprint arXiv :0809.0898F @gited on pge IWFA ISI olker pringelD grlos prenkD nd imon hw hiteF he lrgeEsle struture of the universeF NatureD RRH@UHVVA XIIQU!IIRRD PHHTF @gited on pge UFA ISP olker pringelD tie ngD wrk ogelsergerD eron vudlowD edrin tenkinsD emin relmiD tulio p xvrroD grlos prenkD nd imon hw hiteF he qurius projet X the suhloes of glti hloesF Monthly Notices of the Royal Astronomical SocietyD QWI@RA XITVS!IUIID PHHVF @gited on pge UFA ISQ weng u nd hougls pinkeinerF trong evidene for gmmEry line emission from the inner glxyF arXiv preprint arXiv :1206.1616D PHIPF @gited on pges xivD ITH nd PIIFA ISR ergyro sitsiomi nd engel ylintoF hetetility of neutrlino lumps vi tE mospheri herenkov telesopesF Physical Review DD TT@VA XHVQHHTD PHHPF @gited on pge PIFA ISS w vniD q frielliniD e ergnD p fo'elliD e fulgrelliD grveoD gttneoD e ghenD gooD i gostD et lF he gile missionF Astronomy & AstrophysicsD SHP@QA XWWS!IHIQD PHHWF @gited on pge PUFA IST tF F vernetF snternl note from the hFeFsFsF ollortionF PHIPF @gited on pge RPFA ISU qewweEe veqi eie egi ivigyiF qlst siene writer9s guideF PHHVF @gited on pge PUFA ISV y iollD x uominD u uoskD w xumnnEqodoD ri gollortionD et lF e new soure disovered lose to the glti enter X ress jIURIEQHPF sn HIGH ENERGY GAMMA-RAY ASTRONOMY : Proceedings of the 4th International Meeting on High Energy Gamma-Ray AstronomyD volume IHVSD pges PRW!PSPF es ulishingD PHHWF @gited on pge WIFA ISW e inF rospets for drk mtter nnihiltion signl towrds the sgittrius dwrf glxy with ground sed herenkov telesopesF sn Journal of Physics : Conference SeriesD volume QUSD pge HSPHQIF sy ulishingD PHIPF @gited on pge IISFA ITH sl inentD t henneD tp ruppertD wnigotD w he xuroisD xymnD t E vernetD p oussenelD vw ghounetD f hegrngeD et lF erformne of the hess mersF FRONTIERS SCIENCE SERIESD S XPVVU!PVWHD PHHQF @gited on pges QS nd QUFA ITI g eekesD r fdrnD h fillerD s fondD frduryD t fukleyD h grterEvewisD w gtneseD griswellD guiD et lF erits X the very energeti rdition imging telesope rry systemF Astroparticle PhysicsD IU@PA XPPI!PRQD PHHPF @gited on pge PUFA ITP ghristoph enigerF e tenttive gmmEry line from drk mtter nnihiltion t the fermi lrge re telesopeF Journal of Cosmology and Astroparticle PhysicsD PHIP@HVA XHHUD PHIPF @gited on pges xivD PRD VWD ISSD ISWD PHQD PIID PIP nd PPIFA ITQ ghristoph enigerF e tenttive gmmEry line from drk mtter nnihiltion t the fermi lrge re telesopeF Journal of Cosmology and Astroparticle PhysicsD PHIP@HVA XHHUD PHIPF @gited on pge ITFA ITR tulius ess nd tonthn fggerF Supersymmetry and supergravityF rineton niverE sity ressD IWWPF @gited on pge WFA ITS idwrd ittenF wss hierrhies in supersymmetri theoriesF Physics Letters BD IHS@RA XPTU!PUID IWVIF @gited on pge IHFA Bibliographie 241

3

  Improvement of the run quality selection software for H.E.S.S.II analyses 57

QFI snterest of run seletion for rFiFFF nlyses

  hrk wtter nlysis X gittrius hwrf qlxy with rFiFFFs F IHQ RFQFI se of the yxEypp nlysis for hrk wtter detetion F

  Dark Matter in the Universe . . . . . . . . . . . . . . . . . . . . . . . 2

t n energy of IQH qeF pinllyD summry of the presented work nd of the most importnt results is given in the Conclusion setionF Introduction Contents 1.1 1.1.1 Evidence for cosmological Dark Matter . . . . . . . . . . . . . . . . . . 2 1.1.2 Framework : Λ-CDM and WIMP . . . . . . . . . . . . . . . . . . . . . . 7 1.1.3 Particle candidates for WIMP Dark Matter . . . . . . . . . . . . . . . . 9 1.2 Towards indirect detection of the Dark Matter in γ-rays . . . . . . . 12 1.2.1 3 complementary detection approaches . . . . . . . . . . . . . . . . . . . 12 1.2.2 γ-ray ux from Dark Matter halos . . . . . . . . . . . . . . . . . . . . . 18 1.2.3 Dark Matter observational targets and recent results with γ-ray observatories . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23 1.3 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25

  Λ-CDM and WIMP he work in this thesis is sed on the indiret detetion of the hw in the frmework of the ΛEghw wodel of gosmologyF yservtionl evidene reported in 1.1.1 suggest tht the hw prtiles re nonEryoni nd re wekly interting with ryoni mtterF o help (nding onsistent prtile ndidte for the hwD further onstrints on its nture re otined from hw struture formtion predited y the ΛEghw modelD espeilly with results from xEody simultionsD s well s onstrints on its reli density in the primordil niverseF 1.1.2.1 Dark Matter structures formation

	gosmologil prmeter ymol wesurement @lnk PHISA
	rule onstnt	H 0	67.74 ±0.46
	gurvture density	Ω k	0.0008 +0.0040 -0.0039
	hrk inergy density	Ω Λ	0.6911 ±0.0062
	wtter density @ChwA	Ω m	0.3089 ±0.0062
	hrk wtter density	Ω DM	0.2589 ±0.0022
	fryoni density	Ω b	0.0486 ±0.0003
	dition density	Ω r	< 0.001

Figure IFQ ! TVFQ7D WSFR7 nd WWFU7 gv ontours on Ω m nd Ω Λ otined from gwfD typeEI supernove nd fey onstrintsD nd their omintionF he (gure is tken from uowlski et lF @IIPD PHHVAF he PHIS lnk ontrints t TV7 gv re represented in red TT Figure IFR ! wesurement of ΛEghw osmologil prmeters with lnk @TTD PHISA 1.1. Dark Matter in the Universe 7 1.1.2 Framework :

Table IFI ! tndrd wodel prtiles nd their prtners in the ww modelF le dpted from UV 1

 IFI .2 Towards indirect detection of the Dark Matter in γ-rays

	Standard Model particles and elds		Supersymmetric partners
			sntertion eigensttes		wss eigensttes
	ymol	xme	ymol xme		ymol xme
	q = d, c, b, u, s, t qurk	qL , qR	squrk		q1 , q2	squrk
	l = e, µ, τ	lepton	lL , lR	slepton		l1 , l2	slepton
	ν = ν e , ν µ , ν τ	neutrino	ν	sneutrino		ν	sneutrino
	g	gluon	g	gluino		g	gluino
	W ± H -H + B	W Eoson riggs oson riggs oson BE(eld	W ± H-1 H+ 2 B	wino higgsino higgsino ino	   	χ± 1,2	hrgino
	W 3 H 0 1 H 0 2 H 0 3	W 3 E(eld riggs oson riggs oson riggs oson	W3 H0 1 H0 2	wino higgsino higgsino	         	χ0 1,2,3,4	neutrlino
							in PHIS
	t the ollision energy of IQ eF
	1.1.3.3 Other particle candidates
	e lrge numer of nonEsw nd nonE senrios @some models re onsidering extrE
	dimensionsA ould lso explin the nture of the hwF hese re for instne sterile neutrinos
	UT nd exions IQSD mong mny othersF hey will not e disussed in this thesisF e
	omplete review of ll the hw prtile ndidtes is given in fertone et lF @RQD PHHSAF elso
	lterntive theories suh s wyxh IPV nd ee QT n explin the rottionl urves of
	qlxies without the requirement of the hw hypothesisD lthough they nnot ount for
	the oserved properties of qlxy glusters PVF

