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CfA 1.2 m Millimeter-Wave Telescope

The 1.2 meter Millimeter-Wave Telescope at the Center for Astrophysics | Harvard & Smithsonian and its twin instrument at CTIO in Chile have been studying the distribution and properties of molecular clouds in our galaxy and its nearest neighbours since the 1970s. The telescope is nicknamed "The Mini" because of its unusually small size. At the time it was built, it was the smallest radio telescope in the world. Together, "The Mini" and its twin in Chile have obtained what is by far the most extensive, uniform, and widely used galactic survey of interstellar carbon monoxide. "The Mini" is currently in operation from October to May each year.

In the early 1970s, an astronomer at the Goddard Institute of Space Studies in New York named Patrick Thaddeus shattered centuries of precedent in the field of astronomy and bucked a trend dating back to Galileo when he decided that, in order to proceed on a modest project to map the entire Milky Way, he simply did not need and in fact refused to use a larger telescope made available for his research. He wanted a small one. In an era made conspicuous by bigger, more sophisticated, and more expensive telescopes, Thaddeus insisted on a small and relatively inexpensive instrument, which he and his colleagues proceeded to build from scratch.

Purpose
Interstellar carbon monoxide is the best general tracer of the largely invisible molecular hydrogen that constitutes most of the mass in molecular clouds. Hydrogen is the simplest and most abundant element in the universe, and molecular hydrogen is by far the most abundant molecule. Unfortunately, under typical interstellar conditions molecular hydrogen does not emit at radio or millimeter wavelengths.

Carbon monoxide, however, the second most abundant ingredient in molecular clouds, has a rich and strong millimeter-wave spectrum and it seems to maintain a fairly constant ratio with molecular hydrogen of about 1:100,000. For this reason, carbon monoxide has become the standard tracer or "stain" for the invisible molecular hydrogen which constitutes most of the molecular mass.

Achievements
A total of 24 PhD dissertations have so far been written based on observations or instrumental work with these telescopes.

The 1.2 meter telescope has played an important or dominant role in all of the important general findings on molecular clouds (MCs) listed below. Many of these are now considered conventional wisdom but some were originally controversial (e.g., the very existence of giant molecular clouds, their ages, and their confinement to spiral arms).
 * 1977: Carbon monoxide is the best general-purpose tracer of molecular cloud mass.
 * 1977: Galactic carbon monoxide emission peaks in a broad "molecular ring" at R~4 kpc.
 * 1977/1994: Molecular clouds are mainly confined to a thin Gaussian layer ~100 pc wide, but a faint layer ~3 times as wide also exists.
 * 1980/1983: Molecular clouds are excellent tracers of galactic spiral structure.
 * 1980: Molecular clouds are relatively short-lived galactic objects.
 * 1982/1983: The molecular cloud mass spectrum is steep, with most of the mass in the largest clouds.
 * 1983: Intercomparision of carbon monoxide, HI, and diffuse gamma ray emissions provides perhaps the best large-scale calibration of carbon monoxide as a molecular mass tracer. The term X-factor was coined in this paper.
 * 1985/1989/1991: Molecular clouds are dark nebulae both in the optical and the near infrared.
 * 1986: Giant molecular complexes containing more than a million solar masses are not kinematic artifacts—as some had argued—but are well-defined objects that can be readily located throughout the galaxy.
 * 1988: Roughly half of the interstellar gas within the solar circle is molecular.
 * 2008: The enigmatic Expanding 3-kpc Arm has a Far 3 kpc symmetric counterpart on the far side of the Galactic Center.
 * 2011: The Scutum–Centaurus spiral arm extends almost 360 degrees around the galaxy, from the end of the central bar to the warp near its outer edge.

Personnel
Prof. Patrick Thaddeus (the Robert Wheeler Willson Professor of Applied Astronomy, Emeritus, Harvard University; Senior Space Scientist, Smithsonian Astrophysical Observatory), who was leading the Millimeter-Wave group, died on April 28, 2017. Tom Dame (Radio Astronomer, Smithsonian Astrophysical Observatory; Lecturer on Astronomy, Harvard University) has coordinated telescope observations over the last decade. Sam Palmer (Electronics Engineer, Smithsonian Astrophysical Observatory; Lecturer on Astronomy, Harvard University) continues to maintain the telescope hardware.

History
Built by Thaddeus and colleagues in 1974, the telescope was operated from a Columbia University rooftop in Manhattan until it was moved to the CfA in 1986. Its twin instrument was constructed at Columbia and shipped to Cerro Tololo Inter-American Observatory, Chile in 1982.

Observations of carbon monoxide had revealed that molecular gas in space was much more extensive than ever suspected. Initially, Thaddeus and his colleagues, Ken Tucker and Marc Kutner, had originally begun mapping the carbon monoxide using the sixteen-foot radio telescope at the McDonald Observatory in western Texas. The plan was to keep mapping outward from the clouds they were observing (the Orion Nebula and the Horsehead Nebula) until they found a place where there was no more carbon monoxide. They soon discovered that there was so much to be mapped that to do it with that size telescope would take many years. That large telescope could look at only a small area of the sky with each observation.

Thaddeus and his colleagues designed a radio telescope custom-built for the task of mapping the entire galaxy in carbon monoxide. The "Mini" was designed with a relatively small dish and consequently a relatively large beamwidth of about 1/8 degree, which can be likened to a wide-angle lens. With this new instrument, it suddenly became possible to map large stretches of sky in relatively small amounts of time.

Over the course of the next several years, a remarkable network of molecular clouds and filaments was uncovered, extending much further away from the Orion Nebula than expected. So large was the area covered, in fact, that Thaddeus and Dame (who had since joined the Columbia group) wished that they had an even smaller telescope, one which could quickly show them the big picture. Instead of building a smaller telescope, however, they decided to make a relatively simple change in the mini's control program. Rather than pointing at a single spot on the sky, they had the telescope antenna step through a square array of sixteen points on a 4 x 4 grid. In effect, this allowed the mini to mimic a smaller antenna with a half-degree beam. Because it is impossible to view the entire galaxy from New York, they also built an identical twin of the mini, which was shipped to Cerro Tololo, Chile to observe the southern sky.

After a decade of mapping using the superbeam technique, Dame and Thaddeus had created the first complete map of the galaxy in CO, covering more than 7,700 square degrees (nearly one-fifth of the sky) and representing more than 31,000 individual observations. The mapping revealed the distribution of molecular gas not only on the plane of the sky, but also in radial velocity. The large spread of observed velocities result mainly from the differential rotation of the galaxy.

Current research
Over the past few years a major goal of the 1.2 meter telescope has been completion of a survey of the entire northern sky lying outside the sampling boundary of the composite carbon monoxide survey of Dame et al. (2001). As of June 2013 this survey is nearly complete, consisting of over 375,000 spectra and covering ~24,000 sq-deg with 1/4° sampling. In addition, all molecular clouds at |b| > 10° and dec > −15° (~248) have been mapped every beamwidth.

In 2011, Dame and Thaddeus found clear evidence in existing 21 cm surveys for a large extension of the Scutum-Centaurus Arm, one of the two major spiral arms thought to extend from the ends of the galactic bar. The "Outer Sct-Cen arm" lies well beyond the solar orbit on the far side of the galaxy, roughly 21 kpc from the Sun. The CfA 1.2 m telescope has so far detected 22 distinct giant molecular clouds associated with HI peaks in the arm, and a large, unbiased carbon monoxide survey of the entire arm was begun in the fall of 2013; it is expected to require ~2 years to complete.

Antenna
The antenna system consists of a 1.2 m parabolic primary and 17.8 cm hyperbolic secondary in a Cassegrain configuration with effective f/D=2.8. The antenna primary is a monolithic aluminum casting with f/D=0.375, numerically milled by Philco Ford to 40 μm surface accuracy (l/65 at 115 GHz). The telescope's focus, beam pattern, and main beamwidth were most recently measured and adjusted in the fall of 1994 using a transmitter in the intermediate field (1.4 km distant on the roof of Harvard's William James Hall). The beam pattern matches well the predictions of scalar diffraction theory. The beamwidth (FWHM) is 8.4+/-0.2 arcmin and the main beam efficiency 82%.

The antenna is housed in a 16 ft Ash dome with a 75 in slit. During normal observations, the slit is covered with a screen of woven PTFE (polytetrafluoroethylene—Teflon), selected for its near transparency to microwaves, its strength, and its resistance to aging. The screen keeps the wind out of the dome and makes possible regulation of the temperature inside. LO reflections from the PTFE screen were found to be the source of occasional standing waves in scan baselines; subsequent modification of the mounting plates at the bottom and top of the screen gave it a "V" shape, eliminating surfaces of constant phase for the reflected LO and solving the standing wave problem.

Mount and drive
The telescope mount and drive systems are essentially unchanged from their configurations at Columbia. Because the telescope is small, direct-drive torque motors are used on both axes, with the advantage that the drive system has no gear trains. Although the motors provide only 11 lb.ft of torque, the telescope can change orientation at 10 degrees per second. Both axes are monitored by 16 bit shaft encoders and tachometers read at 100 Hz by the telescope-control computer to calculate torque corrections for pointing.

The pointing of the telescope is fine tuned at the beginning of each season by using a coaligned optical telescope to observe a large number of stars covering a wide range of azimuths and elevations. A least-squares fit to the pointing errors is used to define 5 pointing parameters (offsets of the azimuth and elevation encoders, effective longitude and latitude, and the small nonperpendicularity of the azimuth and elevation axes). Because the relatively large beam of the telescope makes continuum observations of planets inconvenient, pointing is checked weekly by radio continuum observations of the limb of the Sun. Although during the observing season (fall, winter, and spring) the Sun transits below the elevation of most carbon monoxide observations, it is the only practical astronomical source for pointing checks. At elevations used for observations, the root mean square pointing errors of the telescope were less than about 1', about 1/9 beamwidth.

