GAMA: towards a physical understanding of galaxy formation

By S. Driver, P. Norberg, I. Baldry, Steven Bamford, Andrew M. Hopkins, J. Liske, J. Loveday, J. Peacock, D. Hill, Lee S. Kelvin and 39 more. 2009

286 citations recorded by the source corpus.

Simon P Driver, Peder Norberg, Ivan K Baldry, Steven P Bamford, Andrew M Hopkins, Jochen Liske, Jon Loveday, John A Peacock and the GAMA Survey Team (Galaxy and Mass Assembly) review progress on the latest large galaxy redshift survey now underway on the 3.9 m Anglo-Australian Telescope.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5468a8cedad2ae93ea55b48471b28d0157b27c45

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Citations in the corpus

HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, methodology): “Gunawardhana et al. (2011), using a sample of galaxies from the Galaxy And Mass Assembly (GAMA) survey (Driver et al. 2009) covering the redshift range 0 < z < 0.35, find a dependence of x on the SFR that, extrapolated to an SFR = 1000M⊙ yr −1, would give x ≈ 1.5, substantially flatter than the…”
Lightcone mock catalogues from semi-analytic models of galaxy formation – I. Construction and application to the BzK colour selection (2012, methodology): “Mock catalogues constructed in this way have already been used extensively by the Galaxy And Mass Assembly (GAMA) survey (Driver et al. 2009, see also Robotham et al. 2011; Alpaslan et al. 2012).”
The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000 (2014, unknown): “Overlapping surveys include SDSS [77], BOSS [15], CFHTLS [21], XMMXXL [93], Herschel (HerMES & HeLMS, [65, 90]), HSC [83], DES [30], GAMA [32], and KiDS [29].”
EMU: Evolutionary Map of the Universe (2011, methodology): “For nearby galaxies, H Iredshifts will be available from WALLABY, which will provide ,5 105 redshifts, and smaller numbers will be provided by other redshift surveys such as SDSS (York et al. 2000) and GAMA (Driver et al. 2009).”
The Eighteenth Data Release of the Sloan Digital Sky Surveys: Targeting and First Spectra from SDSS-V (2023, background): “The eFEDS X-ray footprint comprises 140 deg2 centered near (α, δ)= (9h, + 1°), encapsulating the “GAMA09” Field (Driver et al. 2009).”
THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2–2 μm WAVELENGTH (2010, methodology): “At the bright end, we added the counts from the Galaxy and Mass Assembly (GAMA) survey (Driver et al. 2009) in NUV+ugrizYJH, which cover AB=10–21 mag (Xu et al. 2005; Hill et al. 2010a).”
Galaxy And Mass Assembly (GAMA): the input catalogue and star–galaxy separation (2009, methodology): “The contiguous SDSS coverage of Stripes 9–12 was chosen to allow GAMA regions that are four-degrees wide: an estimated requirement for group finding and measurement of the halo mass function atz < 0.1 (Driver et al. 2009).”
The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release (2017, background): “In the past decade it has been demonstrated that a panchromatic, X-ray to radio, observational approach is key to develop a consensus on galaxy formation and evolution (e.g., Dickinson et al. 2003; Scoville et al. 2007; Driver et al. 2009, 2011; Koekemoer et al. 2011; Grogin et al. 2011).”
GALAXY AND MASS ASSEMBLY (GAMA): MID-INFRARED PROPERTIES AND EMPIRICAL RELATIONS FROM WISE (2014, methodology): “The Galaxy and Mass Assembly (GAMA; Driver et al. 2009, 2011) survey provides exactly this The Astrophysical Journal, 782:90 (17pp), 2014 February 20 Cluver et al. laboratory.”
Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument (2023, background): “Sample sizes for each target class in the one-month DESI One-Percent Survey compared to related spectroscopic samples (Driver et al. 2009; Dawson et al. 2016).”
Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, background): “…spanning a full range of mass, morphology and environment for which, thanks to facilities such as GALEX, WISE, Spitzer, AKARI and Herschel (e.g. Driver et al. 2009, Eales et al. 2010, Martin 2010) integrated photometry is nowfor the first time becoming routinely available across the full…”
Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release (2010, methodology): “5 of Driver et al. (2009) due to additional spacecraft limitations introduced in-flight.”
Galaxy and Mass Assembly (GAMA): the star formation rate dependence of the stellar initial mass function (2011, methodology): “Motivated by these recent failures of the universal IMF assumption, we have conducted an analysis exploring such variations using a sample of galaxies from the Galaxy and Mass Assembly (GAMA) survey (Driver et al. 2009; Robotham et al. 2009; Baldry et al. 2009).”
Galaxy And Mass Assembly (GAMA): Spectroscopic analysis (2013, background): “The Galaxy And Mass Assembly (GAMA)1 survey is a large multiwavelength photometric and spectroscopic galaxy survey (Driver et al. 2009, 2011) that provides exactly this comprehensive selection of photometric and spectroscopic data.”
Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function at z < 0.06 (2011, background): “The GAMA survey aims to provide redshifts and multi-wavelength images of> 250 000 galaxies over> 250 deg2 to r < 19.8mag (Driver et al. 2009, 2011; Baldry et al. 2010).”
The SAMI Galaxy Survey: Instrument specification and target selection (2014, background): “…et al. 2000; Abazajian et al. 2009), 2-degree Field Galaxy Redshift Survey (2dFGRS; Colless et al. 2001), the Cosmic Evolution Survey (COSMOS; Scoville et al. 2007), the VIMOS VLT Deep Survey (VVDS; Le Fèvre et al. 2004) and the Galaxy and Mass Assembly (GAMA) survey (Driver et al. 2009, 2011).”
KiDS+GAMA : cosmology constraints from a joint analysis of cosmic shear, galaxy-galaxy lensing, and angular clustering (2017, methodology): “We used the KiDS galaxies to measure the cosmic shear correlation functions, and to measure the tangential shear around the foreground galaxies from the GAMA survey (Driver et al. 2009, 2011; Liske et al. 2015).”
Galaxy and mass assembly (GAMA): End of survey report and data release 2 (2015, background): “The motivation and science case of GAMA was explained in more detail by Driver et al. (2009).”