2.1.3F

st should however e mentioned tht up to dte no evidene for xew hysis hs een reported y the vrg experimentsD t lest t ove the 5σ levelF wore interesting results on this topi re expeted in the ner future with nlysis of dt to e tken

  Reconstruction of the γ-ray events . . . . . . . . . . . . . . . . . . . . . 48 2.3 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 55

	Chapitre 2
	The H.E.S.S. experiment
	Contents
	2.1 Detection of the Very High Energy gamma-rays . . . . . . . . . . . . 28
	2.2 The H.E.S.S. telescope array . . . . . . . . . . . . . . . . . . . . . . . 34 1.3 Conclusions 2.2.1 Cameras . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 35
	he serh for the hrk wtter is urrently one the most tive reserh (eld of the PI st enE 2.2.2 Trigger system . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 37
	turyD t the intersetion etween prtile physisD stroprtile physis nd osmologyF he 2.2.3 Calibration . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 39 oservle niverse is full of grvittionl evidene on the existene of dominnt 4drk4 omponent present t the qlti nd osmologil slesF sn the ΛEghw wodel of gosmoE 2.2.4 Autofocus system . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46
	logy the hw ounts for out PT7 of the totl mssEenergy udget of the niverseD nd 2.2.5
	forms hierrhil hlo strutures Y qlxies re loted t the entres of lrge hw hlosD
	themselves inluded in lrger hlo t the qlxy gluster sleD nd so onF
	ekly snterting wssive rtiles @swsA hve een identi(ed s n exellent senrio
	for mthing theoretil preditions with oservtions nd simultionsD for whih one of the
	est prtile ndidte to dy is the neutrlino χD de(ned eyond the tndrd wodel
	of prtile physisF sn this frmeworkD the sws my e diretly deteted from their di'uE
	sion on hevy tomi nuleiD indiretly from the mesurement of their primry nd seondry
	nnihiltion produtsD or produed in prtile elertorsF
	he work presented in this thesis is sed on the indiret detetion of the hw in γErysD with
	the rFiFFF experimentF o hieve this golD the telesopes re pointing t spei( trgets
	where lrge mounts of hw re expetedD suh s the qlti gentre region nd hwrf
	qlxiesD looking t hrteristi γEry spetrl signtures ove stndrd strophysil
	kgroundsF sn prtiulr monohromti nnihiltion lines produed in χχ → γγ proesses
	would e smoking gun for the existene of hwD nd re t the entre of the presented work
	in ghpter 6D in the qlti gentre regionF hw serhes in hwrf pheroidl qlxies re
	lso investigted in ghpter 4 with the spei( se of the gittrius hwrf qlxyF
	yver the lst dede severl hints for the hw existene hve een reportedD essentilly within
	the permiEve dtD however no experiment n lim for rel disovery t presentD while
	onstrints on the sw nnihiltion rossEsetion strt to reh the nturl sle orresE
	ponding to the hw therml reli density predited y the ΛEghw modelF he deep nture
	of the hw still remins one of the mjor puzzles of the enturyF

Table QFI !

 QFI vist of defult run qulity seletion uts in risunulityD for rFiFFFs nlyses @R telesopes onlyAF he seond olumn shows the numer of runs tht pss the orresponding ut in the (rst olumnD with respet to the totl numer of rFiFFFs runsF he third olumn shows the numer of runs tht pss the orresponding ut nd lso ll the uts present in the previous lines of the tleF Chapitre 3. Improvement of the run quality selection software for H.E.S.S.II analyses 3.4 Adapting ParisRunQuality to H.E.S.S.II analyses he rhiteture of the existing dt quisitionD nlysis nd simultion softwres in the rFiFFF experiment hs initilly een dpted to the use of the four gherenkov telesopes of rFiFFFsD working in stereosopyF ine the ommissioning of the gS telesope in PHIPD huge e'orts hve een provided from the whole rFiFFF gollortion to dpt these softwres for stereosopi nlyses with ll the S telesopesD nd lso monosopi nlyses with the use of the gS telesope loneF sn prtiulr the risenlysis softwre @see 2.2.5A is now well performing with rFiFFFssD while still in progress for improvement of the performnes of the reonstrution of the γEry eventsD signlGkground disrimintion nd of the spetrl reonstrutionFIn this context the improvement of the ParisRunQuality run selection software has been considered as a high priority task, with newly-dened quality selection criteria for the CT5 telescope, and revised cuts for the CT1-4 telescopes. ontrol histogrms tht re displyed in the min qs windowF • he module 4eletionqsFpy4 ontins the de(nition of suEqss for eh of the indiviE dul qulity utsD tht re then inluded in the min qsF • pinlly the 4eletionFpy4 module is where the run seletion is relly tivted Y the 4qsFpy4 nd 4eletionqsFpy4 modules only ontin uttons tht re then ssoited with tions de(ned in 4eletionFpy4F rere the informtion loded from the htse is (ltered with respet to the ut vlues entered mnully in the suEqssD nd the informtion of the runs tht pss ll the qulity seletions is returned s n outputF he ontrol plots nd the informtion in the min qs re then updtedF et the end of the seletion proess the run numers n e sved into Fvs (leD tht is redy to e used for further nlysesF

he modi(tion of the risunulity softwre onsists in dding dditionl seleE tions nd funtions to over new requirements for the gS telesopeD nd tht re esy to ontrol from the qsF elso defult uts hve een de(ned for stndrd run seletions with rFiFFFssF 3.4.1 Structure and modication of the code he generl struture of the ode of risunulity is shown in pigure 3.2F he ode is written in pythonGgCCD with the use of gtk tools for the retion of the qs window nd uttonsF • he 4uneletionFpy4 module lods the run dtse with glol run nd individul teE lesope informtionD tht is now ompleted with informtion out the gS telesopeD this informtion eing ville for use in the other softwre modulesF • he 4qsFpy4 module is the min grphil interfeD tht ws shown in pigure 3.1 nd is used to ommunite etween the di'erent modules of the ode nd to trigger tions when liking on the uttonsF he run informtion loded from the htse is (lled into

  of the run quality selection software for H.E.S.S.II analyses

	Data quality selection cuts in ParisRunQuality (H.E.S.S.II)
		Number of runs	Number of runs
	Selection cuts	after cuts	after cuts
		(this cut alone)	(all above cuts)
	All runs	26403	26403
	All runs with CT5 (H.E.S.S.II) [01/2014 → 06/2015]	2847 (100%)	2847 (100%)
	General run properties
	Run duration ≥ 5 min	2655 (93.3%)	2655 (93.3%)
	Humidity level ≤ 90%	2836 (99.6%)	2644 (92.9%)
	Default cuts on CT5
	Pixel/Sector threshold = 4/2.5	2846 (>99.9%)	2644 (92.9%)
	Corrected trigger rate [1200 Hz ; 3000 Hz]	2677 (94.0%)	2519 (88.5%)
	Trigger rate RMS ≤ 10%	2814 (98.8%)	2514 (88.3%)
	Dead time fraction ≤ 10%	2803 (98.5%)	2494 (87.6%)
	Broken pixel fraction ≤ 5%	2458 (86.3%)	2177 (76.5%)
	Autofocus position [66 mm ; 80 mm]	2844 (99.9%)	2174 (76.4%)
	Autofocus position error ± 5%	2828 (99.3%)	2161 (75.9%)
	Default cuts on CT1-4
	Number of telescopes ≥ 3 including CT5	2372 (83.3%)	1764 (62.0%)
	Pixel/Sector threshold = 4/2.5	2842 (99.8%)	1764 (62.0%)
	Corrected trigger rate [100 Hz ; 300 Hz] on at least 3 telescopes	2658 (93.4%)	1719 (60.4%)
	Trigger rate RMS ≤ 10% on at least 3 telescopes	2649 (93.0%)	1657 (58.2%)
	Dead time fraction ≤ 15% on at least 3 telescopes	2784 (97.8%)	1631 (57.3%)
	Broken pixel fraction ≤ 20% on at least 3 telescopes	2592 (91.0%)	1522 (53.5%)
	Radiometer temperature ≤ -20 • on at least 1 telescope	2819 (99.0%)	1513 (53.2%)
	Radiometer temperature RMS ≤ 3% on at least 1 telescope	2770 (97.3%)	1512 (53.1%)

Table QFP !

