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the sloan digital sky survey sdss this allows des to obtain photometric redshift measurements to z 1 decam also contains five lenses acting as corrector optics to extend the telescope s field of view to a diameter of 2 2 one of the widest fields of view available for ground based optical and infrared imaging 6 one significant difference between previous charge coupled devices ccd at the victor m blanco telescope and decam is the improved quantum efficiency in the red and near infrared wavelengths 11 9 ccds edit the dark energy camera s 1 millionth exposure the 1 millionth exposure has been combined with 127 earlier exposures to make this view of the field the scientific sensor array on decam is an array of 62 2048 4096 pixel back illuminated ccds totaling 520 megapixels an additional 12 2048 2048 pixel ccds 50 mpx are used for guiding the telescope monitoring focus and alignment the full decam focal plane contains 570 megapixels the ccds for decam use high resistivity silicon manufactured by dalsa and lbnl with 15 15 micron pixels by comparison the omnivision technologies back illuminated ccd that was used in the iphone 4 has a 1 75 1 75 micron pixel with 5 megapixels the larger pixels allow decam to collect more light per pixel improving low light sensitivity which is desirable for an astronomical instrument decam s ccds also have a 250 micron crystal depth this is significantly larger than most consumer ccds the additional crystal depth increases the path length travelled by entering photons this in turn increases the probability of interaction and allows the ccds to have an increased sensitivity to lower energy photons extending the wavelength range to 1050 nm scientifically this is important because it allows one to look for objects at a higher redshift increasing statistical power in the studies mentioned above when placed in the telescope s focal plane each pixel has a width of 0 27 on the sky resulting in a total field of view of 3 square degrees 12 survey edit des imaged 5 000 square degrees of the southern sky in a footprint that overlaps with the south pole telescope and stripe 82 in large part avoiding the milky way the survey took 758 observing nights spread over six annual sessions between august and february to complete covering the survey footprint ten times in five photometric bands g r i z and y 13 the survey reached a depth of 24th magnitude in the i band over the entire survey area longer exposure times and faster observing cadence were made in five smaller patches totaling 30 square degrees to search for supernovae 14 first light was achieved on 12 september 2012 15 after a verification and testing period scientific survey observations started in august 2013 16 the last observing session was completed on 9 january 2019 13 other surveys using decam edit after completion of the dark energy survey the dark energy camera was used for other sky surveys dark energy camera legacy survey decals covers the sky below 32 declination not including the milky way this survey covers over 9000 square degrees 17 18 the desi legacy imaging surveys legacy surveys as of data release 10 includes decals bass and mzls it also incorporating additional decam data which means that it covers almost the entire extragalactic southern sky including parts of the magellanic clouds the purpose of the legacy surveys is to find targets for the dark energy spectroscopic instrument 18 19 dark energy camera plane survey decaps covers the milky way in the southern sky 20 simulated image of the decam ccd array at focal plane each large rectangle is a single ccd the green rectangle circled in red in the upper left corner shows the size of the iphone 4 camera ccd at the same scale observing edit the footprint of the wide area survey on the sky colored region in celestial coordinates the dashed curve shows the approximate location of the milky way disk in these coordinates each year from august through february observers will stay in dormitories on the mountain during a weeklong period of work observers sleep during the day and use the telescope and camera at night there will be some des members working at the telescope console to monitor operations while others are monitoring camera operations and data process for the wide area footprint observations des takes roughly two minutes for each new image the exposures are typically 90 seconds long with another 30 seconds for readout of the camera data and slewing to point the telescope at its next target despite the restrictions on each exposure the team also need to consider different sky conditions for the observations such as moonlight and cloud cover in order to get better images des team use a computer algorithm called the observing tactician obstac to help with sequencing observations it optimizes among different factors such as the date and time weather conditions and the position of the moon obstac automatically points the telescope in the best direction and