Dark Energy Survey

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The Dark Energy Survey
Dark Energy Survey logo.jpg
Dark Energy Survey logo
Alternative namesDES
Website www.darkenergysurvey.org
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The Dark Energy Survey (DES) is an astronomical survey designed to constrain the properties of dark energy. It uses images taken in the near-ultraviolet, visible, and near-infrared to measure the expansion of the universe using Type Ia supernovae, baryon acoustic oscillations, the number of galaxy clusters, and weak gravitational lensing. [1] The collaboration is composed of research institutions and universities from the United States, [2] Australia, Brazil, [3] the United Kingdom, Germany, Spain, and Switzerland. The collaboration is divided into several scientific working groups. The director of DES is Josh Frieman. [4]

Contents

The DES began by developing and building Dark Energy Camera (DECam), an instrument designed specifically for the survey. [5] This camera has a wide field of view and high sensitivity, particularly in the red part of the visible spectrum and in the near infrared. [6] Observations were performed with DECam mounted on the 4-meter Víctor M. Blanco Telescope, located at the Cerro Tololo Inter-American Observatory (CTIO) in Chile. [6] Observing sessions ran from 2013 to 2019; as of 2021 the DES collaboration has published results from the first three years of the survey. [7]

DECam

A Sky Full of Galaxies. A Sky Full of Galaxies.jpg
A Sky Full of Galaxies.

DECam, short for the Dark Energy Camera, is a large camera built to replace the previous prime focus camera on the Victor M. Blanco Telescope. The camera consists of three major components: mechanics, optics, and CCDs.

Mechanics

The mechanics of the camera consists of a filter changer with an 8-filter capacity and shutter. There is also an optical barrel that supports 5 corrector lenses, the largest of which is 98 cm in diameter. These components are attached to the CCD focal plane which is cooled to 173 K (−148 °F; −100 °C) with liquid nitrogen in order to reduce thermal noise in the CCDs. The focal plane is also kept in an extremely low vacuum of 0.00013 pascals (1.3×10−9 atm) to prevent the formation of condensation on the sensors. The entire camera with lenses, filters, and CCDs weighs approximately 4 tons. When mounted at the prime focus it was supported with a hexapod system allowing for real time focal adjustment. [9]

Optics

The camera is outfitted with u, g, r, i, z, and Y filters spanning roughly from 340–1070 nm, [10] similar to those used in 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

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. Dark Energy Camera's 1 millionth exposure.jpg
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

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

After completion of the Dark Energy Survey, the Dark Energy Camera was used for other sky surveys:

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. DECam iphone insert.PNG
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

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. DES Observing Footprint.png
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 every 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

Cosmology

Constraints on a measure of the clumpiness of the matter distribution (S8) and the fractional density of the Universe in matter (Om) from the combined 3 DES Y1 measurements (blue), Planck CMB measurements (green), and their combination (red). DES clumpiness of the matter distribution.png
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, and for ΛCDM, , and 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 at 68% confidence limits and for ΛCDM with . [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 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 and in ΛCDM at 68% confidence limits, , and 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 ~ 23.0, and top-of-the-atmosphere photometric uniformity < 3mmag. [28]

Weak lensing

DES's 2021 Dark matter map using weak gravitational lensing data set projected in the foreground of observed galaxies. DESDMmap2021.png
DES's 2021 Dark matter map 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

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

Spiral Galaxy NGC 895 imaged by DES Dark Energy Survey - Spiral galaxy NGC 0895 (14935678296).jpg
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

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 deg2 with 0.6 < zphoto < 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 at the effective redshift of our sample to the sound horizon scale at the drag epoch. [52]

The supernova remnant G299.2-2.9 G299-Remnants-SuperNova-Type1a-20150218.jpg
The supernova remnant G299.2-2.9

Type Ia supernova observations

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, . [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

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 linkRef
[[(451657) 2012 WD36|(451657) 2012 WD

36]]

19 November 2012 list [59]
[[(471954) 2013 RM98|(471954) 2013 RM

98]]

8 September 2013 list [60]
[[(472262) 2014 QN441|(472262) 2014 QN

441]]