 QFP vist of defult run qulity seletion uts in risunulityD for rFiFFFss

  Standard ON-OFF analysis . . . . . . . . . . . . . . . . . . . . . . . . 82

	Chapitre 4
	Standard ON-OFF analysis method
	for astrophysical sources and Dark
	Matter detection
	Contents
	4.1

4.1.1 Principle . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 82 4.1.2 Wobble mode . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 83 4.1.3 ON/OFF pairs from dierent elds of view . . . . . . . . . . . . . . . . 87 4.1.4 Signicance of the signal . . . . . . . . . . . . . . . . . . . . . . . . . . . 88 4.2 Analysis of astrophysical sources . . . . . . . . . . . . . . . . . . . . . 89 4.2.1 Spectral analysis in H.E.S.S. . . . . . . . . . . . . . . . . . . . . . . . . 89 4.2.2 Analysis of HESS J1741-302 . . . . . . . . . . . . . . . . . . . . . . . . . 91 4.2.3 Analysis of PKS 2155-304 . . . . . . . . . . . . . . . . . . . . . . . . . . 97 4.3 Example of Dark Matter analysis : Sagittarius Dwarf Galaxy with H.E.S.S.I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 103 4.3.1 Use of the ON-OFF analysis for Dark Matter detection . . . . . . . . . 103 4.3.2 Dwarf Spheroidal Galaxies . . . . . . . . . . . . . . . . . . . . . . . . . . 103 4.3.3 The Sagittarius Dwarf Galaxy . . . . . . . . . . . . . . . . . . . . . . . 107 4.3.4 Data quality, run selection and cuts . . . . . . . . . . . . . . . . . . . . 109 4.3.5 Standard ON-OFF analysis results . . . . . . . . . . . . . . . . . . . . . 111 4.3.6 Limits on potential DM Continuous signals . . . . . . . . . . . . . . . . 114 4.4 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 117

  2 @seond olumnAF e signi(ne of 7.6σ ws foundF he spetrum of the soure ws extrted ssuming powerElw modelD s shown in pigure 4.8F he (tted spetrl index is Γ = 2.28 ± 0.16 F 4.2.2.2 Cross-check with Parisanalysis e rossEhek study ws done with the prenh rFiFFF softwre @risnlysisA to on(rm the spetrl properties of ri tIURIEQHP nd llow further pulition of the results nd presenttion in onferenesF he rossEhek onsists in stndrd yxEypp nlysis t the position of the soure to derive the signi(ne of the signl exessD nd spetrl reonstrution with powerElw modelF Table RFP ! ummry tle X yxEypp nlysis of ri tIURIEQHPD with reEwe @iF yF engünerA nd risnlysisEwodelCC @rossEhek nlysisA using the wultipleypp kE ground on(gurtion nd hrd nlysis uts @lled 4fint4 uts in risnlysisA he nlysis ws performed with the wodelCC lgorithm for the reonstrution of the γEry eventsD with the use of 4fint4 uts tht re similr to the 4hrd4 uts de(ned in reEweF e run list of RRH runs tken with rFiFFFs etween PHHR nd PHIP ws 94 Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection

	ri tIURIEQHP X yxEypp nlysis results
		reEwe risnlysis rossEhek
	xumer of runs	335	440
	vivetime	141.4h	185.9h
	wen enith ngle	22.7 •	17.3 •
	wen wole o'set	1.39 •	1.26 •
	θ ON	0.1 •	0.15 •
	N ON	642	2166
	N OF F	11834	28060
	α	25.48	15.52
	N excess	178	358
	igni(ne	7.6σ	7.9σ
	Gf	0.38	0.20

  1.2D with signi(ne of 7.8σ nd S/B = 0.20F pinllyD the spetrum of the soure ws reonstruted ove QHH qe nd is shown in pigure 4.12D well (tted y powerElw funtion of spetrl index Γ = 2.18 ± 0.15F4.2.2.3 Discussion of the resultshe rossEheked results with risnlysisEwodelCC re well omptile with reE weF he extended soure ri tIURIEQHP is oserved with signi(ne of 7.6 -7.9σ nd the reonstruted spetrum is well (tted y powerElw funtions of indexes 2.28 ± 0.16 nd 2.18 ± 0.15 with reEwe nd risnlysisEwodelCCD respetivelyD omptile within sttistil error rsF elso the very low event sttistis ville ove IH e does not llow investigting the possiility of n exponentil utEo' in the spetrum @with

Table RFR !

 RFR un qulity seletion uts for the gittrius hwrf qlxy dt smple energy of the reonstruted γErysF his llows investigting the stility of the potentil exess nd lso to void systemti nd sttistil )ututions in the numer of yx nd ypp events ner the energy threshold tht my hide the very wek signl we re serhing for @no exess hs een deteted in former pulitions on grhAF por this nlysis the events strt to show up t out IHH qeF he results re (rst produed without energy utsD then onsidering events ove QHH qe tht orresponds to the verge energy threshold for the PHHTEPHIP periodsD nd (nlly events ove SHH qeF exess nd signi(ne sky mps re presented in pigure 4.21D s well s the signi(ne distriution over the pyF elso (gure 4.22 shows the ngulr distriution of the events in the pyD entred on the position of the soureF he yx region orresponds to the (rst Q ins in θ 2 F he nlysis results re summrized in le 4.5F nlike previously pulished results poE tentil yxEypp exess is oserved t the nominl position of grhD tht strts to show up ove QHH qeF he signi(ne of the exess is 2.5σ ove QHH qeD nd inreses with the ut in energy up to 3.0σ ove SHH qeF et this stte of the nlysisD suh low exess signl is still omptile with sttistil

	110 Chapitre 4. Standard ON-OFF analysis method for astrophysical sources and Dark Matter detection 4.3. Example of Dark Matter analysis : Sagittarius Dwarf Galaxy with H.E.S.S.I 111
	ht ulity guts 4.3.5 Standard ON-OFF analysis results min mx	gomments
	xumer of telesopes	R	R	ll rFiFFFs telesopes
	un durtion	PVmin	PVmin	full durtion
	wen zenith ngle	0 •	30 •
	gentrl trigger rte	IHH rz SHH rz
	gentrl trigger rte w	H%	R%
	PEfold dedtime frtion	H%	PH%
	froken pixels frtion	H%	PH%	t lest on Q telesopes
	diometer temperture	-100 •	-20 •	t lest on I telesope
	gittrius hwrf qlxy X yxEypp nlysis results
	Energy cut	no cut E > 300GeV E > 500GeV
	xumer of runs		142
	vivetime		61.6h
	wen enith ngle		14.1 •
	wen wole o'set		0.72 •
	θ ON		0.1 •
	N ON	1067	603	318
	N OF F	18670	9920	4865
	α	18.23	18.31	18.32
	N excess	43.1	61.2	52.4
	igni(ne	1.3σ	2.5σ	3.0σ
	Gf	0.04	0.11	0.20
	Table RFS ! ummry tle X yxEypp nlysis of the gittrius hwrf qlxy using E
	risnlysisD with rFiFFFs dt

he

  Maximum Likelihood formalism . . . . . . . . . . . . . . . . . . . . . . 120 5.1.1 Principle . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120 5.1.2 Binned Maximum Likelihood . . . . . . . . . . . . . . . . . . . . . . . . 120 5.1.3 Modied Poisson Maximum Likelihood with ON and OFF regions (Rolke)121 5.1.4 Binned Poisson Maximum Likelihood with energy side-bands . . . . . . 121 5.1.5 Un-binned Maximum Likelihood . . . . . . . . . . . . . . . . . . . . . . 122 5.1.6 Towards an extended un-binned "Full" Likelihood method for Dark Mat-

	Chapitre 5
	Development of an un-binned Full
	Likelihood Method to search for Dark
	Matter Line-like signals with H.E.S.S.
	Contents
	5.1

ter searches . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 122 5.2 Full Likelihood method . . . . . . . . . . . . . . . . . . . . . . . . . . . 123 5.2.1 General description of the method . . . . . . . . . . . . . . . . . . . . . 124 5.2.2 Development of the method . . . . . . . . . . . . . . . . . . . . . . . . . 127 5.2.3 Statistical estimators . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 140 5.2.4 Performances of the method with Monte-Carlo simulations . . . . . . . 145 5.3 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 155

