The UKIRT Infrared Deep Sky Survey (UKIDSS)
University of Edinburgh1, Imperial College London2, University of Nottingham3, Durham University4, University of Leicester5, University of Hertfordshire6, UK Astronomy Technology Centre7, Cardiff University8, Queen Mary University of London9, University of Cambridge10, Liverpool John Moores University11
21 Aug 2007-Monthly Notices of the Royal Astronomical Society (Oxford University Press)-Vol. 379, Iss: 4, pp 1599-1617
TL;DR: The final version published in MNRAS August 2007 included significant revisions including significant revisions to the original version April 2006.
Abstract: Final published version including significant revisions. Twenty four pages, fourteen figures. Original version April 2006; final version published in MNRAS August 2007
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University of California, Los Angeles1, Jet Propulsion Laboratory2, California Institute of Technology3, University of Arizona4, University of Virginia5, Lawrence Livermore National Laboratory6, University of California, Davis7, Monterey Institute for Research in Astronomy8, Goddard Space Flight Center9, National Radio Astronomy Observatory10, University of California, Berkeley11, Wilmington University12, Advanced Technology Center13
TL;DR: The Wide-field Infrared Survey Explorer (WISE) is mapping the whole sky following its launch on 14 December 2009 and completed its first full coverage of the sky on July 17 as discussed by the authors.
Abstract: The all sky surveys done by the Palomar Observatory Schmidt, the European Southern Observatory Schmidt, and the United Kingdom Schmidt, the InfraRed Astronomical Satellite and the 2 Micron All Sky Survey have proven to be extremely useful tools for astronomy with value that lasts for decades. The Wide-field Infrared Survey Explorer is mapping the whole sky following its launch on 14 December 2009. WISE began surveying the sky on 14 Jan 2010 and completed its first full coverage of the sky on July 17. The survey will continue to cover the sky a second time until the cryogen is exhausted (anticipated in November 2010). WISE is achieving 5 sigma point source sensitivities better than 0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic in bands centered at wavelengths of 3.4, 4.6, 12 and 22 micrometers. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodiacal background. The angular resolution is 6.1", 6.4", 6.5" and 12.0" at 3.4, 4.6, 12 and 22 micrometers, and the astrometric precision for high SNR sources is better than 0.15".
7,182 citations
Daniel J. Eisenstein1, Daniel J. Eisenstein2, David H. Weinberg3, Eric Agol4 +260 more•Institutions (62)
TL;DR: SDSS-III as mentioned in this paper is a program of four spectroscopic surveys on three scientific themes: dark energy and cosmological parameters, the history and structure of the Milky Way, and the population of giant planets around other stars.
Abstract: Building on the legacy of the Sloan Digital Sky Survey (SDSS-I and II), SDSS-III is a program of four spectroscopic surveys on three scientific themes: dark energy and cosmological parameters, the history and structure of the Milky Way, and the population of giant planets around other stars. In keeping with SDSS tradition, SDSS-III will provide regular public releases of all its data, beginning with SDSS DR8 (which occurred in Jan 2011). This paper presents an overview of the four SDSS-III surveys. BOSS will measure redshifts of 1.5 million massive galaxies and Lya forest spectra of 150,000 quasars, using the BAO feature of large scale structure to obtain percent-level determinations of the distance scale and Hubble expansion rate at z 100 per resolution element), H-band (1.51-1.70 micron) spectra of 10^5 evolved, late-type stars, measuring separate abundances for ~15 elements per star and creating the first high-precision spectroscopic survey of all Galactic stellar populations (bulge, bar, disks, halo) with a uniform set of stellar tracers and spectral diagnostics. MARVELS will monitor radial velocities of more than 8000 FGK stars with the sensitivity and cadence (10-40 m/s, ~24 visits per star) needed to detect giant planets with periods up to two years, providing an unprecedented data set for understanding the formation and dynamical evolution of giant planet systems. (Abridged)
2,265 citations
Cites methods from "The UKIRT Infrared Deep Sky Survey ..."
...…data where they are available, including additional SDSS epochs (which improve photometric precision where stripes overlap and, on the southern equatorial stripe, provide variability information) and photometry from GALEX (UV; Martin et al. 2005) and UKIDSS (near-IR; Lawrence et al. 2007)....