Receiver
The heterodyne receiver, which uses a superconducting-insulator-superconducting (SIS) Josephson junction as the mixer, is the two-backshort design of Kerr (Pan et al. 1983). A scalar feed couples the microwave signal to the receiver, where it is mixed with a local oscillator (LO) signal to produce a 1.4 GHz intermediate frequency (IF) signal that is further amplified with a low-noise high electron mobility field effect transistor (HEMT FET) amplifier, and passed to the IF section of the receiver. The IF section further amplifies the signal and heterodynes it down to 150 MHz, passing a bandwidth of 200 MHz to the spectrometer.

The LO signal is generated by a Gunn diode oscillator whose frequency is controlled via a phase-lock loop system by a computer-controlled frequency synthesizer. The SIS mixer and the FET first stage amplifier are on the liquid helium-cooled cold stage of a vacuum dewar; the rest of the electronics are room temperature. Typical receiver noise temperatures at 115.3 GHz are 65–70 K single sideband (SSB). Although the performance improves somewhat to 55 K SSB if the helium dewar is pumped to 2.7 K, it is not standard observing procedure, because the sky noise at 115 GHz dominates at this level of receiver performance. On the best dry, cold days the total system temperatures are less than 350 K SSB, referred to above the atmosphere.

Spectrometer
The telescope has two software-selectable filter banks of a modified NRAO design, each containing 256 channels. At 115 GHz, the 0.5 MHz per channel filter bank provides a velocity resolution of 1.3 km/s, and velocity coverage of 333 km/s, and the resolution and coverage of the 0.25 MHz per channel filter bank are 0.65 and 166 km/s, respectively. The spectrometers divide the 150 MHz final IF signal from the receiver into 16 bands of 4 or 8 MHz width, each centered on 8 MHz. The 16 bands are passed to an equal number of filter boards, each with 16 contiguous two-pole Butterworth filters of 0.25 or 0.5 MHz width. The outputs of the filters are passed to square law detectors. After amplification, the detected signals are accumulated in integrators. The sampling time is 48 ms, followed by a 5 ms hold for sequential read-out by an analog-to-digital converter, after which the integrators are cleared for the next cycle. The 256 values produced by the converter are stored in a buffer during the following cycle, allowing the computer a full 48 ms to read the data.

Computer system
Prior to January 1991, pointing, data taking, and calibration of the radio telescope were controlled by a Data General Nova minicomputer ( picture ) running a custom telescope-control system. The control computer was fairly limited in speed and memory (having only 32 K byte of random access memory and 5 M byte of fixed disk storage), but it was fast enough to allow limited data reduction on-line. For further processing, all scans were transferred via 1600 bpi 9-track magnetic tape to a Digital Equipment VAXstation II/GPX workstation.

In January 1991, the telescope-control functions were transferred to a Macintosh IIfx computer, running a translated and improved version of the telescope-control system written in C. Individual scans or more commonly concatenated files containing large numbers of scans can be obtained from the control computer directly over the Internet. Generally the data is analyzed as FITS-format "cubes" of galactic longitude, latitude, and velocity. Such cubes can be built from the raw scan files either using custom Macintosh software or on Unix workstations with IDL or CLASS.

Calibration and observing techniques
The receiver noise temperature is calibrated at the start of every observing shift by measuring the difference in receiver response to ambient temperature and liquid nitrogen temperature loads. The loads are made of Eccosorb, a carbon-impregnated foam highly absorbent to microwaves and cone-shaped to prevent direct reflection of LO back to the feed.

Carbon monoxide line intensities are calibrated using the room-temperature chopper wheel method and the two-layer atmosphere model of Kutner (1978). At the carbon monoxide signal frequency the atmospheric opacity is appreciable, mostly due to molecular oxygen and water vapor, and corrections to the observed line intensities for signal attenuation must be applied. Kutner's two-layer model of the atmosphere parameterizes the elevation dependence of the correction factor in terms of only 3 parameters, each of which has a physical interpretation. Because oxygen has a much greater scale height than water vapor, the model assumes they can be considered separate layers, oxygen above water, with different characteristic temperatures and opacities. The temperature and opacity of oxygen in the upper atmosphere do not vary much seasonally and are assumed to be constant at 255 K and 0.378, respectively, at the signal frequency. The remaining parameters in the model, the temperature and opacity of water and the fraction of the received power from the sky, are determined through antenna tippings (measurements of the intensity of the sky signal as a function of elevation) at least once per six-hour observing shift, and more frequently if the weather is changing. Typical zenith water opacities ranged from 0.10 to 0.15, with values as low as about 0.05 in the coldest, driest weather. A 1-second calibration is performed at the start of each scan to correct for short term variations of the receiver gain and atmospheric opacity.

The observing season for the 1.2 m telescope, like other millimeter-wave telescopes at temperate northern latitudes, generally runs from October to May, with the best conditions in November through March. Cold, dry days afford the best observations, because of the decreased atmospheric opacity due to water vapor and the colder sky in general. Overall, the weather permits operation of the telescope roughly half of the time between October and May.

To obtain flat spectral baselines close to the galactic plane where emission typically covers a large range in velocity, spectra were acquired by position switching every 15 s between the source position (ON) and two emission-free reference positions (OFFs) selected by the telescope control program to straddle the ON in elevation. The fraction of the time spent on each OFF was adjusted so that the time-weighted average system temperature at the OFFs was equal to that at the ON, resulting in baselines that were flat, and residual offsets that were typically less than 1 K. This offset was generally removed by simply fitting a straight line to the emission-free ends of the spectrum.

Away from the plane in those regions where only one or two relatively narrow carbon monoxide lines are found, frequency-switching by 10–20 MHz at a rate of 1 Hz was often used instead of position switching. Since spectral lines remain within the range of the spectrometer in both phases of the switching cycle, data could be obtained twice as fast as with position switching, although higher order polynomials, typically 4th or 5th order, were required to remove the residual baseline. A telluric emission line from carbon monoxide in the mesosphere, variable in both intensity and LSR velocity, is detected in frequency-switched spectra; because the LSR velocity of the line could be predicted exactly, blending with galactic emission could be avoided by appropriate scheduling of the observations. In a few cases of large surveys (e.g., Taurus and Orion) a model of the telluric line was fit daily to spectra free of galactic emission and used to remove the line from all spectra.

title: CfA 1.2 m Millimeter-Wave Telescope


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User talk:Trakhtman~enwiki

Alternative Philosophy or Trakhtman-philosophy (http://www.trakhtman-philosophy.org) This cognitive philosophy is built like an open system in tespect to all known human ideas and concepts. It means, every idea could be put on the base of this philosophy. It leads to great extending the cognitive philosophy in comparison with known one. The main aspects to be put on the base of this philosophy are: 1. Religions It leads to the idea every Religion (not only Christianity) contains hidden own cognitive idea, own Science and Technologies. 2. Understanding and Not-understanding Accepting non-understanding leads to thinking by computer 3. Thuth and Non-truth together Accepting a paradox like the origin of cognitive philosophy leads to many achievements, firstly - in domains full of conflicts like Social sphere. Politics et cetera.

Your account will be renamed
Hello,

The developer team at Wikimedia is making some changes to how accounts work, as part of our on-going efforts to provide new and better tools for our users like cross-wiki notifications. These changes will mean you have the same account name everywhere. This will let us give you new features that will help you edit and discuss better, and allow more flexible user permissions for tools. One of the side-effects of this is that user accounts will now have to be unique across all 900 Wikimedia wikis. See the announcement for more information.

Unfortunately, your account clashes with another account also called Trakhtman. To make sure that both of you can use all Wikimedia projects in future, we have reserved the name Trakhtman~enwiki that only you will have. If you like it, you don't have to do anything. If you do not like it, you can pick out a different name. If you think you might own all of the accounts with this name and this message is in error, please visit Special:MergeAccount to check and attach all of your accounts to prevent them from being renamed.

Your account will still work as before, and you will be credited for all your edits made so far, but you will have to use the new account name when you log in.

Sorry for the inconvenience.

Yours, Keegan Peterzell Community Liaison, Wikimedia Foundation 03:24, 20 March 2015 (UTC)

Renamed
 This account has been renamed as part of single-user login finalisation. If you own this account you can |log in using your previous username and password for more information. If you do not like this account's new name, you can choose your own using this form after logging in: . -- Keegan (WMF) (talk) 19:57, 22 April 2015 (UTC)

license: Creative Commons - Attribution Share-Alike - https://creativecommons.org/licenses/by-sa/4.0/

title: User talk:Trakhtman~enwiki


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Hwa Chong

Hwa Chong is an educational brand name in Singapore encompassing Hwa Chong Institution, its affiliated institutions, as well as the former Hwa Chong Junior College.

Affiliated Schools
The affiliated schools under the brand name "Hwa Chong" are referred to as the Hwa Chong Family of Schools.

Hwa Chong Institution
Hwa Chong Institution (HCI) is a premier educational institution in Singapore. Established in January 2005 with the merger of The Chinese High School and Hwa Chong Junior College, the institution offers a six-year integrated program in partnership with Nanyang Girls' High School leading to the Singapore-Cambridge GCE Advanced Level examination.

Former Hwa Chong Junior College
The former Hwa Chong Junior College (HCJC) is a premier junior college in Singapore. Established in 1974, the college is one of the top performing junior colleges in Singapore in the 1990s. The college merged to form the current College Section of Hwa Chong Institution in January 2005 after the introduction of the Integrated Programme.

Hwa Chong International School
Hwa Chong International School (HCIS) is an international school in Singapore, and the international wing of Hwa Chong Institution, its parent institution. Founded in 2005, it offers an independent international school program leading to the International Baccalaureate qualification.