  120 Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

	vineElike signls re onsideredF hose developments pve the wy to the dt nlysis
	performed in ghpter 6 in the qlti gentre regionF
	5.1 Maximum Likelihood formalism
	5.1.1 Principle
	he wximum vikelihood @wvA formlism mkes use of vikelihood funtion tht depends
	on one or severl prmeters of given model θF he est (t of these prmeters @the
	preferred modelA is otined when mximizing the ssoited multiEvrile vikelihood
	funtionF por set of n independent vriles x = (x 1 , ..., x n )D the most generl expression
	for the vikelihood funtion is X
	L( x| θ) =

n i P DF (x i | θ) @SFIA where P DF (x i | θ) is the roility hensity puntion tht provides the proility to mesure vlue of x i given ssumed model depending on prmeters θF sts vlue vries etween H nd ID nd its integrl over the whole rnge of the mesured vriles x i is IF sully x i represents the mesured vriles for eh individul event i = 1, ...n deteted y the experimentF 5.1.2 Binned Maximum Likelihood

  the performnes of the pull vikelihood method will e reviewed for oth the rFiFFFss wono nd tereo telesope on(gurtionsF 128 Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

			rFiFFFs	rFiFFFss
		sps	tereo	wono	tereo
		eeptne @m 2 A	E	5.0 × 10 3 2.3 × 10 3
	IHH qe	inergy is @%A inergy resolution @%A	E E	+23 21.5	+12 13.0
		engulr resolution @ • A	E	0.250	0.125
		eeptne @m 2 A	1.2 × 10 4 3.9 × 10 4 4.9 × 10 4
	PHH qe	inergy is @%A inergy resolution @%A	+2.0 9.6	-3.7 25.2	-4.7 12.2
		engulr resolution @ • A	0.081	0.182	0.083
	I e
					nd
	tereo

•

• yptil e0ieniesa78.4% for gS nd 52.5% for the other R telesopesD representtive of the oservtion runs tken in the eginning of PHIRF le 5.1 referenes sp vlues t IHH qeD PHH qe nd I eF es expeted rFiFFFs nd rFiFFFss tereo re equivlent t high energies sine gS only rings dditionl senE sitivity t low energiesF rFiFFFss wono hs lower eeptne threshold t high energies nd worse inergy nd engulr resolutions sine only gS telesope is onsidered nd the reonstrution of the γEry events without stereosopy is less urteF sn setion 5.2.4

Figure SFI ! snstrument esponse puntion @sFFpFsA of rFiFFF to gmmErysF he eE eptne in m 2 D the inergy is @%AD the inergy resolution @%A nd the engulr resolution @ • A re represented for the Q telesope on(gurtions X rFiFFFs tereoD rFiFFFss wono

Table SFI !

 SFI lue of the snstrument esponse puntions t IHH qeD PHH qe nd I e in rFiFFFs stereo nd rFiFFFss wono & tereo telesopes on(gurtions 130 Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S. 5.2.2.2 Probability Density Functions Denition he roility hensity puntion of the event i desries the proility for the model prmeters M ( θ) to e onsistent with the mesured quntities of this event E i D t i D φ x D φ y nd φ z F sts vlue lies etween H nd ID nd its integrl over the whole phseEspe of the mesured quntities is IF nder the ssumptions desried in 5.2.1.2 nd 5.2.1.3 the hp is funtion of signl hp nd kground hp tht depend on the signl nd kground model prmeters respetively nd on the individul mesured energies E i onlyF e deteted event i of energy E i hs proility P DF S (E i ) to e signl event nd proility P DF B (E i ) to e kground eventF PDF and energy spectra P DF S nd P DF B shpes re relted to the energy spetr of the signl nd the kground omponentsF roweverD sine mesured dt is 'eted y sps the mesured energy distriE utions re not nymore representtive of the originl gmmEry spetrumF gonsequently there re two possiilities for generting the hps X

Table SFP !

 SFP -2∆ln(L) vlues ssoited with on(dene levels @%A orresponding to douleE sided gs nd for the reonstrution of m model prmetersF

  142 Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S. 5.2.3.2 Test Statistics and Signicance vet ssume pull vikelihood multiEvrile (t of model prmeters θ nd mesured vriles xF he est ttistis @A estimtor is de(ned from the rtio of the wximum pull vikelihood vlues for two di'erent hypotheses on the model θD most generlly 4existing signl4 versus 4no oserved signl4F st estimtes the preferred hypothesisF

	T S = -2ln	L( x| θ, rypothesis P) L( x| θ, rypothesis I)	@SFIUA
	sf only one prmeter is involved in the null hypothesisD the signi(ne ssoited with the
	vlidtion of rypothesis I with respet to rypothesis P is derived from the vi&w formul
	IIW

  Response Functions (I.R.F.s) : he ltest ville rFiFFFss wono nd ryrid response funtions shown on (gure 5.1 re usedF hey orrespond to enith engle a 18 • D wole o'set a 0.5 • D ezimuth engle a 180 • nd optil e0ienies a 80% in gS nd 60% in the R smller telesopesF • Energy window : [200GeV ; 3T eV ]F his gives su0ient lever rm with P DF S nd P DF B nd llows reonstruting m χ in omfortle mss rngeF ynly energies ove PHH qe re onsideredD where the present nlysis softwre is est opertingF his voids ontmintion y systemtis due to eptne t the energy threshold of the instrument whih re not studied hereF • Background PDF : e use wg simulted kground hp whih is omiE ntion of the osmiEry @owerEvw index a PFU C sFFpFsA nd di'use @owerEvw index a PFQ C sFFpFsA hp disussed in 5.2.2.2D with frtion of the di'use omponent of 6% with respet to osmiErysF

Table SFR !

 SFR ummry tle X erformnes of the pull vikelihood method with wg simulE tionsD for the PhEreonstrution of the input prmeters (η, m χ ) input D in wono nd tereo teE lesope on(gurtionsF por eh ouple of input prmeters the is de(nes the error etween the input nd the reonstruted vluesD while σ 95%CL represents the sttistil unertinty t WS7 ontinment of the SHH wg simultions @tht is here simple IhEprojetion of the Ph ontourA 154 Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

	HFHS	HFPS	EPPFHR	QQFQQ	HFWP	PPFPH	EVFHH	QHFVQ	HFHR	VFTW
	HFHS	HFQ	EWFTH	QPFTV	HFRU	IVFPR	HFSP	QTFPP	EHFRU	UFSW
	HFHS	HFS	PFIV	PWFVW	EHFHP	IPFIT	QFIP	PQFWW	HFHT	RFVW
	HFHS	HFU	IFUP	PPFTW	HFPH	WFWS	QFHR	IUFIQ	EHFHI	SFPR
	HFHS	I	IFRV	IVFIW	HFI	TFSU	IFQT	IRFPH	EHFHR	QFTU
	HFHS	P	IFSR	IIFUS	EHFIS	SFHP	IFPH	TFQT	EHFHS	PFVI
	HFS	HFPS	EIRFVH	IFRI Mono	HFPR	IFRI	ESFWT Stereo HFWW	HFRV	HFRW
	HFS	HFQ	EUFIH	IFPI	HFIQ	IFPU	EHFST	HFUV	HFIU	HFSU
	HFS	HFS	EHFVH	HFWI	HFHT	IFHT	EHFHP	HFRV	HFHT	HFRR
	HFS	HFU	EHFIP	HFUU	HFHR	HFWH	HFHT	HFUV	H	HFQS
	HFS	I	HFHR	HFTP	H	HFUV	EHFHP	HFRW	H	HFPW
	HFS	P	H	HFRI	H	HFVI	EHFHP	HFQQ	H	HFQU
	HFHS	HFPS	EPPFHR	QQFQQ	HFWP	PPFPH	EVFHH	QHFVQ	HFHR	VFVI
	HFI	HFPS	EPPFWV	ISFRS	HFST	IHFWR	EWFSR	IRFVI	EHFIP	RFII
	HFP	HFPS	EPIFTH	UFPI	HFQT	RFSU	EVFVS	SFTH	HFPR	IFRU
	HFQ	HFPS	EIWFSQ	RFIH	HFPV	PFVI	EUFWU	QFHP	HFHV	UFVQ
	HFS	HFPS	EIRFVH	IFQW	HFPR	IFRP	ESFWT	HFWR	HFRV	HFRW
	HFHS	P	IFSR	IIFUR	EHFIS	SFHP	IFPH	SFVU	EHFHS	PFVI
	HFI	P	HFQH	TFHI	EHFHS	QFHH	HFPH	PFVP	EHFIH	HFTS
	HFP	P	HFIH	PFQQ	EHFHS	IFVW	HFIH	IFIW	EHFHS	HFVU
	HFQ	P	HFHQ	IFRP	H	IFQP	H	HFSP	EHFHS	HFSR
	HFS	P	H	HFRI	H	HFVI	EHFHP	HFPR	H	HFPU