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Space Telescope Science Institute1, University of California, Santa Cruz2, Johns Hopkins University3, Rutgers University4, Durham University5, University of Nottingham6, Harvard University7, University of Innsbruck8, University of Michigan9, DSM10, University of Edinburgh11, University of Massachusetts Amherst12, California Institute of Technology13, UK Astronomy Technology Centre14, University of California, Irvine15, Swinburne University of Technology16, University of Arizona17, Goddard Space Flight Center18, The Catholic University of America19, Hebrew University of Jerusalem20, University of Victoria21, University of California, Berkeley22, Texas A&M University23, University of Notre Dame24, Carnegie Institution for Science25, Smithsonian Institution26, Yale University27, University of Missouri–Kansas City28, University of California, Riverside29, Max Planck Society30, University of Pittsburgh31, Inter-University Centre for Astronomy and Astrophysics32, University of Barcelona33, European Southern Observatory34, University of Minnesota35, National Research Council36, Western Kentucky University37, Stanford University38, Atacama Large Millimeter Submillimeter Array39, University of Missouri40
TL;DR: The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) as discussed by the authors was designed to document the first third of galactic evolution, from z approx. 8 - 1.5 to test their accuracy as standard candles for cosmology.
Abstract: The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) is designed to document the first third of galactic evolution, from z approx. 8 - 1.5. It will image > 250,000 distant galaxies using three separate cameras on the Hubble Space Tele8cope, from the mid-UV to near-IR, and will find and measure Type Ia supernovae beyond z > 1.5 to test their accuracy as standard candles for cosmology. Five premier multi-wavelength sky regions are selected, each with extensive ancillary data. The use of five widely separated fields mitigates cosmic variance and yields statistically robust and complete samples of galaxies down to a stellar mass of 10(exp 9) solar mass to z approx. 2, reaching the knee of the UV luminosity function of galaxies to z approx. 8. The survey covers approximately 800 square arc minutes and is divided into two parts. The CANDELS/Deep survey (5(sigma) point-source limit H =27.7mag) covers approx. 125 square arcminutes within GOODS-N and GOODS-S. The CANDELS/Wide survey includes GOODS and three additional fields (EGS, COSMOS, and UDS) and covers the full area to a 50(sigma) point-source limit of H ? or approx. = 27.0 mag. Together with the Hubble Ultradeep Fields, the strategy creates a three-tiered "wedding cake" approach that has proven efficient for extragalactic surveys. Data from the survey are non-proprietary and are useful for a wide variety of science investigations. In this paper, we describe the basic motivations for the survey, the CANDELS team science goals and the resulting observational requirements, the field selection and geometry, and the observing design.
2,088 citations
Cites background or methods from "The UKIRT Infrared Deep Sky Survey ..."
...Therefore our fundamental astrometric frame for this is the UKIDSS K-band catalog (Almaini et al., priv. comm.; Lawrence et al. 2007), which has been obtained by imaging the field with UKIRT/WFCAM and is registered to the VLA 20 cm survey of the field (Simpson et al. 2006) to a similar level of…...
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...…with wider/shallower imaging of the Extended Groth Strip (EGS: Davis et al. 2007; Newman et al. 2011, in prep), COSMOS (Scoville et al. 2007; Koekemoer et al. 2007), and the UKIDSS UltraDeep Survey (UDS: Lawrence et al. 2007; Cirasuolo et al. 2007), while also permitting a search for SNe Ia....
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..., COSMOS (Scoville et al. 2007; Koekemoer et al. 2007),and the UKIDSS Ultra-Deep Survey (UDS: Lawrence et al. 2007; Cirasuolo et al. 2007)....
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Space Telescope Science Institute1, University of California, Santa Cruz2, Johns Hopkins University3, Western Kentucky University4, University of Massachusetts Amherst5, Carnegie Institution for Science6, European Southern Observatory7, Ohio State University8, Rutgers University9, Durham University10, University of Nottingham11, Max Planck Society12, University of Innsbruck13, University of Michigan14, French Alternative Energies and Atomic Energy Commission15, University of Edinburgh16, Harvard University17, California Institute of Technology18, University of California, Irvine19, Swinburne University of Technology20, University of Arizona21, Goddard Space Flight Center22, Hebrew University of Jerusalem23, Victoria University, Australia24, DSM25, University of California, Berkeley26, Texas A&M University27, University of Notre Dame28, Smithsonian Institution29, Yale University30, University of Missouri–Kansas City31, University of California, Riverside32, Imperial College London33, University of Pittsburgh34, Inter-University Centre for Astronomy and Astrophysics35, National Research Council36, Stanford University37
TL;DR: In this paper, the authors describe the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS).
Abstract: This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers ~125 arcmin2 within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of ~800 arcmin2 across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.
2,011 citations
Cites background or methods from "The UKIRT Infrared Deep Sky Survey ..."
...Therefore our fundamental astrometric frame for this is the UKIDSS K-band catalog (Almaini et al., priv. comm.; Lawrence et al. 2007), which has been obtained by imaging the field with UKIRT/WFCAM and is registered to the VLA 20 cm survey of the field (Simpson et al. 2006) to a similar level of…...