Hwa Chong Institution Boarding School
Hwa Chong Institution Boarding School is a boarding school built by the Hwa Chong family of schools, offering boarding options for students under the Hwa Chong affiliated schools, as well as students from other local institutions.

Origin
The name "Hwa Chong" was first used in 1972 when it was adopted as the name of Singapore's second junior college, and the first government-aided junior college. The name was intended as a direct translation of the abbreviation of the Chinese High School's native name, "華中" (Hua Zhong), which corresponds to "南洋華僑中學" (Nanyang Hua Qiao Zhong Xue). This was to reflect the affiliation of the Hwa Chong Junior College to the Chinese High School, despite being run by separate but related management committees. This is also reflected in the initial native name of the college, "華僑中學附屬初級學院", which translates to "Junior College affiliated to the Chinese High School". The name was shortened to "華中初級學院" in correspondence to its formal name.

In 2004, the decision to merge Hwa Chong Junior College and the Chinese High School led to a conflict about the name of the merged institution due to pressure from alumni, staff, and stakeholders to preserve the name and heritage of both independent schools. After a series of balloting, the merged institution adopted the name "Hwa Chong" from the junior college as the formal name, while retaining the native name of the Chinese High School.

The name, Hwa Chong, had since been adopted in schools in Singapore and overseas that are established under the educational organization encompassed under Hwa Chong Institution, as the institution sets to expand its global brand.

Emblem
The emblem shared across the Hwa Chong Family of Schools is in a form of the traditional Chinese character "學" (xué), which literally means to learn. The crest, with a red background, also bears many similarities to a burning torch of passion.

title: Hwa Chong


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Cherenkov Array at Themis

The Cherenkov Array at Themis (CAT) was an imaging atmospheric Cherenkov telescope (IACT) for detection of very-high-energy gamma rays (~200 GeV to a few tens of TeV). The project started operation in Autumn 1996 on the site of the former solar plant Thémis, France.

title: Cherenkov Array at Themis


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User talk:Shanedidona

Hi Shane

Welcome to Wikipedia. Can I ask you that, before creating new articles (say, 3DS Max primitive, Turbosquid), you consider contributing your knowledge to existing articles (say 3D Studio Max)?

Rgds, Rl 13:42, 20 Feb 2005 (UTC)

To-do list for WikiProject NCSU
I put NC State Wolfpack Football back in the requests section, as the article simply redirects you to NC State Wolfpack. It is not an article that needs to be expanded, but rather one that needs to be created. AceKingQueenJack 03:46, 13 December 2006 (UTC)

Images for cleanup
Why did you remove the ((ifc)) template from Image:Caelsanderson.bmp?

image:NCZooRustCube.JPG
Could you edit the description page of this image and state the source of this image, then could you add a copyright tag such as if it is your own photograph. Thanks   — Zeimusu | Talk 14:11, 11 Mar 2005 (UTC)

Re: Donal Hord
Hello Shane: You posted {I think} a "marker" at Donal Hord suggesting that the piece needed "This biographical article" help. While the piece is less than perfect, I don't see the "biological" aspect unless you are =referreing to. .   .    .    .    .   .   .   .  .  . . . . . ..........    don't know what you are referring to? HELP ?! ?! ? ! ? ! ? Carptrash 06:32, 20 Mar 2005 (UTC)

Lew Sapieha
Sorry Shane but I am no computer buff. Could you pls edit for me or leave as is? Thks. Vic

Bugging people
Hi Shane. You do good work, and then people like me come to bug you. :) Seriously, would you mind putting an edit summary? I saw several of your changes on my watchlist, all without edit summary, and it made me worried of what is going on. :) Something like "Linkify year" if you do things like 1977, would be nice. Thanks. Oleg Alexandrov 16:11, 31 Mar 2005 (UTC)

Image:DCP 4259.JPG
Burgundavia (✈ take a flight?) 06:59, May 30, 2005 (UTC)

welcome
Welcome!

Hello, and welcome to Wikipedia. Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! By the way, you can sign your name on Talk and vote pages using three tildes, like this: ~~~. Four tildes (~~~~) produces your name and the current date. If you have any questions, see the help pages, add a question to the village pump or ask me on my Talk page. Again, welcome!
 * The Five Pillars of Wikipedia
 * How to edit a page
 * Editing, policy, conduct, and structure tutorial
 * Picture tutorial
 * How to write a great article
 * Naming conventions
 * Manual of Style
 * If you're ready for the complete list of Wikipedia documentation, there's also Topical index.

Thought this might be usefull, since I've seen you "forget to sign" three out of three :) --MarSch 14:35, 6 Jun 2005 (UTC)

a favor
Hi Shane, I was hoping you could do me a favor as I really need to get some perspective on what other people see when they read Scalar field. I would be especially interested in what you think about my recent additions (the section with the examples). --MarSch 19:14, 11 Jun 2005 (UTC)

GNumber
No, it's just meant to link to other articles with "G" and a number at the end, and this not only includes economic summits, but also other useful disambig articles. secfan 10:20, Jun 12, 2005 (UTC)

your categories
Hi shane, you haven't voted yet on Categories_for_deletion. --MarSch 13:09, 12 Jun 2005 (UTC)

I'm confused by WikiProject Wikification
I don't understand what you are trying to do with WikiProject Wikification. The Scope talks about making a how-to article, but doesn't say what the subject would be(we already have instructions on how to Wikify pages...) and the Goals just says: wikify the pages that need it - which seems obvious. What is the project intended for? JesseW 30 June 2005 07:09 (UTC)

On the Catholic Church of Wikipedia
As you have described yourself as a Catholic, I thought I would alert you as a co-religionist to your opportunity to delete the particularly offensive article, Catholic Church of Wikipedia.--Thomas Aquinas 21:57, 27 November 2005 (UTC)

A Message to Pro-Life Wikipedians
The section "Foetal Pain" (Fetal Pain) has been deleted from the Abortion article. Could you help restore it? If you would like to see what was deleted, go to my talk page, scroll to "Fetal Pain," and click the provided link.--Thomas Aquinas 22:29, 28 November 2005 (UTC)

Pro-life Alliance
The article Pro-Life Alliance has been nominated for deletion. Chooserr

This type of censorship makes me sick
Vote to keep, show these hypocrites what's what, tolerance? ha, only when it's good for them--Diatrobica;l 23:15, 15 December 2005 (UTC)

Catholic Alliance
I think it'd be a braw Idea, although recently I've begun to feel a bit disappointed with Catholics...not the firm ones but the ones that don't listen to the Pope and feel they can ignore the laws set down by the Church. Chooserr 06:10, 24 December 2005 (UTC)

Braw is used commonly to mean fine, or good. Chooserr 22:05, 24 December 2005 (UTC)

Possible schism?
If you look in Category:Christian Wikipedians you will see that there is now two Catholic groups. -- Fplay 20:42, 24 December 2005 (UTC)

 * I realize that it was just a silly lack of awareness of the other category. Since I assume that these cats exist so that users can associate based on their affinities, it might be good to unify on the larger, older category name. -- Fplay 20:59, 24 December 2005 (UTC)

CAoW
I think it would be a good idea for you to join the Catholic Alliance of wikipedia, which is a pro-life group. --Shanedidona 21:13, 24 December 2005 (UTC)

Well I'll join if that's the case. Chooserr 22:06, 24 December 2005 (UTC)

Hi
could you please explain to me what the CAoW is? I am pro-life person, but wiki should be neutral even though abortion is an evil. if an artical is on just what abortion is then theres nothing wrong with it even though it disgusts me but if it starts going on about how great abortion is after i vomit then thats just wrong and not neutral, so could you explain to me what exactly the CAoW is please? thank you and merry christmas

ok I think that even though pro life is fantastic and that I support it, wiki is supposed to be neutral like Canada, and even though abortion is disgusting we shouldn't try to pull others into voting a certain way I'm sorry I can't vote to save this.

I can see that now, but shouldn't we try to keep this as unbiased as possible? I want to save them too, but we do need to make things unbiased. and I don't know how to do that and still keep the articals prolife I mean this is an encyclopedia, I'm starting to become torn on this issue here. but I honestly don't know what to say right now.

Happy holidays!

Deckiller 03:29, 25 December 2005 (UTC)

CAoW
Sorry, I haven't been on Wikipedia for a couple of days so I didn't get your request for a vote on its deletion until it was too late - although since your message was only three days ago I presume it must have been speedied anyway Cynical 14:42, 28 December 2005 (UTC)

Userboxes
You recently created the userbox User evol-0. To that, I've added User evol-1, User evol-2, User evol-3 and User evol-4. Because of those new userboxes, User evol-0 largely overlaps with User evol-1. Evol-0 says that "this user doubts one or more components of the theory of evolution", while Evol-1 says that "this user is not fully convinced of the theory of evolution." I personally think that it would be best if the wording of Evol-0 were edited to something like "this user does not believe in the theory of evolution." That way, the userbox would mirror the 0-category in the language userboxes ("this user does not speak [X]"). How do you feel about this? Aecis Mr. Mojo risin' 23:14, 30 December 2005 (UTC)

 * I have copypasted the original wording of User evol-0 to User evol-1, because I believe that the wording is more appropriate in 1 (doubting) than in 0 (not believing). I also believe that it is more appropriate than what I had originally written in User evol-1 (not fully convinced), which would probably belong in 2 or 3. Aecis Mr. Mojo risin' 16:18, 2 January 2006 (UTC)

Penis
Because you list yourself as Catholic I thought I would inform you of a particularly offensive image on the Penis page, or the subject in question. It shouldn't belong here, and the diagram is enough for me. If you feel the same please remove it, or help fight the case on the talk page. Chooserr 05:42, 2 January 2006 (UTC)

Euro
Well I guess hate might be overstating it. I just don't think it is right for the UK, and if I was in any other country I wouldn't support a "Global Currency", but I do like the fact that there is a Vatican Euro.