18 August 2014 list [61]
[[(483002) 2014 QS441|(483002) 2014 QS

441]]

19 August 2014 list [62]
[[(491767) 2012 VU113|(491767) 2012 VU

113]]

15 November 2012 list [63]
[[(491768) 2012 VV113|(491768) 2012 VV

113]]

15 November 2012 list [64]
[[(495189) 2012 VR113|(495189) 2012 VR

113]]

28 September 2012 list [65]
[[(495190) 2012 VS113|(495190) 2012 VS

113]]

12 November 2012 list [66]
[[(495297) 2013 TJ159|(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.

See also

Related Research Articles

<span class="mw-page-title-main">Physical cosmology</span> Branch of cosmology which studies mathematical models of the universe

Physical cosmology is a branch of cosmology concerned with the study of cosmological models. A cosmological model, or simply cosmology, provides a description of the largest-scale structures and dynamics of the universe and allows study of fundamental questions about its origin, structure, evolution, and ultimate fate. Cosmology as a science originated with the Copernican principle, which implies that celestial bodies obey identical physical laws to those on Earth, and Newtonian mechanics, which first allowed those physical laws to be understood.

<span class="mw-page-title-main">Dark matter</span> Concept in cosmology

In astronomy, dark matter is a hypothetical form of matter that appears not to interact with light or the electromagnetic field. Dark matter is implied by gravitational effects which cannot be explained by general relativity unless more matter is present than can be seen. Such effects occur in the context of formation and evolution of galaxies, gravitational lensing, the observable universe's current structure, mass position in galactic collisions, the motion of galaxies within galaxy clusters, and cosmic microwave background anisotropies.

<span class="mw-page-title-main">Redshift</span> Change of wavelength in photons during travel

In physics, a redshift is an increase in the wavelength, and corresponding decrease in the frequency and photon energy, of electromagnetic radiation. The opposite change, a decrease in wavelength and increase in frequency and energy, is known as a blueshift, or negative redshift. The terms derive from the colours red and blue which form the extremes of the visible light spectrum. The main causes of electromagnetic redshift in astronomy and cosmology are the relative motions of radiation sources, which give rise to the relativistic Doppler effect, and gravitational potentials, which gravitationally redshift escaping radiation. All sufficiently distant light sources show cosmological redshift corresponding to recession speeds proportional to their distances from Earth, a fact known as Hubble's law that implies the universe is expanding.

<span class="mw-page-title-main">Accelerating expansion of the universe</span> Cosmological phenomenon

Observations show that the expansion of the universe is accelerating, such that the velocity at which a distant galaxy recedes from the observer is continuously increasing with time. The accelerated expansion of the universe was discovered in 1998 by two independent projects, the Supernova Cosmology Project and the High-Z Supernova Search Team, which used distant type Ia supernovae to measure the acceleration. The idea was that as type Ia supernovae have almost the same intrinsic brightness, and since objects that are farther away appear dimmer, the observed brightness of these supernovae can be used to measure the distance to them. The distance can then be compared to the supernovae's cosmological redshift, which measures how much the universe has expanded since the supernova occurred; the Hubble law established that the farther away that an object is, the faster it is receding. The unexpected result was that objects in the universe are moving away from one another at an accelerating rate. Cosmologists at the time expected that recession velocity would always be decelerating, due to the gravitational attraction of the matter in the universe. Three members of these two groups have subsequently been awarded Nobel Prizes for their discovery. Confirmatory evidence has been found in baryon acoustic oscillations, and in analyses of the clustering of galaxies.

<span class="mw-page-title-main">Hubble's law</span> Observation in physical cosmology

Hubble's law, also known as the Hubble–Lemaître law, is the observation in physical cosmology that galaxies are moving away from Earth at speeds proportional to their distance. In other words, the farther they are, the faster they are moving away from Earth. The velocity of the galaxies has been determined by their redshift, a shift of the light they emit toward the red end of the visible light spectrum. The discovery of Hubble's law is attributed to Edwin Hubble's work published in 1929.

