Jacqueline D Campbell
email: jacqueline.campbell@earth.ox.ac.uk

B Schmitt

O Brissaud

J-P Muller

The Detectability Limit of Organic Molecules within Mars South Polar Laboratory Analogues

A new spectrum diagnostic of Polycyclic Aromatic Hydrocarbons (PAHs) pertinent to Mars has been produced • The detectability limit of PAHs in Mars South Pole analogues has been established • The evolution of the spectra of PAHs in Mars South Pole analogues as ice sublimates under emulated Martian conditions has been recorded

Introduction

Our neighbouring planet, Mars, has increasingly been the target of scientific exploration and of particular interest are its geological history, current environmental conditions, and perhaps most importantly, its potential as a host for extraterrestrial life [START_REF] Fairén | Astrobiology through the Ages of Mars: The Study of Terrestrial Analogues to Understand the Habitability of Mars[END_REF]. The polar caps of Mars have more recently emerged as an area of scientific interest due to their abundance of water ice and their dynamic nature, especially with the discovery of a possible stable body of liquid water beneath the Martian South Pole [START_REF] Orosei | Radar evidence of subglacial liquid water on Mars[END_REF]. The Martian North and South Pole manuscript submitted to JGR Planets have permanent ice caps that expand throughout their respective winters, and maintain residual caps in the summer. The North Polar Cap (NPC) is composed almost entirely of water ice, while the longer, colder winter in the higher altitude southern hemisphere means that the central part of the South Polar Cap (SPC) is covered by a permanent layer of CO2 ice [START_REF] Byrne | The Polar Deposits of Mars[END_REF], up to 10 metres thick, underlain, and surrounded by, water ice layers known as Polar Layered Deposits (PLD;Piqueux et al., 2008).

Seasonal cycles of sublimation and deposition of CO2 ice on the SPC are responsible for the formation of 'Swiss Cheese Terrain' (SCT). This unique cryomorphology manifests as flattopped mesas with flat floored, quasi-circular depressions that form patterns resembling Emmental Swiss Cheese [START_REF] Malin | Observational evidence for an active surface reservoir of solid carbon dioxide on Mars[END_REF]. This terrain forms by preferential and progressive sublimation and erosion of the walls of the depressions, at a typical speed of 3 metres per Mars year. The reason these SCT sublimations features are of interest to this study is because of the exposure of dust previously shielded within the SPC [START_REF] Jian | Seasonal patterns of condensation and sublimation cycles in the cryptic and non-cryptic regions of the South Pole[END_REF]. The exposed dust that has been concentrated by CO2 ice sublimation may be a candidate site for the detection of a class of organic molecules, Polycyclic Aromatic Hydrocarbons (PAHs), that may have been protected from the Sun's radiation within the SPC. If PAH is dispersed in the ice instead of being associated with the dust, it will also be concentrated at the surface with the dust as the ice sublimates away leaving any particles behind.

Work was previously carried out in order to look for PAH signatures on the thin, dust-covered rims of SCT to no avail [START_REF] Campbell | A search for polycyclic aromatic hydrocarbons over the Martian South Polar Residual Cap[END_REF] using the well-known PAH diagnostic absorption feature at 3.29 µm [START_REF] Allamandola | PAHs and Astrobiology. PAHS and the Universe[END_REF], but no signs of PAHs were found. However, this strong band is situated in the high wavelength wing of the very strong 3.1µm band of water ice and may thus be hidden in places where abundant water ice is present, such as on SPC margins (Douté et al. 2007) and rim scarps [START_REF] Campbell | A search for polycyclic aromatic hydrocarbons over the Martian South Polar Residual Cap[END_REF]. It may be also hidden by the wide hydration bands of minerals (adsorbed and structural water) that can extend up to 4 µm and may even be saturated in some cases.

The aims of the experiments carried out and reported here were to generate a diagnostic nearinfrared spectrum for PAHs of astrobiological interest in the context of the Martian South Pole.

We emulate the parameters of the CRISM instrument's Full Resolution Targeted (FRT) ~18 m/pixel mode to constrain the detectability limit of PAHs in CO2 ice to establish the characteristics of PAH spectral features at wavelengths other than the absorption feature at 3.29 µm, where they might be easier to discern against the CO2 and H2O ice spectrum. In addition, we discuss how the detectability of these bands is affected by the presence of dust.

Polycyclic Aromatic Hydrocarbons

PAHs are a group of chemical compounds consisting of benzene rings of carbon with hydrogen.

In its NPAH form, nitrogen can be substituted for carbon atoms in the aromatic ring [START_REF] Tang | PAHs/NPAHs[END_REF]. PAHs occur not only on Earth, but throughout the universe. They have been found to coalesce in space within dust clouds [START_REF] Mulas | Estimated IR and phosphorescence emission fluxes for specific Polycyclic Aromatic Hydrocarbons in the Red Rectangle[END_REF], and are thought to account for up to 20% of total cosmic carbon [START_REF] Allamandola | PAHs and Astrobiology. PAHS and the Universe[END_REF].

PAHs frozen within ice particles in dense molecular clouds in space undergo processing by ultraviolet light and cosmic rays to produce more complex species [START_REF] Dartnell | Experimental determination of photostability and fluorescence-based detection of PAHs on the Martian surface[END_REF]. PAHs manuscript submitted to JGR Planets can also arise and increase in abundance through the irradiation of complex polymeric organic material such as those found in carbonaceous meteorites [START_REF] Thompson | The effect of progressive space weathering on the organic and inorganic components of a carbonaceous chondrite[END_REF]. A recent paper on the Mukundpura carbonaceous chondrite meteorite found in India measured 500ppm PAH [START_REF] Kalpana | Polycyclic aromatic hydrocarbons in the Mukundpura (CM2) Chondrite[END_REF]. PAHs eventually rain down on primordial planets directly from planetary accretion discs, or are delivered on comets and meteorites [START_REF] Allamandola | PAHs and Astrobiology. PAHS and the Universe[END_REF].

Therefore, PAHs should be present, or should have been present in the past, on all planetary bodies in the solar system [START_REF] Dullemond | Dust sedimentation in protoplanetary disks with polycyclic aromatic hydrocarbons[END_REF]. PAHs have been detected on the surfaces of Saturnian icy moons and comets [START_REF] Cruikshank | Hydrocarbons on Saturn's satellites Iapetus and Phoebe[END_REF][START_REF] Cruikshank | Aromatic and aliphatic organic materials on Iapetus: Analysis of Cassini VIMS data[END_REF][START_REF] Lopez-Puertas | Large abundances of polycyclic aromatic hydrocarbons in Titan's upper atmosphere[END_REF][START_REF] Li | PAHs in comets: An overview[END_REF] and have been measured in other carbonaceous chondrites meteorites at the level of a few ppm [START_REF] Becker | Polycyclic aromatic hydrocarbons (PAHs) in Antarctic Martian meteorites, carbonaceous chondrites, and polar ice[END_REF].