The other items on my "hate list" are BCE, because it means "before the Common Era" and is meant only to remove Christ from the dating system (It's more obvious in the switch from A.D. to C.E. <-- Common Era), the Metric System because of the way it's enforced, and the term happy holidays for the same reason as BCE. Chooserr 03:20, 20 January 2006 (UTC)

 * Oh I wanted to ask if you'd add the MAKEABORTIONHISTORY banner from my talk to your talk page....If you don't want to that's fine, but it promotes awareness, and helps promote Pro-life billboards and the option of adoption. It's a US charity as well, and you can put it in different sizes... Chooserr 03:30, 20 January 2006 (UTC)

 * There is also a vote for deletion on F.A.C.T.1, a pro-life organisation whose name stands for "Father's of Aborted Children Together as One", I just wanted to give you the option to vote. Chooserr 03:33, 20 January 2006 (UTC)

F.A.C.T.1
Shanedidona, hi. I noticed your comment on Chooserr's talk page, and thought I'd reply to you here. Do you really believe that F.A.C.T.1 was deleted for political reasons? I ask because I really don't see that, and maybe you can show me what I'm missing. It seems to me that it was a perfectly routine deletion of an article about an organization that, while "valid" and real, hasn't really aroused comment in the world at large. Many Wikipedians follow what it says at Verifiability: "Subjects that have never been written about by third-party published sources, or that have only been written about in sources of dubious credibility should not be included in Wikipedia."

F.A.C.T.1, despite all the good work I'm sure they do, hasn't been written about by third-party published sources that anyone here has been able to find. Their contact info appears on a few lists out on the 'net; that's all. They haven't even been written about by themselves, as their website is "under construction". At that point, their politics don't really enter into the equation, most Wikipedians of AfD will support deletion of un-remarked on organizations, whether they're conservative, liberal, or neither.

I have seen articles nominated for deletion for political reasons, but I don't think this was one of them. If you really think it was, and can convince me, I'll support a deletion review on it. I'm against people using Wikipedia to advance their political views; I just don't see that going on here. Can you show me what I'm not seeing? -GTBacchus(talk) 20:35, 22 January 2006 (UTC)

 * Shanedidona,
 * I too noticed your comment on my talk page, and can start of by saying that I'd never mistake you for a person "who doesn't like conservative values" :). That said though I do want to add that while the article mostlikely was nominated because it didn't have too much content I believe that some of the voters were very liberal people who don't want it on wikipedia.
 * My best advice is that we work together to re-right the article in a place like User:Chooserr/F.A.C.T.1 or User:Shanedidona/F.A.C.T.1, and reinstate it to the position of a proper article once we've enough evidence to argue it's validity, and enough sources to show that quite a few third parties have written about it. Chooserr 07:48, 23 January 2006 (UTC)

Stalking?
Absolutely not. I've been subscribed to the article F.A.C.T.1 and to Chooserr's talk page for some time, and I take an interest in certain politically sensitive areas of Wikipedia. I have much better things to do than stalk anyone. You are welcome to reply to the content of what I said to you, or to ignore me completely, but no, I'm not stalking you. I'm not subscribed to any of your pages, and I don't follow your edits, nor have any interest in doing so. -GTBacchus(talk) 21:10, 23 January 2006 (UTC)

Replacement?
I made an article to replace the deleted F.A.C.T.1 one Chooserr 01:54, 24 January 2006 (UTC)

Could you address something?

 * Could you address a question on the discussion page for the following Wikipedia article? David C. Geary

Hello CAoW
I was wondering if it would be alright for me to reword the CAoW bit, and add some other information to tempt wikipedians to join this noble organisation. Chooserr 00:47, 1 February 2006 (UTC)

"Safe Sex"
I don't want to violate the 3rvt rule, so I was wondering if you'd look over the safe sex article and determine whether or not it deserves to have quotes "" around the word as in "war on christmas". Chooserr 22:51, 1 February 2006 (UTC)

Help
Okay I'll get right on it, but could you help me out on the Casual sex page and the Safe sex page, because on both my reverts are up, and my contributions are important. Please look them over, Chooserr 01:12, 2 February 2006 (UTC)

Oh yeah LifeStyles is up for deletion if you want to weigh in. Chooserr 01:17, 2 February 2006 (UTC)

CAoW
Saw your post on Chooserr's talk -- see Wikipedia:Miscellany for deletion/User:Shanedidona/CAoW. There are other discussions linked at the top. --Sar e kOfVulcan 21:38, 3 February 2006 (UTC)

Boxes
I don't know what happend to them, and I don't know who created them, but there was no time for a vote to be drawn so some admin over stepped there power and deleted them. I'll go see if I can find anything more on it. Chooserr 19:32, 18 February 2006 (UTC)

Userboxes
No, I just noticed a bunch of red links and decided to clean itup. You can always check who deleted them by going to Special:Log and typing in the name of the page. Dmcdevit·t 19:15, 19 February 2006 (UTC)

new Catholic Weekly Collaboration!
Just thought I would let you know that there is a new Catholic Collaboration of the Week! I hope you can contribute! --Hyphen5 16:52, 31 March 2006 (UTC)

Use of fair use images in user space
I removed Image:Vatican coa.png from your userpage because the image is tagged as a fair use image. According to Wikipedia policy, you may not use such images outside of the main article namespace. Thus, your use of it in userspace is against policy. My removal of it was not vandalism. For the relevant policy, please see Fair_use item #9. Please revert your re-insertion of the image. I will not revert your revert because I have no desire to get into an edit war about this. I would much rather you understood why this is necessary and have you take the appropriate action. Thank you, --Durin 19:59, 15 April 2006 (UTC)

Conservative_notice_board
Hello, I noticed that you identify as a conservative Wikipedian. So I would like to invite you to post any conservative issues you might have over at the new project page, Conservative_notice_board. Thanks. --Facto 05:54, 15 June 2006 (UTC)

Iraq and the War on Terrorism
WOT has opened its straw poll, and is open to discussion. Rangeley 00:58, 19 June 2006 (UTC)

Donation link
Shanedidona, hi.

I thought I should let you know that the link on your talk page, under the words "Make abortion history" has recently been removed from another user's talk page, with pretty strong administrative support. Per WP:UP, our user pages are really for building the encyclopedia, and while we are generally happy for people to use their pages to tell us a little bit about themselves, soliciting donations crosses the line from simple information to advocacy. I think it would be best if you remove that link, and I can't guarantee that another admin, seeing it, won't just be bold and delete it. -GTBacchus(talk) 00:26, 19 June 2006 (UTC)

 * Actually - now that I check, the link appears to be broken anyway... -GTBacchus(talk) 00:26, 19 June 2006 (UTC)

Asheboro
not me! WillC 19:14, 6 July 2006 (UTC)

Question about [...]
I answered your question about the puncuation on the Talk:G20 developing nations. --chemica 22:48, 25 July 2006 (UTC)

coor dms template and AWB
How did you set AWB to apply the coor dms template? --Shanedidona 14:36, 16 August 2006 (UTC)
 * to the top of the page that has been nominated for deletion (just below the existing speedy deletion or "db" tag), coupled with adding a note on : explaining your position, but be aware that once tagged for speedy deletion, if the page meets the criterion it may be deleted without delay. Please do not remove the speedy deletion tag yourself, but don't hesitate to add information to the page that would render it more in conformance with Wikipedia's policies and guidelines. Lastly, please note that if the page does get deleted, you can contact one of these admins to request that they userfy the page or have a copy emailed to you.   DougsTech (talk) 03:36, 20 March 2009 (UTC)

March 2009
Welcome to Wikipedia. A page you recently created may not conform to some of Wikipedia's guidelines for new pages, so it will shortly be removed (if it hasn't been already). Please use the sandbox for any tests. For more information about creating articles, you may want to read Your first article. You may also want to read our introduction page to learn more about contributing. DougsTech (talk) 03:39, 20 March 2009 (UTC)

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title: User talk:Shanedidona


text:
Countess Maria of Nassau (1556–1616)

Countess Maria of Nassau (7 February 1556, Breda – 10 October 1616, Buren) was the second daughter of William the Silent by his first wife Anna of Egmont. She was named after William's first daughter, Maria, who had died in infancy.

Biography
At the start of the Eighty Years' War her older brother Philip William was removed to Spain where he was raised as a Catholic. Maria vigorously defended her brother's claims to the title Prince of Orange and the barony and city of Breda against the claims of their half-brother Maurice of Nassau.

It was her wish to marry Philip, Count of Hohenlohe, whom she had known since she was eleven. This plan met with initial resistance of her father (he gave his permission in 1582) and continued resistance from her brother Maurice. She was supposed to marry the (Catholic) son of the duke of Aerschot, to help acquire him as an important ally against the Spanish forces, but Maria refused to marry him as she had become a Calvinist. Also, Maria claimed guardianship of the possessions of Philip William while hostage in Spain, because of her being a full sister to Philip William, while Maurice was only his younger half-brother, and started a trial.

On 2 February 1595, at the age of 39, Maria finally married Philip of Hohenlohe in Buren, in the Dutch Reformed Church. The couple remained childless and Philip died in 1606. Her brother Philip William was released in 1595 and returned to Breda in 1610. In 1612, Maria founded a large orphanage in Buren.