<span class="mw-page-title-main">Observable universe</span> All of space observable from the Earth at the present

The observable universe is a ball-shaped region of the universe consisting of all matter that can be observed from Earth or its space-based telescopes and exploratory probes at the present time; the electromagnetic radiation from these objects has had time to reach the Solar System and Earth since the beginning of the cosmological expansion. Initially, it was estimated that there may be 2 trillion galaxies in the observable universe. That number was reduced in 2021 to several hundred billion based on data from New Horizons. Assuming the universe is isotropic, the distance to the edge of the observable universe is roughly the same in every direction. That is, the observable universe is a spherical region centered on the observer. Every location in the universe has its own observable universe, which may or may not overlap with the one centered on Earth.

<span class="mw-page-title-main">Sunyaev–Zeldovich effect</span> Spectral distortion of cosmic microwave background in galaxy clusters

The Sunyaev–Zeldovich effect is the spectral distortion of the cosmic microwave background (CMB) through inverse Compton scattering by high-energy electrons in galaxy clusters, in which the low-energy CMB photons receive an average energy boost during collision with the high-energy cluster electrons. Observed distortions of the cosmic microwave background spectrum are used to detect the disturbance of density in the universe. Using the Sunyaev–Zeldovich effect, dense clusters of galaxies have been observed.

<span class="mw-page-title-main">Reionization</span> Process that caused matter to reionize early in the history of the Universe

In the fields of Big Bang theory and cosmology, reionization is the process that caused electrically neutral atoms in the universe to reionize after the lapse of the "dark ages".

<span class="mw-page-title-main">Age of the universe</span> Time elapsed since the Big Bang

In physical cosmology, the age of the universe is the time elapsed since the Big Bang. Astronomers have derived two different measurements of the age of the universe: a measurement based on direct observations of an early state of the universe, which indicate an age of 13.787±0.020 billion years as interpreted with the Lambda-CDM concordance model as of 2021; and a measurement based on the observations of the local, modern universe, which suggest a younger age. The uncertainty of the first kind of measurement has been narrowed down to 20 million years, based on a number of studies that all show similar figures for the age. These studies include researches of the microwave background radiation by the Planck spacecraft, the Wilkinson Microwave Anisotropy Probe and other space probes. Measurements of the cosmic background radiation give the cooling time of the universe since the Big Bang, and measurements of the expansion rate of the universe can be used to calculate its approximate age by extrapolating backwards in time. The range of the estimate is also within the range of the estimate for the oldest observed star in the universe.

<span class="mw-page-title-main">Lambda-CDM model</span> Model of Big Bang cosmology

The Lambda-CDM, Lambda cold dark matter, or ΛCDM model is a mathematical model of the Big Bang theory with three major components:

  1. a cosmological constant, denoted by lambda (Λ), associated with dark energy
  2. the postulated cold dark matter, denoted by CDM
  3. ordinary matter
<span class="mw-page-title-main">Redshift-space distortions</span>

Redshift-space distortions are an effect in observational cosmology where the spatial distribution of galaxies appears squashed and distorted when their positions are plotted as a function of their redshift rather than as a function of their distance. The effect is due to the peculiar velocities of the galaxies causing a Doppler shift in addition to the redshift caused by the cosmological expansion.

<span class="mw-page-title-main">South Pole Telescope</span> Telescope at the South Pole

The South Pole Telescope (SPT) is a 10-metre (390 in) diameter telescope located at the Amundsen–Scott South Pole Station, Antarctica. The telescope is designed for observations in the microwave, millimeter-wave, and submillimeter-wave regions of the electromagnetic spectrum, with the particular design goal of measuring the faint, diffuse emission from the cosmic microwave background (CMB). Key results include a wide and deep survey of discovering hundreds of clusters of galaxies using the Sunyaev–Zel'dovich effect, a sensitive 5 arcminute CMB power spectrum survey, and the first detection of B-mode polarized CMB.