The delivery of complex organic compounds to planets via bolide impact is a very important concept in astrobiology, and could be instrumental in explaining abiogenesis (the origin of life).

Carbon's propensity to catenate (form long chains), and the carbon-based nature of all life on Earth, means that the presence of carbon compounds is considered an essential component of any potentially habitable environment [START_REF] Plaxco | Astrobiology: A Brief Introduction[END_REF]. PAHs are sought after on many solar system bodies in the search for the origin of life, but are conspicuously missing on Mars [START_REF] Benner | The missing organic molecules on Mars[END_REF]. The discovery of PAHs on Mars would tell us that these organics could survive in oxidizing environments receiving high levels of UV radiation, and may have accumulated in the past when Mars had warmer and wetter conditions favourable to the emergence of life.

PAHs on Mars

The detection of organics has been a primary objective of orbiters and landers since the Viking missions [START_REF] Klein | The Viking biological experiments on Mars[END_REF]. Despite apparent negative results for the detection of extant life by the Viking landers in the 1970s, which searched for traces of biologically important compounds [START_REF] Klein | The Viking biological experiments on Mars[END_REF][START_REF] Schuerger | Viking biology experiments; Lessons learned and the role of ecology in future life-detection experiments[END_REF], perchlorates were discovered by the 2008 Phoenix lander [START_REF] Hecht | Detection of perchlorate and the soluble chemistry of Martian soil at the Phoenix lander site[END_REF]. More recently, organics were discovered by the Sample Analysis at Mars (SAM) instrument on NASA's 2012 rover mission, Mars Science Laboratory [START_REF] Freissinet | Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars[END_REF], known as "Curiosity". Perhaps of even more interest, is the re-analysis of the 1976 Viking Lander data by Navarro-Gonzalez et al. (2010) using modern laboratory techniques suggested that there were both perchlorates and organic carbon present at the Viking Lander sample sites, although they were not identified at the time. To date, no PAHs have been found on Mars, but concentrations of about 1ppm of PAH have been found in Martian meteorites with potential extraterrestrial origin [START_REF] Mckay | Search for past life on Mars: Possible relic biogenic activity in martian meteorite ALH84001[END_REF][START_REF] Becker | Polycyclic aromatic hydrocarbons (PAHs) in Antarctic Martian meteorites, carbonaceous chondrites, and polar ice[END_REF][START_REF] Botta | Extraterrestrial organic compounds in meteorites[END_REF].

A study by [START_REF] Dartnell | Experimental determination of photostability and fluorescence-based detection of PAHs on the Martian surface[END_REF] found that PAHs might be afforded protection from the effects of UV radiation and oxidization within the subsurface of Mars, within rock, or in permanently shadowed areas. Ice can also provide a barrier to deep UV solar radiation [START_REF] Vincent | Transparency of Antarctic ice-covered lakes to solar UV radiation[END_REF] manuscript submitted to JGR Planets [START_REF] Cockell | The ultraviolet environment of Mars: Biological Implications past, present and future[END_REF], resulting in partial shielding and allowing organic compounds to become more complex [START_REF] Herbst | Complex Organic Interstellar Molecules[END_REF][START_REF] Oberg | Formation rates of complex organics in UV irradiated CH3OH-rich ices[END_REF].

Laboratory Analysis

Instruments

Laboratory Analysis

The site of the experiments was the Cold Surfaces Spectroscopy Facility (https://coldspectro.sshade.eu) at the Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) in France and has facilities for in-situ formation of ices, and cold rooms capable of keeping samples up to -40°C to allow stable thermal conditions during preparation of icy materials for experiments. This allows analysis of samples in the cryogenic CarboN-IR environmental cell, which can maintain cold temperatures and low gas pressures, using the SHINE (SpectropHotometer with variable INcidence and Emergence) instrument to record reflectance spectra in visible and near-mid infrared wavelengths.

Spectro-gonio radiometer

The SHINE spectro-gonio radiometer was developed at IPAG, and is designed to measure bidirectional reflectance and polarisation distribution functions of planetary material, enabling the production of accurate datasets to help describe surface composition, roughness and texture [START_REF] Brissaud | Spectrogonio radiometer for the study of the bidirectional reflectance and polarization functions of planetary surfaces[END_REF]. In particular, the SHINE spectro-gonio radiometer is able to characterise the light scattering properties of snows of various grain-size, compactness and surface roughness at different stages of metamorphism. The instrument is able to measure from 0.35-4.80 μm, with spectral resolution of between 6-40 nm, dependent on wavelength (ibid). SHINE can be used in conjunction with the CarboN-IR environmental cell to analyse materials at low temperatures.

CarboN-IR Environmental Cell

The CarboN-IR environmental cell system (https://cold-spectro.sshade.eu/carbo-nir-simulationchamber) allows for the study of planetary material samples in stable conditions. It can cool the sample down to -210°C within an isothermal copper cell that can maintain a stable gas pressure in thermodynamic equilibrium with the sample at the same temperature. The chamber is designed to enable visible and near-IR monitoring throughout the physical evolution of ice samples thanks to sapphire windows (Grisolle 2013).

Methods

The concept of this work is to produce empirical experimental data to support the interpretation of data from orbital observations of the Martian SPC, namely the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on board NASA's Mars Reconnaissance Orbiter manuscript submitted to JGR Planets (MRO), which has a surface spatial resolution of around ~18m/pixel [START_REF] Murchie | Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO)[END_REF], with a spectral resolution of ~6 nm.

Instrument parameters

The CRISM instrument has a resolution, of 9-19 nm full width at half maximum (FWHM) with 6.55 nm sampling over the 0.36-3.92 µm range [START_REF] Murchie | Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO)[END_REF] In order to get a spectral resolution as close as possible to CRISM, we recorded spectra over the 0.7-3.6 µm spectral range using SHINE with a fixed slit of 1.5 mm, leading to 9-19 nm spectral resolution, and sampled every 10 nm (except for the first experiment sampled at 20 nm). To complete a full reflectance spectrum at this resolution took > 2.5 hours, so in order to effectively reduce the time between two spectra, especially during ice sublimation, in many instances multiple shorter spectra at wavelengths of interest were taken. The SHINE angular parameters used were fixed incidence angle = 0°, and observation angle = 20°, optimized for the CarboN-IR cell. This is comparable with a median phase angle of 0-30° for CRISM [START_REF] Ceamanos | Surface reflectance of Mars observed by CRISM/MRO: 1. Multi-angle Approach for Retrieval of Surface Reflectance from CRISM observations (MARS-ReCO)[END_REF].