She died in 1616 in Buren. She was entombed in the Saint Lambert Church there, which by then had become a Protestant Reformed Calvinist church.

title: Countess Maria of Nassau (1556–1616)


text:
NSX

NSX may refer to:

Stock exchanges

 * Namibian Stock Exchange (NSX)
 * National Stock Exchange (Jersey City, New Jersey), US (NSX)
 * National Stock Exchange of Australia (NSX)

Other uses

 * Honda NSX (New Sportscar eXperimental/eXperience), an automobile distributed as Acura NSX in North America
 * Post Office Sorting Van (NSX), a British rail vehicle
 * VMware NSX, a network virtualization product
 * Narrow Shape Cross-Section Blade (NSX), an ice-skating blade designed by Diederik Hol

title: NSX


text:
Chicago Air Shower Array

The Chicago Air Shower Array (CASA) was a significant ultra high high-energy astrophysics experiment operating in the 1990s. It consisted of a very large array of scintillation detectors located at Dugway Proving Grounds in Utah, USA, approximately 80 kilometers southwest of Salt Lake City. The full CASA detector, consisting of 1089 detectors began operating in 1992 in conjunction with a second instrument, the Michigan Muon Array (MIA), under the name CASA-MIA. MIA was made of 2500 square meters of buried muon detectors. At the time of its operation, CASA-MIA was the most sensitive experiment built to date in the study of gamma ray and cosmic ray interactions at energies above 100 TeV (1014 electronvolts). Research topics on data from this experiment covered a wide variety of physics issues, including the search for gamma rays from Galactic sources (especially the Crab Nebula and the X-ray binaries Cygnus X-3 and Hercules X-1) and extragalactic sources (active Galactic nuclei and gamma-ray bursts), the study of diffuse gamma-ray emission (an isotropic component or from the Galactic plane), and measurements of the cosmic ray composition in the region from 100 to 100,000 TeV. For the topic of composition, CASA-MIA worked in conjunction with several other experiments at the same site: the Broad Laterial Non-imaging Cherenkov Array (BLANCA), the Dual Imaging Cherenkov Experiment (DICE) and the Fly's Eye HiRes prototype experiment. CASA-MIA operated continuously between 1992 and 1999. In summer 1999, it was decommissioned.

Specifications and design
CASA was built to study the possibility of astrophysical sources of ultra high energy (UHE, E > 100 TeV) gamma-ray emission (see Science below). Gamma rays at these energies interact in the Earth's atmosphere to create an extensive air shower that propagates to the Earth's surface. At the surface, the shower consists predominantly of electrons/positrons, low-energy gamma rays, muons, and some hadrons, with a typical footprint on the ground of 50–100 m. (There is also a component of Cherenkov radiation reaching the ground that can be recorded by imaging atmospheric Cherenkov telescopes). An air shower array is a distributed set of particle detectors (scintillation detector, water Cherenkov detectors, etc.) spread out on the ground to record the passage of the shower particles. The primary particle direction is estimated from the relative arrival time of the shower hitting each detector; the primary particle energy is estimated from the number of particles recorded in each detector and from the lateral distribution of those measurements. Prior to CASA, air shower arrays were typically modest in size, typically consisting of 50-100 detectors covering an area of around 50,000 square meters. The plan for CASA was to build a much more sensitive experiment that would be much larger in size, use state-of-the-art electronics, and be coupled with a large array of muon detectors (MIA). The expectation was that showers initiated by gamma rays would contain far fewer muons compared to showers initiated by cosmic rays. The original plan was for an array of 1064 detectors, but the number was subsequently increased to 1089.

Some of the key design features CASA-MIA were the following:

The trigger and data-acquisition sequence for CASA was complex because of the distributed electronics; it worked as follows:
 * 1089 scintillation detectors, spread out on a square grid of 33 x 33 detectors, with a detector spacing of 15 m, covering a total area of 230,000 square meters.
 * A CASA detector consisted of four separate scintillation counters; each counter consisted of a piece of acrylic scintillator 61 cm x 61 cm x 1.27 cm in size and read out by a single photomultiplier tube (PMT, either Amperex 2212 or EMI 9256).
 * Each CASA detector contained a local high voltage module and a custom-made electronics board that allowed each detector to take data independently of other detectors.
 * The CASA detectors were connected to a central controller via a rib-spine network consisting of coaxial cables with three functions: trigger request, trigger acknowledge and Ethernet.
 * The muon array (MIA) consisted of 1024 scintillation counters, each of size 1.9 m x 1.3 m. The muon counters were arranged in 16 patches of 64 counters each and were buried beneath 3 m below the surface. Signals from the MIA counters were run under the ground to a central trailer where relative arrival times were measured by conventional LeCroy 4290 time-to-digital converters (TDCs).

CASA, and its associated muon array MIA, achieved excellent performance and was the state-of-the-art in air shower experiments in the ultra high energy band for a considerable period of time after its operational period in the 1990s. Only in the late 2010s have experiments such as the Tibet Air Shower Array and the High Altitude Water Cherenkov Experiment surpassed CASA-MIA in sensitivity at energies above 100 TeV. The median gamma-ray energy for a source passing near zenith was 115 TeV. The gamma-ray angular resolution varied with the size (number of particles) in the detected shower and was approximately 0.7 degrees for showers with the median number of particles, improving to 0.25 degrees at higher energies. The muon array provided important capability to reject background cosmic ray events; at the median energy of 115 TeV, the fraction of cosmic ray events passing the muon selection criteria for gamma rays was 0.06 (i.e. approximately 17 cosmic ray events were rejected for each one accepted). At higher energies, the background rejection power was significantly increased; for example, at a median energy of 5,000 TeV, the fraction of cosmic rays passing muon selection criteria was reduced to approximately 0.0001.
 * The PMT signals in each counter are each sampled by a low-level and high-level discriminator. The low discriminator level is set to around 0.1 of the signal from a typical minimum-ionizing particle; the high discriminator level is set to around three times that of the low level.
 * A detector with two or more counters firing the high-level discriminator in 30 nsec is "alerted"; a detector with three or more counters firing the high-level discriminator if 30 nsec is "triggered.
 * Alerted stations carry out local data acquisition tasks and inhibit further triggering of the station. Time-to-voltage converters on the local electronics board hold the four relative times of the four counters in a detector (determined by the crossing time of the low-level discriminator) and four times corresponding to the times of arrival of pulses sent by the neighboring four detectors, if they have been alerted. Sample and hold circuits record the four charges corresponding to the integrals of the PMT signals from each counter. Alerted stations wait for 10 μsecs for a trigger acknowledge signal from the central station; if no signal is received, their data are discarded.
 * Triggered stations place a fast current pulse (5 mA, 10 μsec duration) onto the rib trigger request coaxial cable (RG-58, 50Ω); these signals are propagated to a central trigger box via a repeater at the rib/spine junction and a spine trigger request coaxial cable (RG-8, 50Ω).
 * The entire array is triggered when three trigger request levels are received by the central trigger box. Then, a fast signal (12V, μsec duration) is placed on the trigger acknowledge coaxial line where it is propagated back to each station via the rib-spine network.  Upon receipt of a trigger acknowledge signal, alerted stations digitize their eight times and four charges through a multiplexer and a 10-bit analog-to-digital converter (ADC). The digitized data are stored in a memory buffer under the control of a microprocessor (Intel 80186).  The dominant deadtime for the array is when data are digitized (approximately 0.5 msec).
 * Periodically (typically every 30 sec), the station electronic boards receive a command over Ethernet to transmit their data to a central computer (DEC μVAX III+). Each board switches their memory buffer and continues to accumulate data; the previous recorded data are transmitted over the rib-spine network to the center where they are recorded on disk.

History
The scientific motivation for CASA came from intriguing results from several experiments in the 1980s. These experiments reported excess air shower events from the direction of two well-known Galactic X-ray binary sources: Cygnus X-3 and Hercules X-1. In 1983, the Kiel and Haverah Park experiments reported an excess of events from the direction of Cygnus X-3, where the arrival times of the events appeared to be modulated by the 4.8-hour orbital periodicity of the binary source. The statistical significance of each signal was weak (around four standard deviations above background), but the results implied that Cygnus X-3 was a luminous emitter of ultra high energy gamma rays and that, in order to do so, it must be a very efficient accelerator of high energy cosmic rays and hence it could provide a large fraction of the pervading flux of cosmic ray particles in our Galaxy.

After these results, a number of groups around the world began designing, or improving, air shower arrays to make follow-up studies. One of these groups was from the University of Chicago,led by James Cronin. Cronin's idea was to build a definitive experiment that could easily verify, or refute, the results on Cygnus X-3. The experiment would be much larger (and much more sensitive) than the Kiel or Haverah Park experiments and it would use a large array of muon detectors to reject the background of hadronic cosmic ray events (i.e. protons and nuclei). (Showers initiated by gamma-ray primaries are expected to have far fewer muons than those initiated by cosmic ray primaries). Cronin assembled a team of scientists (discussed in Collaboration) to develop and construct CASA. The University of Chicago group was partnered with groups from the University of Michigan and the University of Utah, who had already constructed a muon array and smaller air shower array, and the site for CASA would be on Dugway Proving Grounds.

The construction and deployment of CASA took place between 1988 and 1991. Construction activities were carried out at the University of Chicago in the Accelerator Building of the Enrico Fermi Institute. The completed scintillation detectors, along with electronics, were shipped to Utah in large semi-trailers, where they were installed by students, postdocs and faculty. An initial array of 49 detectors became operational in 1989, followed by a 529-detector array in 1990. Standard science operation of the full 1089-detector CASA array (along with the 1024-counter muon array) started in December 1991. CASA operated very successfully, largely without interruption, until 1997. During that time a total of approximately 3 billion air showers events were recorded. Partial operations continued for several more years, in conjunction with the BLANCA and DICE experiments. The various experiments at the site, including CASA, ceased operation in 1999.

Science
The scientific results from CASA-MIA encompassed a dozen scientific publications and covered topics in three broad areas of high-energy astrophysics: gamma-ray point sources, diffuse gamma-ray sources, and cosmic ray physics.