  • , and represents less than 0.5% of the total number of reconstructed events in the R.O.I. (including the cosmic-ray background).

	oure	plux IQH qe % gr plux I e % gr
	gr xeul	4.93e -9	100%	3.76e -11	100%
	ri tIURIEQHP	2.22e -11	0.45%	2.12e -13

Table TFQ !

 TFQ gomprison of )ux ontriutions from ri tIURIEQHPD gr xeulD glti di'use emission nd eniger IQH qe vineF pluxes re expressed in γ.cm -2 .s -1 .T eV -1 6.4 Contribution of nearby source HESS J1745-303

  Data quality and run selection ht qulity heks hve een performed in two steps X the (rst step using stndrd seletion with the new rFiFFFss E updted risrunqulity softwre @see ghpter 3 for detils out the softwre developmentsA nd the seond step looking t kground mps for heking the homogeneity of the kground events ndGor unexpeted fetures in the pFyFF 6.5.2.1 Parisrunquality software selection e run seletion sed on dt qulity riteri hs een performed using the risrunqulity softwreF he softwre ompiles glol run nd individul telesope informtion displyed in histogrmsF he suspiious runs n e rejeted following to hosen run seletion riteriF hefult pro(les re ville in the grphil interfe ut sine it is preferle to sve s mny runs s possile for the permi rotspot nlysis it hs een deided to relx some of the seletion uts ordinglyF sn prtiulr the dedtime nd roken pixel frtion of telesopes gIER re prtiulrly high in the vine n dtset ompred to the usul dt smples with rFiFFFsD nd (ne tuning of those qulity seletion uts ws then neessry to void too lrge run rejetionF le 6.5 lists the dt qulity riteri nd uts tht re pplied to the whole vine n dtsetF

	6.5.2 Data Quality Cuts		min	max		Comments
	Number of telescopes		4	5		including CT5
	Trigger rate CT1-4		100 Hz 300 Hz at least on 3 telescopes
	Trigger rate RMS CT1-4	0%	10%		at least on 3 telescopes
	Deadtime CT1-4		0%	15%		at least on 3 telescopes
	Trigger rate CT5		1200 Hz 3000 Hz
	Trigger rate RMS CT5	0%	10%
	Broken pixels fraction CT1-4	0%	25%		on all 4 telescopes
	Broken pixels fraction CT5	0%	10%
	Autofocus position CT5	60mm	80mm
	Autofocus error CT5		-10%	+10%
							efter seletion
							veft	ight
		runs	hours	runs	hours	runs hours runs hours
	P4 @eprilA	PP	WFI	IS	TFQ	U	QFP	V	QFI
	P6 @tuneA	QI	IQFS	PQ	IHFP	IH	RFR	IQ	SFV
	P7 @tulyA	RP	IVFS	QW	IUFI	IR	TFI	PS	II
	Total	WS	RIFI	UT	QQFT	QH	IQFU	46	19.9
		Table TFR ! vine n dt tken in PHIR

  6.7. Choice of H.E.S.S.II reconstruction : Mono / Stereo 187 In conclusion, all those arguments are going in favour of the Stereo reconstruction for the Line analysis presented, that brings best sensitivities to Line signals for the whole scan between 100 GeV and 2 TeV. Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II 6.8 Probability Density Functions he roility hensity puntion formlism hs een introdued in hpter 5F he hps re the most importnt elements for improving the performnes of the methodD whih re sed on the spetrl signtures of the signl nd the kground omponentsF sn this setion the genertion nd the (tting proedure of the signl nd the kground hps re desried in the ontext of the present vine n dt nlysisF he vine signl hp is generted from wg simultions for wide rnge of msses down to IHH qeD while the hoie of n optiml kground hp dpted to this spei( nlysis on(gurtion is fully desriedD resulting in the use of ypp kground regions in the pFyFF to estimte the hp shpeF 6.8.1 Line signal P.D.F.

Table TFT !

 TFT he xf is the min kground noise deteted in rFiFFF mersD kground light resulting from the ontriution of strs in the night sky nd tht rndomly triggers the mers with hrteristi pixel rte from SHwrz to QHHwrz depending on the oserved region of the skyF he xf rndomly 'ets the numer of photoEeletrons deteted in eh mer pixel nd dds ises to the shower imgesD interfering with rel gherenkov photonsF he xf photons n lso unexpetedly trigger the detetor like n inident strophysil γEry or kground osmi ryF e lrge frtion of these xf gmmElike events re rejeted with pproprite xf uts in the nlysis hin nd shower imges lened during the lirtion proess @see ghpter 2AF he e'etive xf level @fter gmm events reonstrutionA in the qg region n vry etween IHH nd QHH wrz with n verge vlue of IPS wrz t the permi rotspot positionD while the e'etive xf level in the region of u PISSEQHR is of out TH wrzF he wg dtset ws produed with stndrd sFFpFs tht hve defult xf level of IHH wrzF e deeper look t the e'et of the xf level on the energy threshold ws done in the frme of this nlysis with the prodution of pull wg simultions @omplete simultions tht hndle everything from the genertion of ir showers to the struture of the detetorA with di'erent input xf levelsF foth wono nd tereo simultions were onsidered with SHD IHHD IPS nd PHH wrz nd ompred the resulting eptne funtion with respet to the energyF his omprison is shown on pigure 6.20F e signi(nt impt of the xf level is oserved on the energy thresholdD more pronouned in wonoF he ftor in eptne etween SHwrz nd PHHwrz is of out IQ t VH qe @T t IHH qeA in wonoD while T t VH qe @Q t Figure TFPI ! gomprison of the kground hp from ontrol smple vine n R nd from wg simultions t di'erent xf levels in wono nd tereo telesope on(gurtions inergy vlues orresponding to the mximum of the kground hp distriuE tions for the vine n R dt nd wg dt t di'erent xf levelsIHH qeA in tereoF feyond PHH qe there is only moderte e'et of the xf level on the eptne shpe euse lmost ll xf events re removed y the shower seletionsF imilr studies hve lso een performed for the energy is nd energy resolution nd hve shown tht those sFFpFs re stle with respet to the xf levelF he seond step onsists in heking if the xf level is su0ient explntion for the high energy threshold seen in the vine n R dtsetF yn pigure 6.21 the kground hp for the vine n R dt smple @ypp woleA is ompred with the wg hps t the di'erent xf levels etween SH nd PHH wrzF por given xf level the ssoited wg kground hp hs een genertedD smered y the eptne reported in pigure 6.20 t tht given levelF le 6.6 summrizes the energy vlues orresponding to the mximum of these hp distriutionsF sn wono n xf level ∼PHH wrz reprodues the vine n R dt t low energies @`PHH qeAF sn tereoD n xf level of PHH wrz is not su0ient to mth R dtF yn the other hndD the verge xf level in the permi rotspot region is out IPS wrz nd then the dierences between MC and Line Scan background PDFs cannot be explained by a simple dierence in NSB levels, even if this contributes to a signicant extent. gonerning the hp shpe t higher energies @b PHH qeA the R dt hs softer powerElw index thn wg X rel dt is then more omplex thn simple omintion of region with H.E.S.S.II

		Background PDF : Energy value at maximum (TeV)
			MC PDF		Line Scan P4
	NSB level (MHz)	50	100	125	200	<125>
	Mono	0.098 0.119 0.118 0.138	0.140
	Stereo	0.139 0.136 0.140 0.149	0.164

Table TFU !