Sample Preparation

Three samples were analysed for various ratios of PAHs mixed with CO2 ice and two with finely ground Martian simulant JSC-Mars 1 [START_REF] Allen | Martian Regolith Simulant JSC Mars-1[END_REF]. Much of the existing literature on PAHs found on icy moons and comets references the laboratory spectra recorded by [START_REF] Colangeli | Raman and infrared spectra of polycyclic aromatic hydrocarbon molecules of possible astrophysical interest[END_REF], which is pertinent to PAHs of astrophysical interest, rather than astrobiological, or specifically Martian. The six PAH species analysed by [START_REF] Colangeli | Raman and infrared spectra of polycyclic aromatic hydrocarbon molecules of possible astrophysical interest[END_REF] were benzene, chrysene, triphenylene, perylene, benzo [a] pyrene, pentacene and coronene. While chrysene and perylene have been found in Martian meteorites [START_REF] Becker | Polycyclic aromatic hydrocarbons (PAHs) in Antarctic Martian meteorites, carbonaceous chondrites, and polar ice[END_REF] and phenanthrene, pyrene, chrysene, perylene or benzopyrene and anthanthracene were found by [START_REF] Mckay | Search for past life on Mars: Possible relic biogenic activity in martian meteorite ALH84001[END_REF] the remaining four types of PAH have never been detected in Martian material. Therefore, we analysed our own mixture of PAHs based on those identified by [START_REF] Mckay | Search for past life on Mars: Possible relic biogenic activity in martian meteorite ALH84001[END_REF] in the ALH84001 and EETA79001 Martian meteorites but absent from Colangeli's analysis. The PAHs used were an existing mixture of anthracene (C14H10), phenanthrene-d10 (C14D10), and pyrene (C16H10) in raw form, obtained from Sigma-Aldrich (www.sigmaaldrich.com), in a 300 mg sample of equal parts of each PAH species. We will not discuss in this paper the bands due to or modified by the deuterated species as they do not contribute to PAH spectral features of interest.

In studies of Saturnian moons Iapetus and Phoebe [START_REF] Cruikshank | Hydrocarbons on Saturn's satellites Iapetus and Phoebe[END_REF], the amount of PAHs detected on the surface was 10 -4 to 10 -3 g/cm 3 (0.01-0.1 %) so the first sample used 0.10 % PAH followed by 0.54 % and 0.67 % weight fractions for our three PAH samples mixed with CO2 ice in order to allow the detection limit to be determined by plotting band depth as a function of concentration. The percentage amounts of PAH in CO2 ice were difficult to fix precisely because some CO2 ice sublimated during the process of mixing the materials, but they were precisely measured when the sample holder was filled with the prepared mixture, just before their introduction into the cell (see below). Increases in the amount of PAH for Samples 2 and 3 were chosen based on how well we could see the PAH features in Sample 1.

CO2 ice was obtained from liquid decompression with a commercial device SnowPack©. This produces a granular snowpack of 312.5 cm 3 composed of small CO2 ice grains. The average size of the grains, 150 μm, was estimated by measuring the true surface of the grains observed with a manuscript submitted to JGR Planets binocular microscope [START_REF]Microphysique des processus saisonniers des glaces de Mars et Pluton : suivi par télédétection hyperspectrale et étude expérimentale[END_REF]. Part of the CO2 ice snow pack was then manually crushed, weighed, and a known mass of PAH powder was added and thoroughly mixed in a stainless-steel container pre-cooled with liquid nitrogen to limit CO2 ice sublimation. The cell, also pre-cooled at -196°C, was filled up to its rim with the mixture (slightly compressed) and weighed before rapid installation inside the pre-cooled CarboN-IR environment chamber (-100 °C). The Martian South Pole's lowest temperatures can reach -153 °C and never exceeds -60 °C with the spring/summer temperatures for the SPC typically ranging between -80 and -100 °C [START_REF] Smith | Interannual variability in TES atmospheric observations of Mars during 1999-2003[END_REF]; hence the choice to keep the environmental cell at the lower spring/summer temperature. The sapphire windows of the cryogenic chamber and of the external chamber were then successively closed and air was completely evacuated from both volumes by pumping using a detailed protocol developed to avoid frost condensation on the windows.

The grain sizes of our CO2 ice samples are much smaller than what is generally observed on Mars South Polar Cap where CO2 ice tends to have very coarse centimeter sized grains, generally in the form of compact slab [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF]). However, a major decrease in grain size, down to the millimeter, occurs after equinox [START_REF] Langevin | Observations of the south seasonal cap of Mars during recession in 2004-2006 by the OMEGA visible/near-infrared imaging spectrometer on board Mars Express[END_REF]) and corresponds to the large increase of albedo oberved over the perennial cap during its sublimation phase. The grains in our samples are typically 5-10 times smaller than during the polar cap sublimation phase of interest.

However, preparing such coarse grained CO2 ice grains is a quite complex process and takes several weeks and was not possible given the experimental constraints [START_REF]Microphysique des processus saisonniers des glaces de Mars et Pluton : suivi par télédétection hyperspectrale et étude expérimentale[END_REF]. But, as we will discuss later, using smaller grains may put stronger or weaker constraints on the detectability of PAHs, depending where their bands are situated relative to the CO2 ice bands.

In addition, we measured one mixture of 1.5% PAH combined with a fine fraction (<25µm) of JSC-Mars 1 Mars simulant as well as this dust alone, as a reference.

The sample holder is 4.5 cm in diameter and 2 cm deep and has a total volume of 31.8 cm 3 .

Knowing the mass of the sample, measured just after filling the holder, and the density of bulk CO2 ice (1.562 g.cm -3 ) allowed to estimate the initial density and porosity of the sample, which is simply the fraction of the volume of the sample holder not occupied by CO2 ice.

The percentage of H2O ice mixed in the CO2 snow was estimated (with uncertainty +/-20%) by comparison of its 1.5 µm band depth with that of the nearby CO2 bands (at 1.435 and 1.58 µm) and relative to the spectra of a series of CO2:H2O ice mixtures previously measured and modelled (Philippe 2016). The mass fraction of H2O ice in our samples is mostly of the order of the maximum values determined for the South Polar Cap, 0.08-0.12% [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF]) except in one case (~0.20%) where it exceeds these limits.

Experiment Protocol

After introduction of the sample holder containing the PAH-CO2 ice mixture into the CarboN-IR cell and throughout the experiments, the cell and sample holder temperatures were kept at -100°C. Following initial measurements of the samples, sublimation experiments were conducted by pumping the CO2 gas into the cell to monitor spectral and detection limit changes with sublimation. Bidirectional reflectance spectra (at single geometry) on both full Vis-NIR and manuscript submitted to JGR Planets partial spectral ranges were recorded regularly during the sublimation experiment to reflect regions of interest for later comparison to observational results from orbital sensors.