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...…with wider/shallower imaging of the Extended Groth Strip (EGS: Davis et al. 2007; Newman et al. 2011, in prep), COSMOS (Scoville et al. 2007; Koekemoer et al. 2007), and the UKIDSS UltraDeep Survey (UDS: Lawrence et al. 2007; Cirasuolo et al. 2007), while also permitting a search for SNe Ia....
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..., COSMOS (Scoville et al. 2007; Koekemoer et al. 2007),and the UKIDSS Ultra-Deep Survey (UDS: Lawrence et al. 2007; Cirasuolo et al. 2007)....
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Kyle S. Dawson1, David J. Schlegel2, Christopher P. Ahn1, Scott F. Anderson3 +181 more•Institutions (51)
TL;DR: The Baryon Oscillation Spectroscopic Survey (BOSS) as discussed by the authors was designed to measure the scale of baryon acoustic oscillations (BAO) in the clustering of matter over a larger volume than the combined efforts of all previous spectroscopic surveys of large-scale structure.
Abstract: The Baryon Oscillation Spectroscopic Survey (BOSS) is designed to measure the scale of baryon acoustic oscillations (BAO) in the clustering of matter over a larger volume than the combined efforts of all previous spectroscopic surveys of large-scale structure. BOSS uses 1.5 million luminous galaxies as faint as i = 19.9 over 10,000 deg2 to measure BAO to redshifts z < 0.7. Observations of neutral hydrogen in the Lyα forest in more than 150,000 quasar spectra (g < 22) will constrain BAO over the redshift range 2.15 < z < 3.5. Early results from BOSS include the first detection of the large-scale three-dimensional clustering of the Lyα forest and a strong detection from the Data Release 9 data set of the BAO in the clustering of massive galaxies at an effective redshift z = 0.57. We project that BOSS will yield measurements of the angular diameter distance dA to an accuracy of 1.0% at redshifts z = 0.3 and z = 0.57 and measurements of H(z) to 1.8% and 1.7% at the same redshifts. Forecasts for Lyα forest constraints predict a measurement of an overall dilation factor that scales the highly degenerate DA (z) and H –1(z) parameters to an accuracy of 1.9% at z ~ 2.5 when the survey is complete. Here, we provide an overview of the selection of spectroscopic targets, planning of observations, and analysis of data and data quality of BOSS.
1,938 citations
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TL;DR: The Two Micron All Sky Survey (2MASS) as mentioned in this paper collected 25.4 Tbytes of raw imaging data from two dedicated 1.3 m diameter telescopes located at Mount Hopkins, Arizona and CerroTololo, Chile.
Abstract: Between 1997 June and 2001 February the Two Micron All Sky Survey (2MASS) collected 25.4 Tbytes of raw imagingdatacovering99.998%ofthecelestialsphereinthenear-infraredJ(1.25 � m),H(1.65 � m),andKs(2.16 � m) bandpasses. Observations were conducted from two dedicated 1.3 m diameter telescopes located at Mount Hopkins, Arizona,andCerroTololo,Chile.The7.8sofintegrationtimeaccumulatedforeachpointontheskyandstrictquality control yielded a 10 � point-source detection level of better than 15.8, 15.1, and 14.3 mag at the J, H, and Ks bands, respectively, for virtually the entire sky. Bright source extractions have 1 � photometric uncertainty of <0.03 mag and astrometric accuracy of order 100 mas. Calibration offsets between any two points in the sky are <0.02 mag. The 2MASS All-Sky Data Release includes 4.1 million compressed FITS images covering the entire sky, 471 million source extractions in a Point Source Catalog, and 1.6 million objects identified as extended in an Extended Source Catalog.
12,126 citations
"The UKIRT Infrared Deep Sky Survey ..." refers background in this paper
...The UKIRT Infrared Deep Sky Survey (UKIDSS) is the most significant step forward in infrared sky surveys since the Two Micron All Sky Survey Project (2MASS; Skrutskie et al. 2006), and can be considered the near-infrared counterpart of the Sloan Digital Sky Survey (SDSS; York et al. 2000)....
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TL;DR: The Sloan Digital Sky Survey (SDSS) as mentioned in this paper provides the data to support detailed investigations of the distribution of luminous and non-luminous matter in the Universe: a photometrically and astrometrically calibrated digital imaging survey of pi steradians above about Galactic latitude 30 degrees in five broad optical bands.
Abstract: The Sloan Digital Sky Survey (SDSS) will provide the data to support detailed investigations of the distribution of luminous and non- luminous matter in the Universe: a photometrically and astrometrically calibrated digital imaging survey of pi steradians above about Galactic latitude 30 degrees in five broad optical bands to a depth of g' about 23 magnitudes, and a spectroscopic survey of the approximately one million brightest galaxies and 10^5 brightest quasars found in the photometric object catalog produced by the imaging survey. This paper summarizes the observational parameters and data products of the SDSS, and serves as an introduction to extensive technical on-line documentation.
