The Evolutionary Map of the Universe pilot survey (original) (raw)
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EMU: Evolutionary Map of the Universe
2011
Abstract EMU is a wide-field radio continuum survey planned for the new Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The primary goal of EMU is to make a deep (rms~ 10 μJy/beam) radio continuum survey of the entire Southern sky at 1.3 GHz, extending as far North as+ 30 declination, with a resolution of 10 arcsec.
Dark Energy Survey Year 3 Results: Deep Field optical + near-infrared images and catalogue
Monthly Notices of the Royal Astronomical Society, 2021
We describe the Dark Energy Survey (DES) Deep Fields, a set of images and associated multiwavelength catalogue (ugrizJHKs) built from Dark Energy Camera (DECam) and Visible and Infrared Survey Telescope for Astronomy (VISTA) data. The DES Deep Fields comprise 11 fields (10 DES supernova fields plus COSMOS), with a total area of ∼30 sq. deg. in ugriz bands and reaching a maximum i-band depth of 26.75 (AB, 10σ, 2 arcsec). We present a catalogue for the DES 3-yr cosmology analysis of those four fields with full 8-band coverage, totalling 5.88 sq. deg. after masking. Numbering 2.8 million objects (1.6 million post-masking), our catalogue is drawn from images coadded to consistent depths of r = 25.7, i = 25, and z = 24.3 mag. We use a new model-fitting code, built upon established methods, to deblend sources and ensure consistent colours across the u-band to Ks-band wavelength range. We further detail the tight control we maintain over the point-spread function modelling required for the...
The Dark Energy Survey: Data Release 1
The Astrophysical Journal Supplement Series
We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced singleepoch images, coadded images, coadded source catalogs, and associated products and services assembled over the first three years of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (August 2013 to February 2016) by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ∼ 5000 deg 2 of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g = 1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.90 arcsec FWHM, a photometric precision of < 1% in all bands, and an astrometric precision of 151 mas. The median coadded catalog depth for a 1.
We present the combination of optical data from the Science Verification phase of the Dark Energy Survey (DES) with near infrared data from the ESO VISTA Hemisphere Survey (VHS). The deep optical detections from DES are used to extract fluxes and associated errors from the shallower VHS data. Joint 7-band (grizY JK) photometric catalogues are produced in a single 3 sq-deg DECam field centred at 02h26m−04d36m where the availability of ancillary multi-wavelength photometry and spectroscopy allows us to test the data quality. Dual photometry increases the number of DES galaxies with measured VHS fluxes by a factor of ∼4.5 relative to a simple catalogue level matching and results in a ∼1.5 mag increase in the 80% completeness limit of the NIR data. Almost 70% of DES sources have useful NIR flux measurements in this initial catalogue. Photometric redshifts are estimated for a subset of galaxies with spectroscopic redshifts and initial results, although currently limited by small number statistics, indicate that the VHS data can help reduce the photometric redshift scatter at both z < 0.5 and z > 1. We present example DES+VHS colour selection criteria for high redshift Luminous Red Galaxies (LRGs) at z ∼ 0.7 as well as luminous quasars. Using spectroscopic observations in this field we show that the additional VHS fluxes enable a cleaner selection of both populations with <10% contamination from galactic stars in the case of spectroscopically confirmed quasars and < 0.5% contamination from galactic stars in the case of spectroscopically confirmed LRGs. The combined DES+VHS dataset, which will eventually cover almost 5000 sq-deg, will therefore enable a range of new science and be ideally suited for target selection for future wide-field spectroscopic surveys. c 0000 RAS DES r (260 sources) VHS J S/N>10 (51 sources) VHS J S/N>5 (84 sources) VHS J S/N>3 (111 sources) VHS J S/N>2 (147 sources) VHS J S/N>1 (194 sources)
Cosmological Surveys with the Australian Square Kilometre Array Pathfinder
Publications of the Astronomical Society of Australia, 2012
This is a design study into the capabilities of the Australian Square Kilometre Array Pathfinder (ASKAP) in performing a full-sky low redshift neutral hydrogen survey, termed WALLABY, and the potential cosmological constraints one can attain from measurement of the matter power spectrum. We find that the full sky survey will likely attain 6 × 10 5 redshifts which, when combined with expected Planck CMB data, will constrain the Dark Energy equation of state to 20%, for the first time making cosmological constraints from radio observations competitive with the best existing optical surveys.
The Dark Energy Survey: more than dark energy – an overview
Monthly Notices of the Royal Astronomical Society
This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected
2009
Future galaxy surveys will map the galaxy distribution in the redshift interval 0.5<z<20.5<z<20.5<z<2 using near-infrared cameras and spectrographs. The primary science goal of such surveys is to constrain the nature of the dark energy by measuring the large-scale structure of the Universe. This requires a tracer of the underlying dark matter which maximizes the useful volume of the survey. We investigate two potential survey selection methods: an emission line sample based on the \ha line and a sample selected in the H-band. We present predictions for the abundance and clustering of such galaxies, using two published versions of the \galform galaxy formation model. Our models predict that \ha selected galaxies tend to avoid massive dark matter haloes and instead trace the surrounding filamentary structure; H-band selected galaxies, on the other hand, are found in the highest mass haloes. This has implications for the measurement of the rate at which fluctuations grow due to gravitational instability. We use mock catalogues to compare the effective volumes sampled by a range of survey configurations. To give just two examples: a redshift survey down to HrmAB=22H_{\rm AB}=22HrmAB=22 samples an effective volume that is sim5−10\sim 5-10sim5−10 times larger than that probed by an \ha survey with logfha>−15.4\logfha > -15.4logfha>−15.4; a flux limit of at least logfha=−16\logfha = -16logfha=−16 is required for an \ha sample to become competitive in effective volume.
Impact of Redshift Information on Cosmological Applications with Next-Generation Radio Surveys
In this paper we explore the impact of including redshift information on cosmological applications with the forthcoming generation of large-scale, deep radio continuum surveys. By cross-matching these radio surveys with shallow optical to near-infrared surveys we can essentially separate the source distribution into a low redshift sample and the high-z tail of the radio sources that are unidentified, thus providing a constraint on the evolution of cosmological parameters such as those of dark energy. We examine two radio surveys, the Evolutionary Map of the Universe (EMU) and the Westerbork Observations of the Deep APERTIF Northern sky (WODAN). A crucial advantage is their combined potential to provide a deep, full-sky survey. The surveys used for the cross-identifications are SkyMapper and SDSS, for the southern and northern skies, respectively. We concentrate on the galaxy clustering angular power spectrum as our benchmark observable and find that the possibility of including this low redshift information yields major improvements in the results. With this approach, we are able to put strict constraints on the dark energy parameters, i.e. w_0=-0.9+/-0.065(0.087) and w_a=-0.24+/-0.19(0.26) with(without) priors from Planck; this corresponds to a Figure of Merit (FoM) of circa 400(>200), which is two to three orders of magnitude times better than the case without any redshift information and more than three times better than what obtained by using only the cross-identified sources.