Results

Preliminary Measurements

A first guess of the detectability limit for PAHs in CO2 ice was established with reference to levels detected on other planetary bodies such as Iapetus, 10 -4 to 10 -3 g/cm 3 [START_REF] Cruikshank | Hydrocarbons on Saturn's satellites Iapetus and Phoebe[END_REF]. This was then tested at room temperature with a ~1% mix of PAH mixture with a transparent powder (alumine) in order to estimate the minimum amount of PAH required for detection within CO2 ice but outside its absorption bands. From this preliminary experiment, an approximate detection limit of about 0.1% by weight was determined. This experiment also allowed us to define spectral ranges and resolution needed to detect the PAH mixture without interference from CO2 ice spectra.

A spectrum of the 'pure' PAH mixture was also measured between 0.4 and 4.7 µm (at 20 nm sampling) as a reference (grey line in Figure 1). The positions and intensities of the bands are consistent with the reflectance spectra measured at higher spectral resolution up to 2.5 µm for our three PAHs by [START_REF] Izawa | Reflectance spectroscopy (350-2500 nm) of solid-state polycyclic aromatic hydrocarbons (PAHs)[END_REF], except the 2.24 µm band which is much stronger in our PAH mixture spectrum.

Table 1 shows the details of the three CO2 ice samples discussed in the subsequent sections. For the first PAH+CO2 ice sample, an amount of PAH comparable to our pre-estimated detection limit, 0.1%, was used. During this experiment the speed with which the interior chamber was pumped out from the ambient air resulted in water frost particles condensing on the surface of the sample being blown onto the inside of the window, and could not be removed (in the subsequent experiments this was done more slowly and with additional heating of the window to manuscript submitted to JGR Planets avoid this problem) meaning that water contamination at the surface of CO2 ice may be stronger in sample 1.

Two spectra were obtained from 0.4-3.6 µm with spectral sampling of 20 nm. As the vacuum was very stable, to aid sublimation, a lamp was used to heat the sample surface, at 27 cm distance from the window, resulting in 70W/m 2 equivalent to Mars at noon at 70° lat, achieving a sample sublimation of ~3 mm between two spectra. Upon examination of these spectra it was clear that the PAH feature at 3.29 µm is not observed on the side of the strong and broad 3.1 µm water ice band (the small shoulder at 3.32 µm is due to CO2 ice), and so the following spectra were taken only between 0.6 and 2.0 µm at 20 nm sampling. Fig. 1 shows the results.

manuscript submitted to JGR Planets It is clear over time, the overall reflectance of the spectra (PAH1a-1g) decreases as the CO2 ice sublimates, and the slope increases between 0.7 and 1.1 µm. This is likely to be associated with the steep slope in the corresponding pure PAH mixture spectrum (black line) as sublimation increased the ratio of PAH/CO2 ice and probably concentrated the PAH at the surface of the sample. We also notice that the water ice feature dominating around 1.52µm increases with sublimation, as the tiny frost particles present at very low level (~0.12%) in CO2 ice are also segregated at the surface during sample sublimation [START_REF]Microphysique des processus saisonniers des glaces de Mars et Pluton : suivi par télédétection hyperspectrale et étude expérimentale[END_REF]. A subtle absorption feature with a band depth of about 0.6% is visible in the PAH 1a-1g series of spectra corresponding with the pure PAH feature at 1.14 µm, with another weak feature visible at 1.68 µm (band depth ~ 1%). This latter band strongly increases in intensity during CO2 sublimation and reaches an estimated depth of about 3% in the remaining PAH-H2O ice lag deposit, but at this spectral sampling it is difficult to separate it from the 1.645µm band of H2O ice. It would seem that the initial 0.10% PAH/CO2 ice ratio is actually close to the detectability limit at this spectral resolution and sampling, and subsequent experiments used a higher initial ratio and a two times better spectral sampling to confirm the detection of the PAH bands.

4.3. PAH/CO2 = 0.67% -Sample 2

For this second experiment, more care was taken to limit frost condensation at the surface of the CO2 ice sample during transfer to the CarboN-IR cell and the ambient air was pumped more slowly to avoid window condensation or frost particles blown on it, but this was not successful as the water ice bands are about 2 times more intense than in Sample 1 with an estimated amount of H2O ice of about 0.2%.

A higher spectral sampling, 10 nm, was used, meaning it took longer to obtain spectra, so a spectral range of 0.7-2.2 µm was chosen to obtain multiple spectra to observe the evolution of the features at 1.14 and 1.685 µm for the first 4 spectra (PAH2a-PAH2d) during the sublimating sequence. This limitation of the spectral range did not limit this study as CRISM spectra below 2.5 µm are the most useful for this work due to the interference of strong atmospheric water and ices features at 2.7-3.3 µm on Mars and because only the lower wavelength PAH features are detected against a background of CO2 ice. There was a small leak in the cell, increasing sublimation rate, so the lamp was not used for sample 2 to reduce the sublimation rate of CO2.

The spectral range was then increased to 0.7-2.75 µm and left to run overnight, resulting in total of 6 spectra, shown in Fig. 2.

manuscript submitted to JGR Planets With the increased amount of PAH in the ice, the absorption features at 1.14 and 1.685 µm (band depths of 2% and 7% in the mixture, respectively) are now clearly visible throughout all PAH/CO2 ice spectra, as well as the slope at 0.7-1.1 µm. In the extended spectra PAH2e-PAH2p, there are also corresponding features visible at 2.15, 2.24, 2.29, 2.33, 2.41, 2.49 and 2.62 µm in pure PAH and PAH/CO2 ice spectra. It is also clear that with the increased initial amount of H2O ice in this sample (~0.2%, instead of ~0.12% in Sample 1) the CO2 ice absorption feature at 1.435 µm and its triplet features around 2 µm become more rapidly dominated by the strong and broad 1.5 and 2 µm absorption bands of water ice, as CO2 ice sublimates. When all the CO2 ice has sublimated, leaving only a thin deposit (~170 µm) of water ice-dust mixture, the intensity of both the 1.14 and 1.685 µm bands have increased by about 70%, and then started to decrease slowly while the H2O ice band was stable.

4.4. PAH/CO2 = 0.54% -Sample 3

For this experiment a spectral range of 0.4 -2.75 µm was chosen with resolution of 10nm. Details of sample 3 are shown in table 1. This time with an improved preparation protocol we succeeded in efficiently suppressing any additional condensation of frost at the surface of the CO2 ice, and the water ice content (0.08%) is now similar to what was previously achieved for pure CO2 ice, as witnessed by the almost identical ratio between the 1.52 µm band of H2O and 1.435 µm band of CO2 ice in the initial spectrum 3a (Figure 3).

Sixteen spectra were taken throughout the day and overnight during the sublimation sequence.