10,039 citations
Donald G. York1, Jennifer Adelman2, John E. Anderson2, Scott F. Anderson3 +148 more•Institutions (29)
TL;DR: The Sloan Digital Sky Survey (SDSS) as discussed by the authors provides the data to support detailed investigations of the distribution of luminous and non-luminous matter in the universe: a photometrically and astrometrically calibrated digital imaging survey of π sr above about Galactic latitude 30° in five broad optical bands to a depth of g' ~ 23 mag.
Abstract: The Sloan Digital Sky Survey (SDSS) will provide the data to support detailed investigations of the distribution of luminous and nonluminous matter in the universe: a photometrically and astrometrically calibrated digital imaging survey of π sr above about Galactic latitude 30° in five broad optical bands to a depth of g' ~ 23 mag, and a spectroscopic survey of the approximately 106 brightest galaxies and 105 brightest quasars found in the photometric object catalog produced by the imaging survey. This paper summarizes the observational parameters and data products of the SDSS and serves as an introduction to extensive technical on-line documentation.
9,835 citations
"The UKIRT Infrared Deep Sky Survey ..." refers background in this paper
...The primary goal of UKIDSS is to produce IR sky atlases as a fundamental resource of lasting significance analogous to the various Schmidt photographic sky surveys of the 1970s and onwards (Hambly et al. 2001 and references therein), and to the SDSS survey of modern times (York et al 2000)....
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...The UKIRT Infrared Deep Sky Survey (UKIDSS) is the most significant step forward in infrared sky surveys since the Two Micron All Sky Survey Project (2MASS; Skrutskie et al. 2006), and can be considered the near-infrared counterpart of the Sloan Digital Sky Survey (SDSS; York et al. 2000)....
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01 Aug 2008
TL;DR: The ADS abstract service at: http://adswww.harvard.edu has been updated considerably in the last year and new capabilities in the search engine include searching for multi-word phrases and searching for various logical combinations of search terms.
5,584 citations
TL;DR: In this article, a large sample of galaxies from the 2MASS and the Sloan Digital Sky Survey (SDSS) was used to calculate galaxy luminosity and stellar mass functions in the local Universe.
Abstract: We use a large sample of galaxies from the Two Micron All Sky Survey(2MASS) and the Sloan Digital Sky Survey (SDSS) to calculate galaxy luminosity and stellar mass functions in the local Universe. We estimate corrections for passband shifting and galaxy evolution, as well as present-day stellar mass-to-light (M/L) ratios, by fitting the optical‐near-infrared galaxy data with simpl e models. Accounting for the 8% galaxy overdensity in the SDSS early data release region, the optical and near-infrared luminosity functions we construct for this sample agree with most recent literature optical and near-infrare d determinations within the uncertainties. We argue that 2MASS is biased against low surface brightness galaxies, and use SDSS plus our knowledge of stellar populations to estimate the ‘true’ K-band luminosity function. This has a steeper faint end slope and a slightly higher overall luminosity density than the direct estimate. Furthermore, assuming a universally-applicable stellar initial mass function (IMF), we find good agreement between the stellar ma ss function we derive from the 2MASS/SDSS data and that derived by Cole et al. (2001; MNRAS, 326, 255). The faint end slope slope for the stellar mass function is steeper than -1.1, reflecting the low stellar M/L ratios characteristic of lo w-mass galaxies. We estimate an upper limit to the stellar mass density in the local Universe ∗h = 2.0 ± 0.6 × 10 -3 by assuming an IMF as rich in low-mass stars as allowed by observations of galaxy dynamics in the local Universe. The stellar mass density may be lower than this value if a different IMF with fewer low-mass stars is assumed. Finally, we examine typedependence in the optical and near-infrared luminosity functions and the stellar mass function. In agreement with previous work, we find that the characteristic luminosity or mass of early-type galaxies is larger than for later types, and the faint end slope is steeper for later types than for earlier types. Accounting for typing uncertainties, we estimate that at least half, and perhaps as much as 3/4, of the stellar mass in the Universe is in early-type galaxies. As an aid to workers in the field, we present in an appendix the r elationship between model stellar M/L ratios and colors in SDSS/2MASS passbands, an updated discussion of near-infrared stellar M/L ratio estimates, and the volume-corrected distribution of g and K-band stellar M/L ratios as a function of stellar mass. Subject headings: galaxies: luminosity function, mass function ‐ galaxies: g eneral — galaxies: evolution — galaxies: stellar content
2,371 citations
"The UKIRT Infrared Deep Sky Survey ..." refers background in this paper
...To avoid selecting only the brightest and hence most massive galaxies, this requires the detection of galaxies close to the break in the galaxy luminosity function, M∗K which is -22.6 locally (Bell et al. 2003)....
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