 * Gamma-ray point sources: CASA-MIA set stringent limits on the emission from all sources that had been reported by earlier experiments, including Cygnus X-3 and Hercules X-1, the Crab Nebula, and known high-energy active galactic nuclei. For these sources, the CASA-MIA limits were typically two to three orders of magnitude lower than the flux levels reported by the previous instruments. Searches were also made for transient and period emission from point sources and a general survey of the overhead sky was also carried out.
 * Diffuse gamma-ray sources: the rejection power of the large muon array allowed CASA-MIA to study diffuse gamma-ray sources with great sensitivity. The most significant result came from a search of diffuse isotropic emission, which provided a limit on the electromagnetic fraction of the cosmic rays at a level less than 2 x 10−5 at the highest energies. Another significant result came from a study of diffuse emission from the Galactic plane.  A separate study searched for bursts from arbitrary directions in the sky to constrain short timescale cosmic events, such as the explosions of primordial black holes.
 * Cosmic ray physics: with its large and uniform air shower array, couple with a large muon detector, CASA-MIA had good capability to making measurements of the properties of the ultra high energy cosmic rays. The electron and muon shower size distributions (determined from CASA and MIA, respectively) were used to measure the cosmic ray energy spectrum between 100 and 10,000 TeV. The CASA-MIA results showed a smooth steepening of the spectrum, in contrast with some earlier experiments that reported a sharper feature (known as the "knee"). CASA-MIA measurements of the cosmic ray composition were made from a combined fit to the surface and muon detector data and indicated a mixed composition at lower energies (below 1,000 TeV) that evolved smoothly to a heavier composition at energies approaching 10,000 TeV.  A separate, and complementary, measurement of the cosmic ray composition was made by the BLANCA instrument that operated in conjunction with CASA-MIA and used the lateral distribution of the Cherenkov radiation in air showers.

Scientific collaborations
The CASA project was conceived by James W. Cronin and the design and construction were carried out by a team of scientists, engineers and technicians in the Enrico Fermi Institute of the University of Chicago (see for more details). The initial core group of scientists consisted of Cronin, postdoctoral fellows Kenneth Gibbs, Brian Newport, Rene Ong, and Leslie Rosenberg, and graduate students Nicholas Mascarenhas, Hans Krimm and Timothy McKay. During the operational phase of CASA, the Chicago group included postdoctoral fellows Mark Chantell, Corbin Covault, Brian Fick and Lucy Fortson, Kevin Green, and graduate students Alexandre Borione, Joseph Fowler and Scott Oser. The Michigan Muon Array was constructed by a team of researchers from the University of Michigan, including James Matthews, David Nitz, Daniel Sinclair, and John van der Velde, post-doc Kevin Green, and graduate students Mike Catanese and Ande Kennedy Glasmacher.

title: Chicago Air Shower Array


text:
Constellation-X Observatory

The Constellation-X Observatory (Con-X or HTXS) was a mission concept for an X-ray space observatory to be operated by NASA; in 2008 it was merged with ESA and JAXA efforts in the same direction to produce the International X-ray Observatory project, announced on 24 July 2008.

The intention of the Con-X project was to provide enough X-ray collecting area to be able to feed a spectroscope of substantially higher resolution than the previous generation (XMM-Newton, Chandra X-ray Observatory and Suzaku) of space-based X-ray telescopes; this would allow the resolution of individual hot-spots at the event horizon of black holes, of warm intergalactic matter (by seeing absorption lines at various redshifts superposed onto the spectra of background quasars) and of dynamics within galaxy clusters.

Technology for Con-X
The project intended to have separate low-energy and high-energy X-ray telescopes, to work from 100eV to 40keV spectrum. The collecting area requirements would have been achieved using a segmented-mirror technique based on slumping thin (400 μm) glass sheets onto mandrels, which avoids the handling problems of dealing with whole thin shells. Dispersive optics for the spectrometer were developed, as well as a microcalorimeter-array detector providing energy resolution per pixel of about 5eV.

The International X-ray Observatory (IXO)
In May 2008, ESA and NASA established a coordination group involving ESA, NASA and JAXA, with the intent of exploring a joint mission merging the ongoing XEUS and Constellation-X efforts. The coordination group met twice, first in May 2008 at European Space Research and Technology Centre (ESTEC), then in June 2008 at the Center for Astrophysics. As a result of these meetings a joint understanding was reached by the coordination group on a proposal to proceed towards the goal of developing an International X-ray Observatory (IXO). The coordination group proposed the start of a joint study of IXO. A single merged set of top level science goals and derived key science measurement requirements were established.

title: Constellation-X Observatory


text: Category:X-ray telescopes

title: Category:X-ray telescopes


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User talk:Ih8tziswurld

Welcome to the Wikipedia
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Feel free to contact me personally with any questions you might have. About, Help desk, and Village pump are also a place to go for answers to general questions. To read up on the latest wikinews, have a look at the Wikipedia Signpost.

You can sign your name by typing 4 tildes, like this: ~.

(Sam Spade | talk | contributions) 13:55, 20 Feb 2005 (UTC)

title: User talk:Ih8tziswurld


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Louth (Dáil constituency)

Louth is a parliamentary constituency represented in Dáil Éireann, the lower house of the Irish parliament or Oireachtas. The constituency elects 5 deputies (Teachtaí Dála, commonly known as TDs) on the system of proportional representation by means of the single transferable vote (PR-STV).

Boundaries
The constituency was created by the Electoral Act 1923, and first used at the 1923 general election. It currently spans the entire area of County Louth (which includes the towns of Ardee, Dundalk, Drogheda), the smallest county in Ireland, and parts of County Meath (suburbs of Drogheda and Laytown–Bettystown–Mornington–Donacarney). The boundaries were enlarged at the 2011 general election to include an area of County Meath adjacent to the town of Drogheda. This followed a recommendation of the Report of the Constituency Commission on Dáil and European Parliament Constituencies 2007 outlined "by extending the constituency southwards from, and in the environs of, Drogheda and taking in electoral divisions which have extensive linkages with the town. This will allow the inclusion of the town of Drogheda and hinterland areas in a single constituency." This revision also increased the number of seats to 5.

The Electoral (Amendment) (Dáil Constituencies) Act 2017 defines the constituency as:

The Constituency Review Report 2023 of the Electoral Commission recommended that at the next general election, Louth should remain a 5-seat constituency, with the transfer of the electoral division of Julianstown to Meath East.

For the next general election, the Electoral (Amendment) Act 2023 defines the constituency as:

Electoral division
Louth population as per electoral division, for the Dáil constituency of Louth. This population count includes those within the county of Louth, as well as the electoral divisions of Julianstown, and St. Mary's (part) in the county of Meath, as per the Electoral (Amendment) (Dáil Constituencies) Act 2017.

2011 general election
Séamus Kirk was Ceann Comhairle at the dissolution of the 30th Dáil and therefore deemed to be returned automatically. The constituency was treated as a four-seater for the purposes of calculating the quota.

1981 general election
Pádraig Faulkner was Ceann Comhairle at the dissolution of the 21st Dáil and therefore deemed to be returned automatically. The constituency was treated as a three-seater for the purposes of calculating the quota.

1954 by-election
Following the death of Fine Gael TD James Coburn, a by-election was held on 3 March 1954. The seat was won by the Fine Gael candidate George Coburn, son of the deceased TD.

title: Louth (Dáil constituency)


text:
Cosmic Anisotropy Telescope

The Cosmic Anisotropy Telescope (CAT) was a three-element interferometer for cosmic microwave background radiation (CMB/R) observations at 13 to 17 GHz, based at the Mullard Radio Astronomy Observatory. In 1995, it was the first instrument to measure small-scale structure in the cosmic microwave background. When the more sensitive Very Small Array came online, the CAT telescope was decommissioned in a ceremonial bonfire.

title: Cosmic Anisotropy Telescope


text:
Tupla (chocolate bar)

Tupla is a Finnish chocolate bar made by Cloetta. It consists of milk chocolate with a nougat-flavoured filling, coated with bits of almond.

The name "Tupla", meaning "double", comes from the fact that there are always two Tupla bars in a single wrapper. The bars are placed end-to-end.

The original Tupla dates back to the 1960 and is still one of the most popular chocolate bars in Finland. In the 1990s and 2000s two variants have been introduced: Tupla White, with a coating of white chocolate instead of milk chocolate, and Tupla Black, with bits of liquorice added into the filling.

There were even Tupla Easter eggs available in the 1990s. Despite the name, however, there weren't two chocolate eggs nested inside each other.

Ingredients
Glucose syrup, sugar, vegetable fats (palm, shea), skimmed milk powder, cocoa butter, almonds, whole milk powder, cocoa mass, fat reduced cocoa powder, whey powder (milk), hydrolyzed milk protein, salt, flavourings, emulsifier (sunflower lecithin).

Nutrition information
Per 100g: 1954 kJ /463 kcal (Energy), 19g (Fat) of which 10g (Saturates), 64g (Carbonhydrate) of which 57g (Sugars), 6,3g (Protein), 0,47g (Salt).

Weight
Bar weights are 50g TUPLA MAXI and 85g TUPLA KING SIZE.

Tupla Sport
In 2008 a new side-brand was issued, Tupla Sport. Tupla Sport has a high fiber content and comes in two flavours: apple and raspberry. Its main ingredients are chocolate, muesli, almonds and nougat.

Easy to open at any time
In 2019, Tupla ran ads which featured a variety of shots where the packaging was being opened using hands showing the new "Easy to open" feature. The ad was companied by a slogan - "Easy to open at any time". The ads ran in Estonia and Latvia.

title: Tupla (chocolate bar)


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Peter F. Paul

Peter Franklin Paul (born September 2, 1948) is an American former lawyer and entrepreneur who was convicted for conspiracy and drug dealing, and later for securities fraud in connection with his business dealings with Spider-Man co-creator Stan Lee.