selects the exposure using the best light filter it also decides whether to take a wide area or time domain survey image depending on whether or not the exposure will also be used for supernova searches 21 results edit cosmology edit constraints on a measure of the clumpiness of the matter distribution s8 and the fractional density of the universe in matter ωm from the combined 3 des y1 measurements blue planck cmb measurements green and their combination red dark energy group published several papers presenting their results for cosmology most of these cosmology results coming from its first year data and the third year data their results for cosmology were concluded with a multi probe methodology which mainly combine the data from galaxy galaxy lensing different shape of weak lensing cosmic shear galaxy clustering and photometric data set for the first year data collected by des dark energy survey group showed the cosmological constraints results from galaxy clustering and weak lensing results and cosmic shear measurement with galaxy clustering and weak lensing results s 8 σ 8 ω m 0 3 0 5 0 773 0 020 0 026 displaystyle s_ 8 sigma _ 8 omega _ m 0 3 0 5 0 773_ 0 020 0 026 and ω m 0 267 0 017 0 030 displaystyle omega _ m 0 267_ 0 017 0 030 for λcdm s 8 0 782 0 024 0 036 displaystyle s_ 8 0 782_ 0 024 0 036 ω m 0 284 0 030 0 033 displaystyle omega _ m 0 284_ 0 030 0 033 and ω 0 82 0 20 0 21 displaystyle omega 0 82_ 0 20 0 21 at 68 confidence limits for ωcmd 22 combine the most significant measurements of cosmic shear in a galaxy survey dark energy survey group showed that σ 8 ω m 0 3 0 5 0 782 0 027 0 027 displaystyle sigma _ 8 omega _ m 0 3 0 5 0 782_ 0 027 0 027 at 68 confidence limits and σ 8 ω m 0 3 0 5 0 777 0 038 0 036 displaystyle sigma _ 8 omega _ m 0 3 0 5 0 777_ 0 038 0 036 for λcdm with ω 0 95 0 36 0 33 displaystyle omega 0 95_ 0 36 0 33 23 other cosmological analyses from first year data showed a derivation and validation of redshift distribution estimates and their uncertainties for the galaxies used as weak lensing sources 24 the des team also published a paper summarize all the photometric data set for cosmology for their first year data 25 for the third year data collected by des they updated the cosmological constraints to σ 8 ω m 0 3 0 5 0 759 0 025 0 023 displaystyle sigma _ 8 omega _ m 0 3 0 5 0 759_ 0 025 0 023 for the λcdm model with the new cosmic shear measurements 26 from third year data of galaxy clustering and weak lensing results des updated the cosmological constraints to s 8 σ 8 ω m 0 3 0 5 0 776 0 017 0 017 displaystyle s_ 8 sigma _ 8 omega _ m 0 3 0 5 0 776_ 0 017 0 017 and ω m 0 339 0 031 0 032 displaystyle omega _ m 0 339_ 0 031 0 032 in λcdm at 68 confidence limits s 8 σ 8 ω m 0 3 0 5 0 775 0 024 0 026 displaystyle s_ 8 sigma _ 8 omega _ m 0 3 0 5 0 775_ 0 024 0 026 ω m 0 352 0 041 0 035 displaystyle omega _ m 0 352_ 0 041 0 035 and ω 0 98 0 20 0 32 displaystyle omega 0 98_ 0 20 0 32 in ωcdm at 68 confidence limits 27 similarly the des team published their third year observations for photometric data set for cosmology comprising nearly 5000 deg2 of grizy imaging in the south galactic cap including nearly 390 million objects with depth reaching s n 10 for extended objects up to i a b displaystyle i_ ab 23 0 and top of the atmosphere photometric uniformity 3mmag 28 weak lensing edit des s 2021 dark matter map 29 30 using weak gravitational lensing data set projected in the foreground of observed galaxies weak lensing was measured statistically by measuring the shear shear correlation function a two point function or its fourier transform the shear power spectrum 31 in april 2015 the dark energy survey released mass maps using cosmic shear measurements of about 2 million galaxies from the science verification data between august 2012 and february 2013 32 in 2021 weak lensing was used to map the dark matter in a region of the southern hemisphere sky 29 30 in 2022 together with galaxy clustering data to give new cosmological constrains 33 34 and in 2023 with data from the planck telescope and south pole telescope to give once new improved constraints 35 36 37 38 another big part of weak lensing result is to calibrate the redshift of the source galaxies in december 2020 and june 2021 des team published two papers showing their results about using weak lensing to calibrate the redshift of the source galaxies in order to mapping the matter density field with gravitational lensing 39 40 gravitational waves edit after ligo detected the first gravitational wave signal from gw170817 41 des made follow up observations of gw170817 using decam with decam independent discovery of the optical source des team establish its association with gw170817 by showing that none of the 1500 other sources found within the event localization region could plausibly be associated with the event des team monitored the source for over two weeks and provide the light curve data as a machine readable file from the observation data set des concluded