<span class="mw-page-title-main">Atacama Cosmology Telescope</span> Telescope in the Atacama Desert, northern Chile

The Atacama Cosmology Telescope (ACT) was a cosmological millimeter-wave telescope located on Cerro Toco in the Atacama Desert in the north of Chile. ACT made high-sensitivity, arcminute resolution, microwave-wavelength surveys of the sky in order to study the cosmic microwave background radiation (CMB), the relic radiation left by the Big Bang process. Located 40 km from San Pedro de Atacama, at an altitude of 5,190 metres (17,030 ft), it was one of the highest ground-based telescopes in the world.

The Milky Way has several smaller galaxies gravitationally bound to it, as part of the Milky Way subgroup, which is part of the local galaxy cluster, the Local Group.

<span class="mw-page-title-main">Weak gravitational lensing</span>

While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.

<span class="mw-page-title-main">Dark energy</span> Energy driving the accelerated expansion of the universe

In physical cosmology and astronomy, dark energy is an unknown form of energy that affects the universe on the largest scales. Its primary effect is to drive the accelerating expansion of the universe. Assuming that the lambda-CDM model of cosmology is correct, dark energy is the dominant component of the universe, contributing 68% of the total energy in the present-day observable universe while dark matter and ordinary (baryonic) matter contribute 26% and 5%, respectively, and other components such as neutrinos and photons are nearly negligible. Dark energy's density is very low: 7×10−30 g/cm3, much less than the density of ordinary matter or dark matter within galaxies. However, it dominates the universe's mass–energy content because it is uniform across space.

<span class="mw-page-title-main">Ofer Lahav</span>

Ofer Lahav is Perren Chair of Astronomy at University College London (UCL), Vice-Dean (International) of the UCL Faculty of Mathematical and Physical Sciences (MAPS) and Co-Director of the STFC Centre for Doctoral Training in Data Intensive Science. His research area is Observational Cosmology, in particular probing Dark Matter and Dark Energy. His work involves Machine Learning for Big Data.

<span class="mw-page-title-main">Baryon acoustic oscillations</span> Fluctuations in the density of the normal matter of the universe

In cosmology, baryon acoustic oscillations (BAO) are fluctuations in the density of the visible baryonic matter of the universe, caused by acoustic density waves in the primordial plasma of the early universe. In the same way that supernovae provide a "standard candle" for astronomical observations, BAO matter clustering provides a "standard ruler" for length scale in cosmology. The length of this standard ruler is given by the maximum distance the acoustic waves could travel in the primordial plasma before the plasma cooled to the point where it became neutral atoms, which stopped the expansion of the plasma density waves, "freezing" them into place. The length of this standard ruler can be measured by looking at the large scale structure of matter using astronomical surveys. BAO measurements help cosmologists understand more about the nature of dark energy by constraining cosmological parameters.

<span class="mw-page-title-main">Peter Capak</span> Physicist

Peter Lawrence Capak is currently the Architect of Perception Systems at the Oculus division of Facebook. His current focus is developing machine perception technologies, sensors, displays, and compute architectures for the next generation of augmented (AR), mixed (MR) and virtual reality (VR) systems. His research has focused on using physical modeling and advanced statistical methods including artificial intelligence and machine learning to extract information from very large multi-wavelength (hyper-spectral) data sets. He has primarily used this to study structure formation in the universe, cosmology, and the nature of dark matter and dark energy.