He has repeatedly brought suit against Hillary Clinton, accusing her of lying about donations he solicited on behalf of her 2000 senatorial campaign.

In the 1990s, Paul managed Italian model, actor, and author Fabio Lanzoni.

In 1993, the L. A. Times described Paul as "bearded, balding and bespectacled...given to blue blazers and sedate gold pinky rings."

Personal life
In 1993, the L. A. Times reported that Paul owned a Rolls-Royce, Jaguar, Mercedes, and Porsche.

The Cuban coffee caper
In the 1970s, Peter Paul served as President of the Miami World Trade Center. As a result of what Paul described as anti-Communist and anti-Castro political activities, he directed a fraud on the Cuban government of $8.75 million by selling agents of Cuban president Fidel Castro nonexistent coffee. The plan apparently also involved sinking the ship that was to deliver the nonexistent coffee to hide the fraud from Castro and, according to Time magazine, to defraud its insurer, but the conspirators neglected to bribe a port official in Santo Domingo, and the people who were supposed to scuttle the boat were not allowed on board.

Paul pleaded guilty to federal conspiracy charges. When his home was raided by the police in connection with this crime, they found cocaine in his garage, and Paul also pleaded guilty to possessing cocaine with intent to distribute. He was sentenced to eight years in prison for the cocaine charge, and a concurrent three years for fraud; he was paroled after three years. His license to practice law was suspended as a result of the convictions, and he claims to have been sued by the Cuban government as well.

In 1983, Paul was caught traveling to Canada using the identity of a dead man; he pleaded guilty to federal charges of making false statements to customs inspectors. This was a violation of his parole terms from the 1979 felonies, and he went back to prison.

Involvement in politics and the entertainment industry
After being released from federal prison in California, Paul moved to Los Angeles.

In 1985, Paul was appointed President of the California Bicentennial Foundation for the Constitution and Bill of Rights, a foundation designated by the California state legislature and governor to direct California's role in the Bicentennial celebration of the Constitution and Bill of Rights.

In 1987, Paul's efforts on behalf of the Foundation were derided in the Los Angeles Times, in part because the commission was selling a book that described blacks using the slur "pickaninnies", and declared enslavers "the worst victims of slavery", and in part because Paul referred to the founding fathers of the United States as "39 sweaty old men arguing in Philadelphia", and his remark that most Californians weren't able to understand the 18th-century language in the constitution anyway.

In 1988, Chief Justice Warren Burger had commended Paul for his efforts in a letter that read in part, "We commend you for the many contributions you have made during the national commemoration of the Constitution's 200th anniversary."

Paul became a business manager for, or otherwise involved with several celebrities, including becoming manager for a time of romance-novel icon Fabio.

Hillary Clinton's senatorial campaign
Paul emerged in 2000 as the largest contributor to Senatorial candidate Hillary Clinton. Paul and his attorneys have at various times offered two explanations for this. First, that he was trying to attract her husband, then-President Bill Clinton, to serve on the board of Stan Lee Media after leaving office. Second, that he hoped to negotiate a pardon for his previous criminal convictions. Paul produced the event in Los Angeles, days before the 2000 Democratic Convention began. The Hollywood Farewell Gala Salute to President William Jefferson Clinton featured prominent entertainers singing for the President, while raising over $1 million for Hillary Clinton's Senate campaign. The event cost $1.9 million to organize according to Paul and $500,000 according to the Federal Election Commission filing, much of it borrowed fraudulently by Paul from Merrill Lynch. Later indictments would state that Merrill Lynch lost about $5 million it had lent to Paul.

Two days after the gala, the Washington Post publicized Paul's criminal record, and Hillary Clinton denied knowing Paul and "vowed not to take any contributions from him". Through her spokesman, Howard Wolfson, Hillary stated on August 16, 2000, that she would return $2,000 she reported receiving from Paul in June 2000.

Paul alleged that Clinton was deceitful in this, and retained public interest law firm, and frequent Clinton opponent, Judicial Watch to represent him in a series of civil and criminal lawsuits against the Clintons, the Clinton campaign, and ultimately the Federal Election Commission (which he charged was negligent in failing to convict Mrs. Clinton). These charges were delayed, as courts held that Paul could not bring charges against the Clintons as he fought extradition from Brazil (to which he had fled in 2001 to escape Stan-Lee-Media-related criminal charges, see below), but proceeded once he was returned to the States.

In March 2005, Paul had a falling out with his advocates at Judicial Watch. He accused them of using his name to raise more than $15 million from people who disliked the Clintons, while doing little to advance his case. He announced his plan to replace them with a "dream team" of Republican lawyers, and in February 2007, he filed suit against them, saying that they had taken advantage of him and that he was "not a big fan of their behavior".

Regardless, Paul's claims have not found traction. An audit by the Federal Elections Commission found that neither Senator Clinton nor her Senate campaign had accepted any illegal funds in connection with the Hollywood fundraiser, though the campaign was asked to pay $35,000 in fines for having under-reported the cost of the party. Paul's suit against the FEC was thrown out; his attempt to bring ethics charges against Clinton was rejected, and his fraud charges against Senator Clinton were tossed out in April 2006. Paul continued to press civil charges against Senator Clinton and former President Clinton for "looting" his business, but the courts refused to allow him to sue Senator Clinton, with the appellate court specifying that her behavior had been "perfectly legal", and allowing her to recoup her legal fees from Paul. His charges against former President Clinton were tossed by Superior Court Judge Aurelio Munoz in December 2008, who ruled that Paul had waited too long to bring his claims.

Finding no luck in the courts, in 2007 Paul promoted a thirteen and a half minute video titled "Hillary Exposed: The Case of Paul v. Clinton," seeking to expose Senator Clinton. Her office responded "Peter Paul is a professional liar who has four separate criminal convictions, two for fraud. His video repackages a series of seven-year-old false claims about Senator Clinton that have already been rejected by the California state courts, the Justice Department, the Federal Election Commission, and the Senate Ethics Committee."

In January 2008, he re-filed his complaint with the FEC., seeking $41.9 million in damages.

Involvement with Fabio
Peter F. Paul was the manager of Italian model, actor, and author Fabio Lanzoni, helping him achieve international recognition.

When they began working together, Paul "suggested building Fabio's career around [Fabio's] philosophy," packaging products that incorporate his romantic approach to health and fitness. In 1993, Lanzoni was working 17 to 18 hours a day, claiming he could count the number of days he had off that year.

In 1993, he published Fabio's biography, Fabio. It contains over 100 photographs, presumably of Fabio. Lanzoni included Paul in the dedication to his 1995 book Fabio Fitness, though Paul was terminated shortly thereafter.

Founding of Stan Lee Media, fraud, and flight
In 1998, Paul co-founded Stan Lee Media with comic book legend Stan Lee and took the company public via a reverse-merger into a trading shell in August 1999.

In February 2000, in the midst of the Internet stock market boom, Stan Lee Media built a 165-person studio. However, at the end of the year, Stan Lee Media ran out of money. Paul alleged in a later civil fraud and coercion suit against Bill and Hillary Clinton that the company failed because of the intervention of Bill Clinton, who he claims persuaded a large investor not to further support the company.

In the aftermath of the company's collapse, it was alleged that Paul and a corporate officer named Stephan Gordon had illegally tried to support the stock's price by using nominee accounts to buy 1.6 million shares of the company's stock, attempting to pay for the stock with bad checks.

In February 2001, Stan Lee Media filed for bankruptcy, and Peter Paul fled to São Paulo, Brazil. There he managed 112 Interactive do Brazil, a seller of English language acquisition software, and fought extradition.

Stan Lee-related litigation
Paul has promoted lawsuits against Marvel Entertainment claiming that Stan Lee Media owns the rights to all the Marvel characters created by Stan Lee. These would include Spider-Man and The X-Men. Paul and his associates further claim that Stan Lee Media was never properly dissolved as a corporation, and that they control the company. Though courts have found that some Stan Lee Media characters were improperly transferred to Stan Lee's later company, Pow Entertainment, plaintiffs have not yet found traction with these broader claims, and Stan Lee himself has both publicly dismissed these claims and has engaged in a series of cross-suits with Stan Lee Media, Peter Paul, and his associates.

On March 3, 2008, Paul posted a message to his blog, subsequently reposted by one or more unknown parties verbatim on other websites,   in which he claimed that Stan Lee helped disguise the origin of Paul's unreported donations to Hillary Clinton, and that he (Paul) has a video tape of Lee admitting to this subterfuge. Lee responded with a lawsuit against Paul, claiming defamation.

Securities fraud conviction and jail terms
On June 12, 2001, Paul was indicted on one count of violating SEC Reg. 10(b)5, for manipulating the price of the stock in Stan Lee Media. On August 3, 2001, Paul was arrested in Brazil and jailed, pending the outcome of extradition proceedings. Paul failed in his efforts to avoid extradition and, in September 2003, he was delivered to the Metropolitan Detention Facility in Brooklyn, New York, for arraignment and trial.

In August 2004, the SEC formally filed its complaint against Paul for the manipulation of Stan Lee Media's stock in violation of the antifraud provisions of Section 17(a) of the Securities Act of 1933, Section 10(b) of the Securities Exchange Act, and SEC Rule 10b-5. Paul pleaded guilty to the securities fraud charge. The government characterized his conduct as causing "losses to the investing public and financial institutions of approximately $25 million". In July 2005, he settled related civil charges, consenting to a permanent injunction against ever serving as an officer or director of any reporting company. He pleaded poverty and, as a result, was not asked to pay any fine. He then spent four years under house arrest, wearing an "ankle bracelet".