that the optical counterpart they have identified near ngc 4993 is associated with gw170817 this discovery ushers in the era of multi messenger astronomy with gravitational waves and demonstrates the power of decam to identify the optical counterparts of gravitational wave sources 42 dwarf galaxies edit spiral galaxy ngc 895 imaged by des in march 2015 two teams released their discoveries of several new potential dwarf galaxy candidates found in year 1 des data 43 in august 2015 the dark energy survey team announced the discovery of eight additional candidates in year 2 des data 44 later on dark energy survey team found more dwarf galaxies with more dwarf galaxy results the team was able to take a deep look about more properties of the detected dwarf galaxy such as the chemical abundance 45 the structure of stellar population 46 and stellar kinematics and metallicities 47 in feb 2019 the team also discovered a sixth star cluster in the fornax dwarf spheroidal galaxy 48 and a tidally disrupted ultra faint dwarf galaxy 49 baryon acoustic oscillations edit the signature of baryon acoustic oscillations bao can be observed in the distribution of tracers of the matter density field and used to measure the expansion history of the universe bao can also be measured using purely photometric data though at less significance 50 des team observation samples consists of 7 million galaxies distributed over a footprint of 4100 deg 2 with 0 6 z photo 1 1 and a typical redshift uncertainty of 0 03 1 z 51 from their statistics they combine the likelihoods derived from angular correlations and spherical harmonics to constrain the ratio of comoving angular diameter distance d m z eff 0 835 r d 18 92 0 51 displaystyle d_ m z_ text eff 0 835 r_ d 18 92 pm 0 51 at the effective redshift of our sample to the sound horizon scale at the drag epoch 52 the supernova remnant g299 2 2 9 type ia supernova observations edit in may 2019 dark energy survey team published their first cosmology results using type ia supernovae the supernova data was from des sn3yr the dark energy survey team found ωm 0 331 0 038 with a flat λcdm model and ωm 0 321 0 018 w 0 978 0 059 with a flat wcdm model 53 analyzing the same data from des sn3yr they also found a new current hubble constant h 0 67 1 1 3 k m s 1 m p c 1 displaystyle h_ 0 67 1 pm 1 3 mathrm km s 1 mpc 1 54 this result has an excellent agreement with the hubble constant measurement from planck satellite collaboration in 2018 55 in june 2019 there a follow up paper was published by des team discussing the systematic uncertainties and validation of using the supernovae to measure the cosmology results mentioned before 56 the team also published their photometric pipeline and light curve data in another paper published in the same month 57 minor planets edit several minor planets were discovered by decam in the course of the dark energy survey including high inclination trans neptunian objects tnos 58 list of des discovered minor planets numbered mp designation discovery date mp list link ref 451657 2012 wd 36 19 november 2012 list 59 471954 2013 rm 98 8 september 2013 list 60 472262 2014 qn 441 18 august 2014 list 61 483002 2014 qs 441 19 august 2014 list 62 491767 2012 vu 113 15 november 2012 list 63 491768 2012 vv 113 15 november 2012 list 64 495189 2012 vr 113 28 september 2012 list 65 495190 2012 vs 113 12 november 2012 list 66 495297 2013 tj 159 13 october 2013 list 67 discoveries are credited either to decam or dark energy survey the mpc has assigned the iau code w84 for decam s observations of small solar system bodies as of october 2019 the mpc inconsistently credits the discovery of nine numbered minor planets all of them trans neptunian objects to either decam or dark energy survey 68 the list does not contain any unnumbered minor planets potentially discovered by decam as discovery credits are only given upon a body s numbering which in turn depends on a sufficiently secure orbit determination gallery edit dark energy survey deep field image 69 the large spiral galaxy in the center of this image is roughly 385 million light years from earth the three large objects in this image captured by the dark energy camera are galaxies in the nearby fornax cluster roughly 65 million light years from earth dark energy survey galaxy ngc 1398 see also edit cosmic evolution survey dark energy spectroscopic instrument desi references edit home the dark energy survey des collaboration page des collaborators des brazil archived 2014 10 22 at the wayback machine des brazil consortium the dark energy survey collaboration www darkenergysurvey org retrieved 2015 11 21 the project the dark energy survey collaboration the des project site 1 2 3 dark energy camera decam archived 2019 05 23 at the wayback machine cerro tololo inter american observatory des year 3 cosmology results papers the dark energy survey retrieved 3 august 2021 a sky full of galaxies noirlab retrieved 12 march 2021...
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