 TFU tudy of the systemtis from the instrument response funtionsF xuisnes re dded on the input vine energy E line nd on the energy resolution nd the impt on the reonstrution of 5% vine frtion is investigted 6.10.2 Systematics on the background PDF t e Iσ nuisne is introdued on the most sensitive kground hp (t prmeter when omputing the pull vikelihood funtionF his nuisne only 'ets the vikelihood formul nd not the wg event genertion in order to evlute its impt on the reonstrution of the vine signl frtionF he (rst step onsists in (nding the most sensitive (t prmeter de(ned in 6.8.2.2 X sine p 3 nd p 4 re normliztion onstnts no nuisne ftor n e pplied on those prmeters s the hp is renormlized to I in the proessF elsoD p 0 just de(nes the seprtion in energy etween the vndu nd the powerElw (ts of the hpF ynly p 1 D p 2 nd p 5 hve to e onsideredF por given hp (t prmeterD the nuisne ftor is de(ned s Error 68%CL ((t prmeter) is the unertinty resulting from the χ 2 (t of the inned hp funtionF smpt on the 5% vine frtion reonstrution is presented in le 6.8F hese results show signi(nt hnge in se of IQH qe vine tht produe systemtis t the order of ±15 -20% on the reonstruted vine frtion ηF he most sensitive prmeter t IQH qe is p 1 iFeF the position of the mximum of the kground hp whih is diretly relted to the energy threshold of the experiment nd to the rFiFFF eptne s the IQH qe vine is loted very lose to the energy thresholdF e smll hnge in tht hp prmeter rings lrge systemtis in the reonstrution of the signlF his shows the importne of very good modelling of the kground hp s n input of the pull vikelihood proedureF yn the other sideD vine signls over QHH qe re loted in the powerElw prt of the kE ground distriution nd re less 'eted y nuisnes on the lowEenergy side @prmeters p 1 nd p 2 AF es expeted the dominnt systemtis is due to the powerElw index p 5 nd is of the order of only 2 -5% t SHH qe nd 1 -2% t VHH qeF he systemtis re deresing with the vine energy euse the lol numer of kground events dereses nd then the reltive vlue of η is inresing for (xed glol frtion of 5%F

	6.10. Systematics							199
	follows X	xuisne = irror 68%CL @(t prmeterA.sqrt(	χ 2 ndf	)	@TFQA
	where IQH qe	SHH qe		VHH qe
	hp (t prmeter		-1σ	+1σ	-1σ	+1σ	-1σ	+1σ
	p1 @energy t mximumA	-21.0% +15.0% +0.3% -3.4% +0.3% -1.4%
	p2 @width round mximumA	+8.2% -12.9% -3.2% +0.1% -1.4% +0.5%
	p5 @powerElw indexA	-16.9% +11.0% +2.2% -4.7% -2.3% +1.4%

Table TFV !

 TFV tudy of the systemtis from the kground hp (tF ±1σ nuisnes re dded on the relevnt (t prmeters in order to evlute the impt on the vine frtion reonstrutionD (xed to e η = 5% 6.10.3 Systematics on the diuse emission component he glti di'use emission omponent is prtilly inluded in the kground hp from the vine n dtD ut its ext mountD spetrum nd sptil distriution in the qlti plne remin unknown under PSH qeD unless extrpolted from rFiFFFs or permiEve mesurementsF ystemtis on the numer of di'use events nd on the di'use powerElw index re evluted with the wg kground hp de(ned in 6.8.2.1 insted of the vine n dt hpF e nuisne of ±100% is introdued on the di'use frtion D =

	N dif f use
	N dif f use +N bckg

Table TFW !

 TFW tudy of the systemtis from the di'use emission omponent in the kground hpF xuisnes re dded on the di'use frtion h with respet to the totl kground events nd on the di'use spetrl index6.10.4 Summary on the systematics le 6.10 summrizes the ove systemtis on the sFFpFsD the kground hp nd the di'use emission omponent for the reonstrution of 5% vine signl frtionF ynly the lrgest errors on η tken from les 6.7D 6.8 nd 6.9 re representedF he totl systemti unertinties re lulted from the qudrti omintion of the Q ontriutionsF

	ystemtis	IQH qe SHH qe VHH qe
	sFFpFs	+7.5% -9.6%	+3.1% -14.1%	+1.7% -13.9%
	fkground hp	+15.0% -21.0%	+2.2% -4.7%	+1.4% -2.3%
	hi'use emission	+6.8% -7.4%	+3.3% -7.1%	+2.5% -7.7%
	otl	+18.1% -24.3%	+5.0% -16.5%	+3.3% -16.1%

Table TFIH !

 TFIH ummry of the systemtis in the reonstrution of the vine frtion with the pull vikelihood proedureF vine signls t IQHD SHH nd VHH qe re onsidered with n input frtion η = 5%

  6.10 is onsidered to e onservtiveF 202 Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II 6.11 Update -New software version release (v.30)

  6.11. Update -New software version release (v.30) 203 he yx event distriutions for the vine n R dtset re presented in pigure 6.25 with the new softwre relese @vFQHA for the tndrdD voose nd pint gmm reonstrution utsF he energy threshold n e signi(ntly lowered when onsidering the voose utsD whih is of interest for the reonstrution of the IQH qe vineD while keeping the expeted hw signl frtion tht ws lulted from the permiEve results ITP under the previous softwre version @vFPVD tndrd utsAF yn the other hnd with pint uts the energy threshold is too high for the reonstrution of vine signls down to IHH qeF From now on, the analysis of the Line Scan data is performed in Stereo telescope conguration with Loose cuts for the reconstruction of the gamma-like eventsF he updted exess nd signi(ne mpsD thet 2 plot nd the energy distriutions for yxD ypp nd yxEypp re presented on pigure 6.26F he distriution of signi(nes derived from kground )ututions follows qussin distriution s expetedD with signi(nt exess in the pieldEofEiew t the position of gr eBF Using the standard ON-OFF analysis method, no signicant excess (< 1σ) is found in the 0.4 • R.O.I. at the Fermi Hotspot position. 10 -1 1.56 * 10 -1 3.21 * 10 -2 6.62 * 10 -1 1.24 * 10 -3 2.59

	206	Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II
	6.12 Monte-Carlo studies & performances of the Full Likeli-
		hood method
				Background PDF parametrization
		Software version	p 0	p 1	p 2	p 3	p 4	p 5	χ 2 /ndf
		v.30	1.82 * 1.48
		v.28	2.50 * 10 -1 1.73 * 10 -1 3.15 * 10 -2 8.74 * 10 -1 1.96 * 10 -3 2.66	0.19
	Table TFII ! pit prmeters of the kground hpD for previous @vFPVA nd updted @vFQHA
	versions of the rFiFFF softwreF he hp prmetriztion orresponds to eqF6.2

he new kground hp for the pull vikelihood method is presented in pigure 6.27 nd is (tted y the sme funtion prmetriztion @eqution 6.2A with the following prmeE ters X p 0 = 1.82 * 10 -1 eD p 1 = 1.56 * 10 -1 D p 2 = 3.21 * 10 -2 D p 3 = 6.62 * 10 -1 D p 4 = 1.24 * 10 -3 nd p 5 = 2.59F he hiEsqure for the (t is chi 2 /ndf = 43.0/29 = 1.48F hese (t prmeters re lso presented in le 6.11 in omprison with the previous prmeters from setion 6.8.2.2F QU ins in energy were onsidered etween TH qe nd Q eD orresponding to PR ins on the energy window VH qe Y I e nd PT ins on PHH qe Y Q e for the vikelihood (tF pinlly the exess in the FyFsF hs een redued y ftor of (ve with respet to the previous softwre version @vFPVAF st orresponds to frtion of IFIU7 of the dt events nd vi8w exess signi(ne of HFTσD omptile with sttistil )ututionsF

The excess observed below 130 GeV in the ON-OFF energy distribution can be associated to a statistical uctuation or a residual systematics in ON-OFF normalization. region with H.E.S.S.II Figure TFPT ! hei with ltest softwre relese X ixess mpsD igni(ne mpsD θ 2 disE triution nd inergy distriution for the nlysis of the vine n R dtset with rFiFFFss tereo telesope on(gurtion 6.11. Update -New software version release (v.30) 205 Figure TFPU ! hei with ltest softwre relese X fkground hp for the vine n R dtsetD for the rFiFFFss tereo telesope on(gurtionF he hp is (tted etween VH qe nd Q e with χ 2 /ndf of 43.0/29 = 1.48F he hp otined with the previous softwre version is lso represented

  6.12. Monte-Carlo studies & performances of the Full Likelihood method 211 wg sensitivity limits on < σv > re presented in pigure 6.30FThe obtained MC < σv > limits are lling the gap in energy between H.E.S.S.I and Fermi-LAT Line searches. They complete the H.E.S.S.I mass scan at energies under 500 GeV for a comparable livetime of ∼ 100h, and are competitive with the Fermi-LAT limits under 300 GeV with only 20h of observation time (while 3.7 years of data with Fermi). In particular the scan goes suciently down in energy to allow investigating the potential 130 GeV Line feature reported by C. Weniger [162], D. Finkbeiner [153] and the Fermi Collaboration [10].