In July 2009, Paul accepted a plea bargain and was sentenced to ten years in prison, and ordered to pay over $11 million in restitution to Merrill Lynch and Spear, Leeds & Kellogg. He self-surrendered on September 30, 2009, but subsequently tried to have the plea bargain annulled, claiming that the judge coerced him into agreeing to the deal. In March 2011, the courts rejected this attempt, and Paul continued to serve his 10-year imprisonment term as inmate number 78802-012. He was imprisoned at the Federal Correctional Institution, La Tuna in Anthony, Texas, until he was paroled on December 24, 2014.

title: Peter F. Paul


text:
Wikipedia:Articles for deletion/Best Video Game Ever

 This page is an archive of the discussion about the proposed deletion of the article below. This page is no longer live. Further comments should be made on the article's talk page rather than here so that this page is preserved as an historic record. The result of the debate was DELETE. jni 15:24, 26 Feb 2005 (UTC)

Best Video Game Ever
Fork of NiGHTS Into Dreams. --BM 14:00, 20 Feb 2005 (UTC)

This page is now preserved as an archive of the debate and, like some other VfD subpages, is no longer 'live'. Subsequent comments on the issue, the deletion, or the decision-making process should be placed on the relevant 'live' pages. Please do not edit this page.
 * Delete -- NPOV problematic title. Content exists elsewhere. Longhair 14:24, 20 Feb 2005 (UTC)
 * Delete - article forks are bad, name is awful, redirect would be useless. -- Cyrius|✎ 19:42, 20 Feb 2005 (UTC)
 * Delete. The title "Best Video Game Ever" will always lead to a POV article. Zzyzx11 19:53, 20 Feb 2005 (UTC)
 * Delete. Redundant article, title is inherently POV.   — Gwalla | Talk 02:39, 21 Feb 2005 (UTC)
 * Delete. POV. vlad_mv 04:51, 21 Feb 2005 (UTC)
 * Delete. It's a good article about NiGHTS Into Dreams on its own right, but calling it (or any game, for that matter) the "Best Video Game Ever" is a blatant violation of NPOV. 193.167.132.66 07:32, 21 Feb 2005 (UTC)
 * Delete. Right. I'm not even dure what I was THINKING when I did that. It's gone. — unsigned vote by User:69.141.8.245 (contribs); same IP as page author
 * Delete. At one point I put up a question in vfd's discussion as to why people are so willing to delete rather than redirect duplicates. This is not an example of what I had in mind. What I had in mind were titles which may be useful redirects. This title is not useful and can safely be deleted. I have a hunch that this article may be an experiment. 129.177.61.123 10:12, 23 Feb 2005 (UTC)


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Emmanuel Borlaza

Emmanuel "Maning" H. Borlaza (November 5, 1935 – October 11, 2017) was a Filipino movie screenwriter and director.

Early life
Born Emmanuel H. Borlaza on November 5, 1935, in Manila.

Career
Borlaza co-wrote and starred in the 1965 film Iginuhit ng Tadhana (The Ferdinand E. Marcos Story).

Borlaza has directed more than 20 films which starred Vilma Santos, including Dyesebel, Darna and the Giants, Lipad, Darna, Lipad!

He also helmed the films of Sharon Cuneta, namely Bukas Luluhod ang Mga Tala, Bituing Walang Ningning, and Dapat Ka Bang Mahalin?

Borlaza directed Eva Fonda 16 starring Alma Moreno and Snooky Serna's Blusang Itim. He was also the director of Dyesebel starring Charlene Gonzales in 1996.

Aside from being vice chairman of the Movie and Television Review and Classification Board, Borlaza also became chairperson of the Directors' Guild of the Philippines, Inc.

Borlaza's last directorial stint was for the film To Saudi with Love starring Dawn Zulueta, Alice Dixon, and Tonton Gutierrez in 1997.

title: Emmanuel Borlaza


text:
Michael Llewelyn Davies

Michael Llewelyn Davies (16 June 1900 – 19 May 1921) was – along with his four brothers – the inspiration for J. M. Barrie's characters Peter Pan, the Darling brothers, and the Lost Boys. Late in life, his only surviving brother Nico described him as "the cleverest of us, the most original, the potential genius." He died in ambiguous circumstances, drowning with a close friend – and possible lover – just short of his 21st birthday. He was a first cousin of English writer Daphne du Maurier.

Early life and Peter Pan
Michael was the fourth of five sons of Arthur and Sylvia Llewelyn Davies. He was born three years after Barrie became friends with his older brothers and mother in 1897. He and his eldest brother George were the boys closest to Barrie, and he is widely reported as the individual who most influenced the portrayal of Peter Pan in the 1911 novel based on the play. He was an infant as Barrie was writing the first appearance of Peter Pan as a newborn in The Little White Bird. He was four-and-a-half-years-old when Peter Pan, or The Boy Who Wouldn't Grow Up debuted in December 1904. The following winter, he was ill for several months, so in February 1906, Barrie and producer Charles Frohman brought scenery and some of the cast to the family's home in Berkhamsted to perform the play for him. Barrie began writing a sequel to Peter Pan about the boy's brother, to be entitled Michael Pan, but instead incorporated this material (such as the hero's nightmares) into the novel Peter and Wendy.

The statue of Peter Pan in Kensington Gardens, erected in secret during the night of 30 April 1912, was meant to be modelled upon photographs of Michael Llewelyn Davies at the age of six, dressed as the character. However, sculptor George Frampton used a different child as his model, leaving Barrie very disappointed with the result. "It doesn't show the devil in Peter," the writer said.

Barrie became guardian of Davies and his brothers following the deaths of their father in 1907 and mother in 1910. Davies and Barrie remained very close as Davies grew up and went away to school, particularly after his eldest brother George died in combat in Flanders during World War I in 1915. His youngest brother Nico later described Michael and George as "the Ones", the boys who meant the most to Barrie. Davies attended Eton College, where he had difficulty adjusting to life away from his family, and he exchanged letters daily with "Uncle Jim" Barrie. He also suffered from nightmares, which he had experienced since childhood. Nonetheless, he made a number of friends and excelled at his studies, including art and writing poetry, and was generally described as a "brilliant boy", one destined for great things.

Adulthood

After finishing at Eton, Davies attended Christ Church, Oxford, where he continued to correspond regularly with Barrie. He briefly decided to study art at the University of Paris, but returned to Oxford. Several friends from Eton joined him there, but he also became very close to Rupert Buxton, the son of Sir Thomas Fowell Victor Buxton, 4th Baronet and a former pupil of Harrow School. The two became inseparable friends, spending time both at the university and on holiday together. Buxton was also a poet, and had an interest in acting. Buxton was one of the few friends of Davies whom Barrie reported getting along with.

In an interview taped in 1976, Conservative politician Robert Boothby, who had been a close friend of Davies at Eton and Oxford, spoke about Davies' relationships during this time. When asked if Davies were homosexual, Boothby – who was reported by newspapers to have had homosexual relationships as an adult – replied it was "a phase... I think he might have come out of it." Boothby also said, "I don't think Michael had any girlfriends, but our friendship wasn't homosexual. I believe it was – fleetingly – between him and Senhouse". (Roger Senhouse was a friend of Davies at both Eton and Oxford.) Boothby reported that he had discouraged Davies' relationship with Buxton, warning of "a feeling of doom" he had about him. Although Boothby criticised the relationship between Davies and his surrogate father Barrie as "morbid" and "unhealthy", he dismissed the notion that there was a sexual aspect to it. However, he admitted that there had been a sexual relationship between Davies and Buxton.

Death
About a month before Davies's 21st birthday, he and Buxton drowned together in Sandford Lasher, a pool of water downstream of a weir near Sandford Lock on the River Thames, a few miles from Oxford.

The closeness of Davies and Buxton, combined with the uncertain circumstances of their deaths, led to speculation that the pair had died in a suicide pact. Dangerous currents in Sandford Lasher had made the pool notorious as a drowning hazard – there were warning signs and a conspicuous 19th century memorial to previous victims. Despite this, the pair had gone swimming there before.

The water was 20 to 30 ft deep, but calm. Buxton was a good swimmer, but Davies had a fear of water and could not swim proficiently. A witness at the coroner's inquest reported that one man was swimming to join the other, who was sitting on a stone on the weir, but he experienced "difficulties" and the other dived in to reach him. However, the witness also reported, when he saw their heads together in the water they did not appear to be struggling. Their bodies were recovered "clasped" together the next day (sometimes misreported later as "tied together"). The coroner's conclusion was Davies had drowned accidentally, and Buxton had drowned trying to save him.

The Oxford Magazine published the following in an obituary for the pair: "Two House men whose loss would have been more widely and more deeply mourned, it would be impossible to find. They were intimate friends, and in their death they were not divided. It is we who must learn to live without them." Barrie wrote a year later that Davies's death "was in a way the end of me."

Davies's brothers Peter and Nico each later acknowledged suicide as a likely explanation, as did Barrie. Although Boothby, in 1976, described Buxton as having "an almost suicidal streak about him," he did not take a definite stand on whether Buxton had died trying to save Davies and/or impulsively joined him going under, or whether they had in fact died as the result of a suicide pact.

In media
In the 1978 BBC mini-series The Lost Boys, he is portrayed at various ages by Sebastian Buss, Paul Spurrier, Alexander Buss, Charles Tatnall, and William Relton.

The 1988 play The Death of Peter Pan (by Australian playwright Barry Lowe) is based on Davies's life and focuses on his relationship with Rupert Buxton.

In the 2004 film Finding Neverland, he is portrayed by Luke Spill.

In the 2013 play "Peter and Alice", he appears in a scene with Barrie, who disapproves of Davies's relationship with Buxton. Shortly after, Davies commits suicide. He is portrayed by Stefano Braschi.

title: Michael Llewelyn Davies