As with experiment 1, the vacuum was very stable, and slow sublimation occurred, resulting in fairly homogenous spectra. Results are shown in Fig. 3.

manuscript submitted to JGR Planets With 0.54% PAH, the features at 1.14, 1.685, 2.15, 2.24, 2.41, 2.49 and 2.62 µm are visible as with sample 2. With these higher signal-to-noise spectra, it is also possible to better observe the replicated PAH features at 2.29 and 2.33µm, with the PAH/CO2 ice mixture between 2.1 and 2.5µm closely mirroring the shape of the spectrum for pure PAH mixture. The change in the slope at 0.7-1.1 µm is also clear but unfortunately was not monitored until the end of the experiment. Again as with Sample 2, the CO2 ice absorption feature at 1.435 µm becomes muted with sublimation, but the triplet feature at ~2 µm is less affected in the first stages of sublimation with an initial 'contamination' of only 0.08% water ice, as was the case with the small amount of H2O ice in Sample 1. During CO2 sublimation, the intensity of the 1.14 µm band increased by about 50%, and that of the 1.685 µm by a factor of 2.3 when only a H2O ice-dust sublimation residue remained at the bottom of the sample holder (only about 120 µm thick). Other bands, such as those of 1.155 µm and 2.49 µm, increased by an even greater proportion.

4.5. PAH/dust = 1.52% and dust -Samples 4 and 5

A final experiment, with two spectra ranging from 0.4-3.9 µm at a resolution of 10nm, was taken of the PAH mixture in Mars simulant JSC Mars-1, weathered volcanic ash from Hawaii [START_REF] Allen | Martian Regolith Simulant JSC Mars-1[END_REF], as well as a pure dust spectrum for reference (Figure 4). The JSC Mars-1 regolith simulant was previously ground and sieved below 25 µm to simulate Martian atmospheric dust.

Sample details are shown in Table 2. Despite PAH particles being clearly visible in the physical sample, and the ratio of PAH to substrate being 2.5 to 3 times higher than in ice samples 2 and 3, (1.52% compared to 0.67% and 0.54%), no spectral features of PAHs were detectable in the dust spectrum.

Other than the pure dust sample being slightly lower in overall reflectance, there is no observable difference in spectra between pure dust and PAH/dust mix. This is most likely because of the relative opacity of dust compared with CO2 ice, its continuum reflectance being three times lower. If PAHs are not discernible in Martian dust at concentrations an order of magnitude higher than that detected on Iapetus, it is likely to be an extremely limiting factor in detecting PAHs on the SPRC if any potential PAHs are mixed with dust and not in pure form. No known segregation process can concentrate PAH in dust as is the case with PAH/CO2 ice mixtures. In order to ascertain whether PAHs in small amounts of dust are detectable when mixed in CO2 ice, further experiments will need to be carried out to better emulate the scarp wall dust deposits in SCT. However, with our current set of experiments, it is already possible to make some manuscript submitted to JGR Planets extrapolations on the detectability of PAH in materials with different compositions encountered on the South polar cap and in the water ice-dust lag deposits at its margins.

Discussion

The results of these novel experiments are extremely useful to allow a future new analysis of orbital observations from the CRISM instrument on Mars Reconnaissance Orbiter, and establish a detection limit for PAHs in CO2 ice and in H2O ice-dust lag deposits, not only at the poles, but in shadowed regions elsewhere, in sub-surface ice that may be sampled during future exploration missions as well as on icy bodies. In addition, we ascertained the limitations of observing PAHs directly in 'dry' Martian regolith, a first step towards establishing the detectabililty of PAH in the regolith of other planets. This study also provides more relevant bi-directional reflectance data in the near-infrared range on diagnostic PAH signatures of astrobiological importance to Mars, that are pertinent to planetary ices, as most previous literature, except [START_REF] Izawa | Reflectance spectroscopy (350-2500 nm) of solid-state polycyclic aromatic hydrocarbons (PAHs)[END_REF], used midinfrared transmission data from the 1990s which is more relevant to interstellar dust cloud PAH detection.

PAHs are extrememly important to theories of abiogenesis, and while their presence is ubiquitous in space, their detection on planetary bodies remains a major objective in planetary science. The attempt to detect them on Mars is worthwhile given the recent discoveries of other organic compounds and subterranean lakes [START_REF] Freissinet | Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars[END_REF][START_REF] Ojha | Spectral evidence for hydrated salts in recurring slope lineae on Mars[END_REF][START_REF] Orosei | Radar evidence of subglacial liquid water on Mars[END_REF].

In the spectrum of our mixture of three PAHs the strong 1.685 µm band is the first overtone (2νCH) of the fundamental aromatic symmetric C-H stretch modes (νCH) occurring at ~3.29 µm.

From the position of these two bands, we deduce that the 1.14 µm band is the second overtone (3νCH) of these modes, and the weak band at 0.88 µm is the third overtone (4νCH) [START_REF] Izawa | Reflectance spectroscopy (350-2500 nm) of solid-state polycyclic aromatic hydrocarbons (PAHs)[END_REF]. The other bands between 2.1 and 2.9 µm are mostly combination bands between these stretching modes and various types of aromatic C=C deformation modes and C-H stretching and bending modes. Due to the use of phenanthrene-d10 in our sample there are also additional bands at 2.24 and 1.50 µm due to the first and second overtone of the fundamental C-D stretch modes.

Weaker bands between 1.30 and 1.55µm are higher order combinations [START_REF] Izawa | Reflectance spectroscopy (350-2500 nm) of solid-state polycyclic aromatic hydrocarbons (PAHs)[END_REF]. In our discussion we will only consider the 1.14 and 2.685 µm C-H stretch overtone bands.

Detectiability of PAH in CO2 ice

We have shown that the most interesting and sensitive signature of PAH for detection on the Mars residual CO2 ice cap is this 2νCH band at 1.685 µm, well outside the CO2 ice bands and the strongest H2O ice bands (Figure 6). The only band that can slightly interfere with this PAH band is the 1.645 µm band of water ice, which is seen in our spectra as a weak shoulder on the low wavelength side of the PAH band (see e.g. Figure 2). However, it is shifted to lower wavelengths by 0.04 µm, well above the resolution of all current and future near-infrared spectrometers. We found that even with more than 0.1% water in CO2 ice, which is rarely the case in the very dry southern hemisphere [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF] found 0.02-0.12% H2O in CO2 ice), this ice band did not preclude the detection of PAH homogeneously mixed at levels below 0.1% in CO2 ice. In order to better assess the detectability level of this band and the 1.14 µm one for PAH homogeneously mixed with CO2 ice (before any sublimation), we have plotted in Figure 5 the initial relative band depth of both bands versus the mass fraction of PAH containing C-H bonds (removing phenanthrene-d10 which did not contribute to these bands). Assuming the pre-flight SNR value of 450-500 around 1.14 and 1.68µm given for CRISM (Murchie et al., 2007, Fig. 33b), the detection level of these bands in an observed spectrum with reflectance close to 1 (as for CO2 ice) is for a band depth of 0.6% relative to the nearby continuum (i.e. for a 3σ detection level, horizontal dotted line in figure 5). The detectability of the 1.685 µm band of PAH well mixed in fine grained CO2 ice (D ~150 µm) is thus at about 0.04% PAH weight fraction, and that of the 1.14 µm at about 0.13%. The detection level for the 1.685 µm band should be only slightly affected at the lower temperature of the SPC (~-150°C), whereas the 1.645 µm H2O band gets stronger and shifts slightly towards the PAH band (see Fig 2 of [START_REF] Grundy | NIR Optical constants spectrum of H2O Ih crystal and H2O liquid from 20 to 293 K. SSHADE/GhoSST[END_REF]1998). The 1.14 µm band is weaker but, on the other hand, absorbs at a wavelength without CO2 absorption and between two much weaker water ice bands.