  -27 cm 3 .s -1 ) Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II 6.13 Analysis of the Line scan P4 data sample 6.13.1 Mass scan between 100 GeV and 2 TeV

	214	Chapitre 6.
		HFI	IIV	TFHV	HFTH
		HFIQH	IRS	QFUQ	HFTP
		HFP	IRP	IFUV	HFTW
		HFQ	IHU	HFWI	HFVH
		HFR	VW	HFTR	HFWW
		HFS	UW	HFSP	IFPS
		HFT	TP	HFQV	IFQQ
		HFV	SH	HFPV	IFUV
		I	RP	HFPQ	PFPP
		P	QS	HFIV	UFPU
	Table TFIQ ! ummry tle X wg limits t 95% gv for the mss sn etween IHH qe
	nd P eD orresponding to PHh of oservtion time

Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

Reconstruction of the model parameters (η, m χ )

he inputs of the pull vikelihood method re X

• he Region Of Interest @yx regionA eFgF the hw signl serh region • he N ON individual events in the ROI with measured energies E i • he number of background events N OFF in the kground ontrol regions • he Instrument Response Functions of H.E.S.S. tht depend on the γ reonstrution model nd utsD nd on the energy • Probability Density Functions for the DM signal and the cosmicray/astrophysical backgroundsF ih individul event in the ys is ssoited to proility to e signl event @P DF S A nd proility to e kground event P DF B D relted to their expeted spetrl ontriutionsF

• he Energy range for the (t of the model prmeters he generl struture of the pull vikelihood proedure is summrized in digrm on pigure 5.4 where the intertion etween ll the ove inputs nd the steps of the (tting proess re presentedF he im is to (t the hw signl frtion in the ys η = s s+b nd the hw prtile mss m χ F he numer of kground events in the ys n lso e (tted in the proess ut s this numer is estimted from the ypp regions it is here introdued s (xed prmeterF he oisson term for ypp @from eqution 5.9A then eomes onstnt term with b = N OF F /αF snsted sttistil kground )ututions will e introdued in the wg performne studies in 5.2.4 y produing N OF F from qussin of width √ N OF F for lrge numer of independent experimentsF he resulting pull vikelihood funtion is PEdimensionl in prmeter spe with model prmeters (η, m χ ) nd mesured vriles

por given mss m χ in the Ph lultion proessD the logEvikelihood funtion is the sum of oisson nd hpe vikelihood pro(les in ηF his is desried on pigure 5.5F he (gure shows tht the omintion of oisson nd hpe terms in η improves the performnes of the (t s the result is nrrower vikelihood pro(leD here with rel exmple of the reonstrution of hw vine signl with input prmeters (η true = 5%, m χ true = 700GeV )F he resulting minimum is the est (t vlue of η t tht given mss stepF he proess is repeted on the whole mss rnge resulting in PEdimensionl vikelihood funtion in Signicance of the reconstructed signal por eh of the SHH simultions the est ttistis estimtor de(ned in 5.2.3.2 is lulted nd (lled into histogrmF he lirted signi(ne ssoited with the reonstrution of the vine signl (η, m χ ) is derived from the medin vlue of the distriutionD with N σ = medin(T S)F en exmple of distriution is shown on pigure 5.11 with the reonstrution of vine signl t (η = 5%, m χ = 300GeV ) in tereo telesope on(gurtionF prom these wg studies it is then possile to investigte the required vlues of the true prmeters (η, m χ ) true tht llow the reonstrution of the exess with 5σ signi(ne @without systemtisAF Sensitivity limits edditionlly to the reonstrution of signl exess @η true > 0AD the performnes of the method re lso evluted for η true = 0 with the lultion of upper limits t 95% gv on η t given m χ D then on the numer of reonstruted γEry events nd (nlly on the )ux nd on the nnihiltion rossEsetion for the χχ -→ γγ nnihiltion hnnelF rere the lultion of η 95%CL is performed for eh of the SHH simultions ording to 5.2.3.3 nd the results re then (lled into n histogrm in η 95%CL F he prmeter spe is onstrined to physil vlues η 95%CL ≥ 0F he lirted upperElimit in η is de(ned s the medin vlue of the distriutionD s shown on pigure 5.12F Chapitre 5. Development of an un-binned Full Likelihood Method to search for Dark Matter Line-like signals with H.E.S.S.

Figure SFIS ! esults X sensitivity limits of the pull vikelihood method using wg dt when no vine signl events re simulted @η input = 0AD for oth rFiFFFss wono nd tereo telesope on(gurtionsF ih dt point represents lirted limit on SHH experimentsF vestigte the smllest reonstrutile frtion using sensitivity limits of the pull vikelihood methodF pigure 5.15@A shows the lirted limit t WS7 gv on the reonstruted vine frtion when no vine signl events re simulted @η input = 0AF gorresponding limits on the γEry )ux re presented on (gure 5.15@A per sterdin unit so tht the result is independent of the hosen ysF he relted numers re given in le 5.5F he limits re ∼ 15 -20% etter in tereo on(gurtionF he method is le to reonstrut vine signl frtions down to IFS7 level with WS7 gv in wono nd IFQ7 in tereo for QHH qe mssD nd down to 0.3% level in wono nd tereo t P eF his orresponds to γEry )uxes of out 1 -2 * 10 -4 γ.m -2 .s -1 .sr -1 nd 1 -4 * 10 -5 γ.m -2 .s -1 .sr with R me to n endF hen the optimized proedure will e pplied on the T nd U dt smples for minimizing the tril ftorsF 6.5.4 Standard analysis of the Line P4 data ine R dt is unElinded nd urnt for (nl results we n proeed to s mny tests nd optimiztions s neessry for rehing the est sensitivity to the vine signlsF pirst test onsists in looking t the results from stndrd yxEypp nlysis @see ghpter 4A of the vine n R dt t the permi rotspot @V runsD QFIhA using the optimized FyFsFD from whih potentil prolems in the reonstrution of the gmm events re investigtedF his ompletes the qulity heks tht hve een performed with risrunqulityF ixess nd signi(ne mpsD theta 2 distriution of the eventsD energy distriutions for yxD yppD yxEypp nd eptne mps were produed for oth wono nd tereo telesope on(gurtionsF pigure 6.14 shows stndrd nlysis plots for the vine n R dt smple pointing t the permi rotspotF he sky mps don9t show ny exess t the permi rotspot positionD however the vi&w signi(ne is unexpetedly high in wono t the level of RFPσ @PRI exess eventsAF sn tereo the vi&w signi(ne is PFPσ @VU exess eventsAF yn the other hnd n exess is lerly seen in oth wono nd tereo energy distriutionsD onentrted elow PHH qe nd tht ould explin the unexpetedly lrge exess signi(nesF st seems tht we re more likely deling with lrge ises in the dt ner the energy thresholdD whih mimis the IQH qe vine we re looking for 3

