Galaxy And Mass Assembly (GAMA): the input catalogue and star–galaxy separation

By I. Baldry, A. Robotham, D. Hill, S. Driver, J. Liske, P. Norberg, Steven Bamford, Andrew M. Hopkins, J. Loveday, J. Peacock and 17 more. 2009

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We describe the spectroscopic target selection for the Galaxy And Mass Assembly (GAMA) survey. The input catalogue is drawn from the Sloan Digital Sky Survey (SDSS) and UKIRT Infrared Deep Sky Survey (UKIDSS). The initial aim is to measure redshifts for galaxies in three 4 ◦ × 12 ◦ regions at 9, 12 and 14.5 h, on the celestial equator, with magnitude selections r< 19.4, z< 18.2 and K AB < 17.6 over all three regions, and r< 19.8 in the 12-h region. The target density is 1080 deg −2 in the 12-h region and 720 deg −2 in the other regions. The average GAMA target density and area are compared with completed and ongoing galaxy redshift surveys. The GAMA survey implements a highly complete star–galaxy separation that jointly uses an intensity-profile separator (� sg = r psf − r model as per the SDSS) and a

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The VIMOS Ultra-Deep Survey: ~10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 < z ≃ 6 (2014, methodology): “We compare in Figure 30 the number of spectra per square degree vs. the area for different surveys, a high redshift version of that presented in Baldry et al. (2010) and updated by Le Fèvre t al.”
Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function at z < 0.06 (2011, methodology): “The limiting magnitudes of the main survey werer < 19.4 in G09 and G15, r < 19.8 in G12,z < 18.2 andKAB < 17.6 (Baldry et al. 2010).”
Colours and luminosities of z = 0.1 galaxies in the eagle simulation (2015, methodology): “…photometric data from the Sloan Digital Sky Survey (SDSS) and the UK Infrared Digital Sky Survey (UKIDSS), with details on the targeting and star–galaxy separation in Baldry et al. (2010) and on the GAMA-processed photometry, including matched aperture photometry from u to K in Hill et al. (2011).”
GALAXY AND MASS ASSEMBLY (GAMA): MID-INFRARED PROPERTIES AND EMPIRICAL RELATIONS FROM WISE (2014, background): “Details of target selection for the survey are outlined in Baldry et al. (2010) and optimal tiling for the survey in Robotham et al. (2010).”
Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology (2014, methodology): “…our redshift bins using the surface brightness and magnitude limits of the GAMA survey: θ = √ L∗ M∗ M 2π 1 dl 100.2(μlim−M −k(z)−25), (7) where M is the galaxy mass in units of M and we assume an i-band M∗ L∗ = 2 (Baldry et al. 2010), M = 4.6 (Hill et al. 2010) and k(z) = 1.5z (Driver et al. 1994).”
Galaxy And Mass Assembly (GAMA): Spectroscopic analysis (2013, methodology): “These numbers include repeat observations, and not all are main survey targets, as they include “filler” targets that take advantage offibres unable to be allocated to main survey targets on any given observation plate (see Baldry et al. 2010).”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, methodology): “A further cut was made to this sample to remove any stars or unresolved objects; this was done using a star–galaxy separation technique based on optical/IR colour and size, similar to that used by Baldry et al. (2010).”
Quantifying cosmic variance (2010, methodology): “Similarly the GAMA survey (Driver et al. 2009; Baldry et al. 2010) consists of 3 chunks of 4 deg by 12 deg regions for an aspect ratio of 1:3.”
Galaxy and mass assembly (GAMA): End of survey report and data release 2 (2015, methodology): “6 of Baldry et al. 2010), we expect the high surface brightness incompleteness to mainly affect the blue end of our sample.”
THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2–2 μm WAVELENGTH (2010, methodology): “Given the much larger size of the GALEX beam (4–6” FWHM), they do however suffer from more uncertain star-galaxy separation, which for GALEX needed to be done by using multi-color information as well (Baldry et al. 2010).”
Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release (2010, methodology): “Note the numbers shown in Table 2 may disagree with those shown in Baldry et al. (2010) as some repeat observations of previous targets were made.”
Galaxy and Mass Assembly (GAMA): the GAMA galaxy group catalogue (G3Cv1) (2011, methodology): “For this study, we use a global GAMA (k+e)-correction, of the form: (k + e)(z) = N ∑ i=0 ai(zref , zp)(z − zp)i +Qzref (z − zref) (8) 1 See Baldry et al. (2010) for additional GAMA-I selections.”
TWO MICRON ALL SKY SURVEY PHOTOMETRIC REDSHIFT CATALOG: A COMPREHENSIVE THREE-DIMENSIONAL CENSUS OF THE WHOLE SKY (2013, background): “The GAMA I survey extends over three equatorial survey regions of 48 deg2 each, called G09, G12 and G15 (Baldry et al. 2010).”
Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions (2011, methodology): “We therefore re-implement the GAMA target selection criteria detailed by Baldry et al. (2010) on samples of objects selected from the SDSS DR6 PHOTOOBJ table.”
The SAMI Galaxy Survey: Instrument specification and target selection (2014, methodology): “The total number of galaxies included in this selection 4 The GAMA catalogues used here are TilingCatv29.fits (Baldry et al. 2010), ApMatchedCatv03.fits (Hill et al. 2011), GalacticExtinctionv02.fits, DistancesFramesv08.fits (Baldry et al. 2012), SersicCatAllv07.fits (Kelvin et al. 2012), StellarMas”
Galaxy And Mass Assembly (GAMA): improved cosmic growth measurements using multiple tracers of large-scale structure (2013, methodology): “The GAMA I target selection is described by Baldry et al. (2010) and GAMA II by Liske et al. (in preparation).”
The VISTA deep extragalactic observations (VIDEO) survey (2012, methodology): “Following Baldry et al. (2010), we fit a quadratic function to the stellar locus and separate the galaxies from the stars using the distance from the locus of the J − Ks colour (see equation 2 in Baldry et al. 2010).”
The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ iAB ≤ 24.75 (2013, methodology): “Following Baldry et al. (2010), we have compiled a list of spectroscopic surveys, as listed in Table 5.”