The slope between 0.7 and 1.1 µm, and the absorption features in the 2.1-2.5 µm range may also provide additional clues to confirm detection. The visible slope of PAH occurs in a range of full transparency of both ices, but it cannot be used as a detection criteria as it may be confused with the slope induced by a small amount of contaminating reddish dust. The bands between 2.1 and 2.5 µm are also mostly outside any strong CO2 absorption and are clearly observed in most of our spectra, down to a PAH abundance at 0.1% level, despite a larger abundance of H2O ice in our samples compared to the Mars South Polar Cap. However, the two generally weak CO2 ice manuscript submitted to JGR Planets bands at 2.295 and 2.35 µm may become much stronger in some situations (larger grain size, see e.g. [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF][START_REF] Langevin | Observations of the south seasonal cap of Mars during recession in 2004-2006 by the OMEGA visible/near-infrared imaging spectrometer on board Mars Express[END_REF]) and strongly interfere with this set of PAH bands.

On the other hand, the 'classical' strong 3.29 µm fundamental band of PAH interferes with the relatively strong 3.32 µm band of CO2 ice but is also buried in the wing of the strong water ice band at 3.1 µm which can saturate even with a very small amount (<< 0.1%) of H2O trapped in CO2 ice (see e.g. Figure 1). Similarly, when mixed with martian soil this band falls in the wing of the very strong band of both structural and adsorbed H2O. This 3.29 µm band thus cannot be used to detect PAH in reflectance spectra of icy surfaces.

An important point to consider here is the difference in CO2 ice grain sizes between our samples (~150 µm) and the perennial cap: from several centimetres (clear compact slab) decreasing down to a few millimeters during sublimation in spring (Langevin et al. 2006, Douté et al. 2007).

Larger grains increase the intensity of the CO2 absorption bands and can efficiently hide any other signatures there on in their wings, but on the other hand, such large grains allow light to penetrate and probe much deeper in the wavelength ranges outside the relatively narrow CO2 bands. In particular, the 1.685 µm PAH band is situated at a wavelength where the absorption coefficient of CO2 is extremely low (< 3 10 -4 cm -1 ; [START_REF] Quirico | Near-IR optical constants of crystalline CO2 ice at 179 K completed with 28K data[END_REF]Schmitt 2004, Hansen 2005). So it is anticipated from radiative transfer considerations that the detection level of this PAH band should be largely improved in such coarse grained or slab ice, possibly down to the 0.01% level.

The main limitation will come from the abundance of water ice which has an absorption coefficient around 10 cm -1 at 1.685 µm (in the wing of the 1.645 µm H2O band) for pure ice [START_REF] Grundy | NIR Optical constants spectrum of H2O Ih crystal and H2O liquid from 20 to 293 K. SSHADE/GhoSST[END_REF]1998), i.e. about 4 orders of magnitude above that of CO2 ice. A water ice abundance above a few percent should preclude the detection of trace amounts of PAH at this wavelength. On the other hand the 1.14 µm band is situated at a wavelength of minimum absorption of H2O ice (~ 5 10 -2 cm -1 ) and may be a better probe where H2O ice is moderately abundant.

Also, as CO2 ice sublimates, the PAH contained in the sublimated layers segregates at its surface together with H2O ice and its band depth progressively increases by a factor which depends on the initial amount of H2O ice. This increase is only by a factor of 1.55 when the H2O/CO2 ratio is large, as for sample 2 (0.20%), but can reach a factor of 2.3 when this ratio is small, as for sample 3 (0.08%). So the 'visibility' of PAH is increased by the CO2 sublimation only until a mix of PAH and H2O ice remains. On Mars the accumulation factor of PAH at the surface (at the same initial concentration) will be larger as the thickness of sublimated CO2 is more than an order of magnitude larger than for our sample (2 cm).

Detectability in the PAH-H2O ice lag deposit

Another important result is that for all our samples, the PAH bands are still observed in the H2O-PAH mixture left over after complete sublimation of the CO2 ice, and with an increased intensity despite the relatively high initial content in H2O ice (0.08-0.20%) relative to the Mars South Polar Cap. Our three resulting sublimation lag deposits have H2O/PAH ratios ranging from 15 to 120% (see Table 1) and display very clear and strong PAH bands at all wavelengths for Samples 2 and 3 (Figures 2 and3). Even for Sample 1, where H2O ice dominates the composition of the manuscript submitted to JGR Planets mixture, the 1.685 µm is easily detectable, although blended with the 1.645 µm H2O band (but the sampling was only 20 nm for this sample) which now has a similar intensity (see the blue curve in figure 1). Its relative band depth is about 3%. So PAH may still be detectable in the lag deposit, as a shoulder ~1% deep on the side of the 1.645 µm band, if the initial weight abundance of PAH relative to H2O ice is more than about 25% (~3 times less than for Sample 1). Given the average concentration of 0.02-0.04% for H2O ice in CO2 ice determined for the dry ice-rich terrains [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF]) at Ls~140°, we can still expect to be able to detect PAH mixed with pure H2O ice in the sublimation lag deposit when PAH is present in the initial CO2 ice down to a concentration as low as 0.005-0.01%.

In our experiment, we did not find a good correlation between the PAH band depths and the PAH/H2O ice weight ratio, but rather some correlation with the PAH mass column in the sample (Figure 6). This is probably due to the fact that this lag deposit is very thin (65-170 µm, assuming a porosity of 50%) and thus probably still optically thin in these bands. In our experiments a mass column of 0.3 mg/cm 2 may be derived as the 0.6% band depth detection level (for CRISM SNR, see 5.1) for PAH in PAH-H2O mixtures. However, for optically thick water ice deposits, as on Mars, this may be underestimated. These estimates call for future experiments to measure the actual level of detectability of PAH mixed with water ice.