Investigations on the nature of the bias ixtended studies were done in order to understnd the nture of the is oserved in the dt elow PHH qeF sn prtiulr dditionl nlyses hve een performed of the vine n R dt smple t T di'erent pointing positions round the permi rotspot s sptil sideEnds for testing the yxEypp reonstrutionF R pointings lie in the qlti lne (-0.7

while the P others lie t ±0.8 • ltitude from the permi rotspotF inergy distriutions were omputed nd re shown on pigure 6.15 for the T onsidered pointing positionsD with the wono reonstrutionF imilr exesses elow PHH qe re oserved in those sptil sideEndsF he sme fetures re lso oserved with the tereo reonstrutionF e seond test hs een performed on ontrol smple u PISSEQHR using list of SI runs tht pssed defult uts in the rFiFFFss tereo seletion pro(le within risrunqulity nd requiring zenith ngles < 20 • F he ide is to look t lnk (elds in the (eld of view of the soure where only hdroni kground events re expeted nd hek the yxEypp energy distriution t tht spei( lotionF pigure 6.16 desries the priniple of the lnk (eld nlysis nd shows the energy distriutions in wono nd tereo for lnk (eld loted t +0.8 • he from the pointElike soureF xo exess is expeted ut the vi&w signi(ne is very high X 8.8σ @ITHW exess eventsA in wono nd 4.3σ @QWR exess eventsA in tereo nd the energy distriutions show lrge exess loted elow QHH qeF yn the other hnd the θ 2 distriutions indite n overll underestimtion of the kground level in the ypp regionsF Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II 6.6 Energy range for the Full Likelihood t he hoie of the energy rnge for the pull vikelihood proedure is n importnt issue in the e0ient disrimintion of the signl nd kground hpsD s disussed in ghpter 5F pirst rnge of IHH qe Y I e hs een onsideredF his provided sfe lowEend ove the physil energy threshold of the instrument for oth wono nd tereo on(gurtions nd su0ient lever rm t high energies for the hp disrimintionF rowever this energy rnge does not provide enough lever rm under IQH qe for the potentil permi vine signl where edge e'ets re 'eting the results from the pull vikelihood (tF Optimization for a 130 GeV Line : ests with the pull vikelihood method hve een performed on wg dt smples with the wono telesope on(gurtion for PH simulted vines etween IHH qe nd PSH qe nd (xed vine signl frtion of 10% on the energy rnge IHH qe Y I eF he is @in eA on the reonstrution of the vine energy is plotted on pigure 6.17F rere systemtis oming from the method re oservedD visile in tht very nrrow energy window of simulted vines X the is on the reonstruted vine energy strts inresing signi(ntly under IQH qe euse of lrge frtion of the vine events out of the rnge due to the energy resolution e'etsF sn onsequeneD the lowEend of the energy rnge ws extended down to VH qeF Range for the complete Line scan in energy : prom the energy distriutions of the vine n R dtset @see pigure 6.14A we see tht few gmm events re reonstruted ove I e with rFiFFFss X the hoie of I e s the highEend of the energy rnge is then ompromise for hving the lrgest lever rm in energy for the hp disrimintion nd resonle ontinment of the kground dt eventsF roweverD this hoie is optimized for the reonstrution of low energy vines nd hs to e reonsidered for lrger mssesF sn this hpter we re interested in produing results for the lrgest possile rnge of msses iFeF etween IHH qe nd P eF por this purpose it hs een deided to de(ne two seprte energy rnges for the pull vikelihood method X • [80 GeV ; 1 TeV] for Lines ≤ 500 GeV • [200 GeV ; 3 TeV] for Lines > 500 GeV his ensures lrge energy leverErm to the (t in eh se @ove nd elow the position of the potentil vine fetureAD nd gets rid of the low energy is reported in setion 6.5.4 y exluding the energy region `PHH qe when onsidering msses ove SHH qeF Conclusions : Choice of the control sample for the background PDF e hve investigted Q ontrol smples for the genertion of the kground hp for the pull vikelihood method X wg simultionsD ypp regions round u PISSEQHR nd ypp regions round the permi rotspotF he xf level is the dominnt riterion for getting relisti energy threshold with wg dt in greement with the energy threshold oserved in the permi rotspot regionD ut is not su0ient explntionF e will lso show in 6.10 tht the error on the kground hp energy threshold is the dominnt systemtis in the pull vikelihood proedureD whih shows the importne of hving more relisti simultionsF his is foreseen in ner future with the development of runEwise simultions tht will e produed for eh individul oservtion runF et present omintion of relisti xf level nd relisti zimuth ngle is lso not su0ient to reprodue tht energy thresholdF pinlly the wg kground hp shpe is lso not omptile with the vine n dt t energies ove PHH qeF For all those reasons we concluded that the MC background PDF cannot be used as a realistic background PDF for the Line search studiesF st is lso unrelisti to use u PISSEQHR s ontrol smple sine the verge xf level is only TH wrz in this region @while IPS wrz t the permi rotspotA nd it would e di0ult to pply proper orretions in the kground hp to ompenste tht e'etF woreover the u PISSEQHR ontrol smple doesn9t inlude ny glti di'use emission omponent then wg di'use events should e dded on top of the hdroni kground dt events for produing relisti kground hpF por those resons we lso exluded the use of hp reonstruted from the u PISSEQHR ontrol smpleF In consequence the best choice for the background PDF is to consider background regions around the Fermi Hotspot. feuse the FyFsF nd the kground regions re de(ned in the sme py the xf level nd the zimuth ngles re in good ordneD nd the hp doesn9t require ny orretionsF king ypp regions round the permi rotspot hs the dvntge of prtilly hndling the di'use omponent in the kground hpF ystemti unertinties relted to the di'use emission omponent will e estimted in dedited setion elow @see 6.10AF

Optimization check : OFF wobble versus ON spatial side-bands sn 6.5.4 the existene of systemti is present in the dt hs een disussed whih signi(ntly 'ets the vine serhF e normliztion prolem ws pointed out etween the yx nd ypp regions tht spontneously retes n exess under PHH qe nd ontmintes the potentil ontriution from IQH qe vine signlF he kground hp for the vine n R dtset hs een studied with n ttempt for reduing this e'et X insted of ypp wole regionsD R independent nlyses of the vine n R dt pointing t the R symmetril 4yx4 positions round the permi rotspot @-1.1 • Y 0 • AD @-1.9 • Y 0 • AD @-1.5 • Y -0.8 • A nd @-1.5 • Y +0.8 • A were onsideredF he kground hp derived from the resulting event distriution @omining the R pointingsA is shown in pigure 6.23 in omprison with the hp from ypp wole regionsD in the energy rnge VH qe Y I eF he two hps re omptile within sttistil error rs nd doesn9t show ny siE gni(nt di'erenes under PHH qeF he impt on the reonstrution of vine signl Chapitre 6. Search for Dark Matter Line signatures in the Galactic Centre region with H.E.S.S.II @m χ = 130GeV Yη = 5%A hs een studied y simulting wg kground events from the (rst hp nd using the seond hp in the lultion of the pull vikelihood funtionF he e'et on the reonstrution of η is found to e < 1%F sn onsequeneD it is not possile to redue the impt of the systemti is y reonsidering the de(nition of the kground regions in the pyF he nture of the systemti is seems to e due to reonstrution prolem relted to the tretment of the eptne grdients in the gS merF Figure TFPQ ! gomprison of kground hps from the vine n R dtsetF wo senrios re onsidered X kground events from ypp wole regions round the permi rotspot @in greenA nd kground events from R yx regions round the hotspot @in lueA 6.9. DM signal leakage in the OFF regions 197 6.9 DM signal leakage in the OFF regions hue to the lrge extension of the glti hw hlo frtion of the hw signl is expeted to lek in the ypp regions @tht re used for the determintion of the kground hpAF sts mount depends on the onsidered hlo pro(leD the size of the ypp regions nd the wole o'setF por the present vine nlysis the hw signl lekge hs een lulted using hw iinsto pro(le nd single ypp region of extension θ ROI = 0.4 • o'Eentred from the hw hlo with n o'set of 1.1 • tht orresponds to the the verge wole o'set for the vine n dtF sn this on(gurtion the lekge represents PSFI7 of the vine signl events in the FyFsF gorretions re pplied on the < σv > limits presented in setions 6.12 nd 6.13F