References

  1. ↑ "Home". The Dark Energy Survey.
  2. ↑ DES Collaboration Page, DES Collaborators.
  3. ↑ DES-Brazil Archived 2014-10-22 at the Wayback Machine , DES-Brazil Consortium.
  4. ↑ "The Dark Energy Survey Collaboration". www.darkenergysurvey.org. Retrieved 2015-11-21.
  5. ↑ The Project - The Dark Energy Survey Collaboration, The DES Project Site.
  6. 1 2 3 Dark Energy Camera (DECam) Archived 2019-05-23 at the Wayback Machine , Cerro Tololo Inter-American Observatory.
  7. ↑ "DES Year 3 Cosmology Results: Papers". The Dark Energy Survey. Retrieved 3 August 2021.
  8. ↑ "A Sky Full of Galaxies". NOIRLab . Retrieved 12 March 2021.
  9. 1 2 DECam Presentation Archived 2011-09-27 at the Wayback Machine , Pdf Presentation about the specific details about how a CCD device works and about the specific properties of the DECam, made by a Fermilab specialist.
  10. ↑ "Camera | SDSS".
  11. ↑ Flaugher, Brenna L.; et al. (September 24, 2012). "Status of the Dark Energy Survey Camera (DECam) project". In McLean, Ian S; Ramsay, Suzanne K; Takami, Hideki (eds.). Ground-based and Airborne Instrumentation for Astronomy IV. Vol. 8446. International Society for Optics and Photonics. pp. 343–357. doi:10.1117/12.926216. S2CID   121613505 – via www.spiedigitallibrary.org.
  12. ↑ "The Camera". The Dark Energy Survey. Retrieved 2024-05-02.
  13. 1 2 "NOAO: A Survey Machine and a Data Trove – Dark Energy Survey's Rich Legacy | CTIO". www.ctio.noao.edu. Archived from the original on 22 September 2021. Retrieved 3 August 2021.
  14. ↑ Dark Energy Survey Collaboration. "Description of the Dark Energy Survey for Astronomers" (PDF). The Dark Energy Survey. Retrieved 1 March 2015.
  15. ↑ "Dark energy camera snaps first images ahead of survey". BBC. 2012-09-18.
  16. ↑ "The Dark Energy Survey begins". Fermilab. 2013-09-03.
  17. ↑ Survey, Legacy (2012-11-08). "The Dark Energy Camera Legacy Survey (DECaLS)". Legacy Survey. Retrieved 2023-12-31.
  18. 1 2 Dey, Arjun; Schlegel, David J.; Lang, Dustin; Blum, Robert; Burleigh, Kaylan; Fan, Xiaohui; Findlay, Joseph R.; Finkbeiner, Doug; Herrera, David; Juneau, Stéphanie; Landriau, Martin; Levi, Michael; McGreer, Ian; Meisner, Aaron; Myers, Adam D. (2019-05-01). "Overview of the DESI Legacy Imaging Surveys". The Astronomical Journal. 157 (5): 168. arXiv: 1804.08657 . Bibcode:2019AJ....157..168D. doi: 10.3847/1538-3881/ab089d . ISSN   0004-6256.
  19. ↑ Survey, Legacy (2023-09-28). "Data Release Description". Legacy Survey. Retrieved 2023-12-31.
  20. ↑ Schlafly, E. F.; Green, G. M.; Lang, D.; Daylan, T.; Finkbeiner, D. P.; Lee, A.; Meisner, A. M.; Schlegel, D.; Valdes, F. (2018-02-01). "The DECam Plane Survey: Optical Photometry of Two Billion Objects in the Southern Galactic Plane". The Astrophysical Journal Supplement Series. 234 (2): 39. arXiv: 1710.01309 . Bibcode:2018ApJS..234...39S. doi: 10.3847/1538-4365/aaa3e2 . ISSN   0067-0049.
  21. ↑ "Observations". The Dark Energy Survey. Survey and operations.
  22. ↑ DES Collaboration; Abbott, T. M. C.; Abdalla, F. B.; Alarcon, A.; Aleksić, J.; Allam, S.; Allen, S.; Amara, A.; Annis, J.; Asorey, J.; Avila, S. (2018-08-27). "Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing". Physical Review D. 98 (4): 043526. arXiv: 1708.01530 . Bibcode:2018PhRvD..98d3526A. doi:10.1103/PhysRevD.98.043526. ISSN   2470-0010. S2CID   52219057.
  23. ↑ Troxel, M. A.; MacCrann, N.; Zuntz, J.; Eifler, T. F.; Krause, E.; Dodelson, S.; Gruen, D.; Blazek, J.; Friedrich, O.; Samuroff, S.; Prat, J. (2018-08-27). "Dark Energy Survey Year 1 Results: Cosmological Constraints from Cosmic Shear". Physical Review D. 98 (4): 043528. arXiv: 1708.01538 . Bibcode:2018PhRvD..98d3528T. doi:10.1103/PhysRevD.98.043528. ISSN   2470-0010. S2CID   52993521.
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