Effect of dust on the detectability of PAH

As we already saw with our single experiment of PAH-dust mixture, the limitation on the detectability of PAH is also strongly constrained by the amount of dust present in the ice. Indeed the martian dust aerosol particles that are mixed with CO2 ice have strong absorption coefficients over all the near infrared range (in the range 30-120 cm -1 @ 1.14 µm, 50-180 cm -1 @ 1.685 µm manuscript submitted to JGR Planets and increasingly larger above; [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF], so one to three orders of magnitude larger than for H2O ice and four to six orders larger than for CO2 ice at the wavelengths of these PAH absorptions. Furthermore, aeolian dust has a much smaller grain size (<10 µm) and therefore, in addition to strongly absorbing light, it will scatter it efficiently and reduce the probed depth. The non-detection of 1.5% PAH in a fine fraction (< 25 µm) of JSCMars-1 analogue is most likely an underestimate of the detection limit of PAHs in dust.

On Mars a small amount of dust is mixed with CO2 ice on the South Polar Cap. Its concentration has been estimated in the 0.02-0.14% range with a dust/H2O ratio ranging between 0.5 and 4 in the CO2 ice-rich terrains [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF]). These authors also derived very similar dust/H2O ratios for the water ice-rich terrains on the margins of the cap, as expected after sublimation of the CO2 ice.

Considering the similarity in absorption coefficient between dust and the strong absorption peak at 2µm of H2O ice (~100 cm -1 ), a high abundance of dust (~0.14%) mixed with CO2 ice will certainly cancel the positive effect of larger CO2 grain size and limit the detectability of PAH to a higher level than our measured value of 0.06%, possibly closer to 1%. The reflectance of such types of dusty CO2 ice is only slightly larger (by ~30%) than for the surrounding 'dry' terrains [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF]. So penetration of light is already quite limited. But if dust is present in lower amounts (~0.02-0.04%, reflectance almost twice that of dust) the penetration depth of light in slab CO2 ice should allow a lower detection limit for PAHs.

In the PAH-H2O-dust sublimation lag deposit a similar degradation of the detection level should occur depending on the dust/ H2O ratio. If it is at its lower limit (~0.3) the effect should be mostly to reduce the reflectance in the continuum absorption and thus reduce the detectability of the 1.14 µm band and significantly affect the visible slope, but this will only partly reduce the relative band depth of the 1.685 µm band. For higher concentrations of dust relative to both CO2 and H2O ice, its effect is likely to strongly reduce the detection level of PAH, possibly up to ~1% for the largest observed dust/H2O ratio ~4 [START_REF] Douté | South pole of Mars: Nature and composition of the icy terrains from Mars Express OMEGA observations[END_REF].

All these results and rough estimates based on relative values of absorption coefficients call for experiments to directly measure the detectability of PAHs in mixtures of PAH/dust/H2O ice dispersed in small amounts in slab CO2 ice and as sublimation lags in order to better assess both the boosting effect of large CO2 grain size and the deleterious effects of dust. Radiative transfer models may also help us to understand the detection limits both in experiments and in observations.

Extrapolation to other PAHs

Another important question now arises about the wider applicability of our experiments with a selection of only three of the simplest PAHs in comparison to other more complex molecules in this family. being generally dominant (100% in anthracene and pyrene, 80% in phenanthrene). For the fundamental stretching modes, the two bands occur respectively in the 3.205-3.23 µm (bay H) and 3.23-3.28 µm (non-bay H) ranges for the gas phase, and slightly shifted to higher wavelength in the condensed phase. Accordingly, from a study of the visible-near-infrared reflectance spectra of 47 simple and substituted PAHs in the solid state, [START_REF] Izawa | Reflectance spectroscopy (350-2500 nm) of solid-state polycyclic aromatic hydrocarbons (PAHs)[END_REF] showed that the overtone bands have mostly one major band (as we observed too) and their positions are relatively well constrained in a narrow range: 1.138-1.150 µm for 3νCH and 1.673-1.690 µm for 2νCH mode, with a small shoulder in the range 1.645-1.650 µm.

Depending on the exact PAH or mixture, its detectability from the 2νCH 1.685 µm band may therefore be only slightly decreased if the band shifts to the lower limit of its wavelength range (more interference with the 1.645 µm H2O ice band) but will increase if its peak shifts away from this band. For the 3νCH band, no effect on detectability is expected as there is no interfering band nearby. All these shifts have no effects for the detectability in dust as the aeolian dust spectrum display no features in these ranges having a quite flat spectrum.

Another factor that may affect detectability (by weight %) is the H/C ratio of the molecule or the PAH mixture. In our mixture this ratio is relatively low (0.45) due to the use of one deuterated molecule. It is similar to the values for larger compact PAH molecules, e.g. 0.5 for coronene (C24H12), and lower than for the small PAHs found in Martian meteorites [START_REF] Becker | Polycyclic aromatic hydrocarbons (PAHs) in Antarctic Martian meteorites, carbonaceous chondrites, and polar ice[END_REF]:

0.6 for chrysene (C18H12), 0.625 for pyrene (C16H10), 0.67 for perylene (C20H12) and 0.71 for both anthracene and phenathrene (C14H10). But these differences are quite small compared to the previously discussed radiative transfer effects controlling the detectability of PAHs.

Only if some aromatic C=C bonds in the PAH material are eliminated, either by substitution (by oxygen atoms, OH, CH3, …) or by hydrogenation, will the number of aromatic C-H stretching modes decrease, and consequently the strength of both the 1.14 and 1.685 µm bands. In the last case (Hn-PAHs) new, intrinsically stronger, aliphatic C-H stretching modes will appear at higher wavelength, shifted by +0.10-0.26 µm for the fundamental modes [START_REF] Sandford | The infrared spectra of polycyclic aromatic hydrocarbons with excess peripheral H atoms (Hn-PAHs) and their relation to the 3.4 and 6.9μm PAH emission features[END_REF] and thus by about +0.05-0.13 µm for the first overtone, and + 0.03-0.09 µm for the the second, as observed by [START_REF] Izawa | Reflectance spectroscopy (350-2500 nm) of solid-state polycyclic aromatic hydrocarbons (PAHs)[END_REF]. Their first overtone will be easier to observe as it will shift towards the minimum absorption between the 1.645 µm and the broad 2-µm water ice bands, but it will be the reverse for the second overtone as it will shift in the wing towards the peak absorption of the 1.26 µm H2O band. However, this particular family of PAH molecules has not been studied in our experiments.

Conclusions

To summarise: a detectability limit of ~0.04% has been established for observing PAH features in sublimating CO2 ice but this detection limit may drop by a large factor (to ~0.01%) in coarse grained ice if the amount of dust is at its lowest values (~0.02%) measured on the South Polar Cap. On the other hand, even at its maximum detected concentration in CO2 ice (~0.12%), water ice should have only a limited effect on the detectability of PAHs.

Similarly in the PAH-H2O-dust lag deposits observed on the SPC margins and rim scarps the amount of dust is the main factor that may strongly limit the detectability of PAH (up to only 1% manuscript submitted to JGR Planets in the original CO2 ice) while in dust-poor PAH-H2O lag deposits PAHs can be detected when the PAH/H2O ice ratio is larger than 25%, i.e. for initial PAH concentration in CO2 ice in the range 0.01-0.05 %.

These detectability limits are roughly applicable to most types of CnHn PAHs as the two diagnostic bands only slightly change in position and specific band strength among this PAH family. If other PAH families (substituted, hydrogenated…) are present on Mars or other icy bodies, then specific studies of their mixtures with CO2 or H2O ice and dust should be performed to assess their detection limits in specific environments.

The detectability levels achievable in the near-infrared in favorable conditions on Mars are thus of the same order than the amount detected on other planetary bodies, i.e., 10 -4 to 10 -3 g/cm3 [START_REF] Cruikshank | Hydrocarbons on Saturn's satellites Iapetus and Phoebe[END_REF]. One particular advantage of the near infrared bands may be that they allow us to probe deeper into the surface (up to few millimeters or centimeters for clear CO2 ice slab) than just the very first microns seen by the 3.29 µm PAH band.

When future space observations of the SPC are recorded at higher spectral resolution & sampling than our measurements (19 nm/10 nm) the better separation between the relatively narrow 1.685 µm PAH band and the 1.645 µm H2O ice band will further improve the PAH detectability.

Figure 1 :

 1 Figure 1: Top: Spectra from sample 1, 0.10% PAH in CO2 ice (with small amount of H2O ice ~0.12%) at -100°C during progressive sublimation of CO2 (PAH_1a to 1g). Black, dotted vertical lines indicate the main infrared PAH absorption features. The sublimation was first free (1a, 1b) then triggered by illumination with a lamp (55W/m 2 at sample surface): 1e-1g. The spectrum of the PAH mix and of CO2 ice (with small amount of H2O ice ~0.075%) are also shown for reference. Note the increasing slope below 1.1 µm and the bands at the limit of detection at 1.14 and 1.685 µm. Bottom: Detail of PAH absorption features incicated by black arrows

Figure 2 :

 2 Figure 2: Top: Spectra from sample 2, 0.67% PAH in CO2 ice (with small amount of H2O ice ~0.2%) at -100°C during progressive sublimation of CO2 (PAH_2a to 2n). Black, dotted vertical lines indicate the main infrared PAH absorption features, transparent grey boxes indicate transforming CO2 ice absorption features. The sublimation was free until the complete disappearance of CO2 ice. The spectrum of the PAH mix and of CO2 ice (with small amount of H2O ice ~0.075%) are also shown for reference. Note the increasing slope below 1.1 µm and the bands clearly appearing at 1.14 and 1.685 µm, but also in the 2.1-2.6 µm range. Bottom: Detail of PAH absorption features incicated by black arrows

Figure 3 :

 3 Figure 3: Top: Spectra from sample 3, 0.54% PAH in CO2 ice (with small amount of H2O ice ~0.08%) at -100°C during progressive sublimation of CO2 (PAH_3a to 3p). Black, dotted vertical lines indicate the main infrared PAH absorption features, transparent grey boxes indicate CO2 ice absorption features mentioned in the text. The sublimation was free until complete disappearance of CO2 ice. The spectrum of the PAH mix and of CO2 ice (with small amount of H2O ice ~0.075%) are also shown for reference. Note the increasing slope below 1.1 µm and the bands clearly appearing at 1.14 and 1.685 µm, but also in the 2.1-2.6 µm range. Bottom: Detail of PAH absorption features incicated by black arrows.

Figure 4 :

 4 Figure 4: Spectra from samples 4 and 5, 1.52% PAH in JSC Mars-1 (dust_PAH_4a), and JSC Mars-1 (dust_5a) at room temperature. Black, dotted vertical lines indicate the main infrared PAH absorption features. The spectrum of the PAH mix is also shown for reference (right scale). Note that no sign of increase of slope below 1.1 µm and no bands are detected at 1.14, 1.685 µm, nor at 3.29 µm,

  Figure 5: Relative band depth of the 1.14 and 1.685 µm bands of PAH versus the mass fraction of PAH (contributing to these aromatic C-H stretching bands) of the initial homogeneous mixture in CO2 ice at -100°C. The horizontal line represents a band depth detection level of 0.6% (at 3σ with S/N=450-500).

Figure 6 :

 6 Figure 6: Relative band depth of the 1.14 and 1.685 µm bands of PAH versus the mass column of PAH (contributing to these aromatic C-H stretching bands) in the PAH-H2O ice sublimation lag deposit. The horizontal line represents a band depth detection level of 0.6% (at 3σ with S/N=450-500).

Figure 7 :

 7 Figure 7: Spectra from three initial samples (1a, 2a, 3a) with varying amount of PAH in CO2 ice (with small amount of H2O ice ~0.08-0.2%) compared to the spectrum of the PAH mix and with those of CO2 ice (with ~0.075% H2O ice) and pure H2O ice at 173K (Philippe 2016). Black, dotted vertical lines indicate the main infrared PAH absorption features.

Table 1 :

 1 Sample Details

	Sample No.	Sample 1	Sample 2	Sample 3
	CO2 Mass in g	31	23.5	30
	PAH Mass in mg	32.7	158.1	161.6
	Weight percentage of PAH to CO2 in %	0.10	0.67	0.54
	Weight percentage of H2O to CO2 in %	~0.12	~0.2	0.08
	Weight fraction of PAH relative to H2O	~0.8	~3.3	6.75
	Density in g/cm 3	0.98	0.74	0.94
	Porosity in %	38.5	52	40
	4.2. PAH/CO2 = 0.1% -Sample 1

Table 2 :

 2 Details of Samples 4 and 5

	Sample Description	Sample 4 : PAH/ JSC Mars-1	Sample 5: JSC Mars-1
		Dust Mix	Dust
	Dust Mass in g	7.7	15.4
	PAH Mass in mg	117	-
	Weight percentage of PAH to dust in %	1.52	-
	Density in g/cm 3	1.895	1.91
	Porosity in %	48.1	49.3

Acknowledgments, Samples, and Data The measurements described in this work are the outcome of the Trans-National Access research project "Laboratory Analysis of Martian South Polar Residual Cap Analogues for Comparison with CRISM Observations" selected and funded in the framework of the Europlanet 2020 RI program (http://www.europlanet-2020-ri.eu). Europlanet 2020 RI received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 654208. The lead author is supported by MSSL STFC Consolidated grant no. ST/K000977/1 STFC under PhD studentship no. 526933.

The complete set of data presented in this paper (Campbell et al., 2017) is available online upon publication of this paper in the CSS database of the SSHADE database infrastructure (https://www.sshade.eu/db/css): https://doi.org/10.26302/SSHADE/EXPERIMENT_BS_20181101_001