Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release

By S. Driver, D. Hill, Lee S. Kelvin, A. Robotham, J. Liske, P. Norberg, I. Baldry, Steven Bamford, Andrew M. Hopkins, J. Loveday and 45 more. 2010

799 citations recorded by the source corpus.

The Galaxy and Mass Assembly (GAMA) survey has been operating since 2008 February on the 3.9-m Anglo-Australian Telescope using the AAOmega fibre-fed spectrograph facility to acquire spectra with a resolution of R ≈ 1300 for 120 862 Sloan Digital Sky Survey selected galaxies. The target catalogue constitutes three contiguous equatorial regions centred at 9h (G09), 12h (G12) and 14.5h (G15) each of 12 × 4 deg2 to limiting fluxes of rpet < 19.4, rpet < 19.8 and rpet <19.4 mag, respectively (and additional limits at other wavelengths). Spectra and reliable redshifts have been acquired for over 98 per cent of the galaxies within these limits. Here we present the survey footprint, progression, data reduction, redshifting, re-redshifting, an assessment of data quality after 3 yr, additional image analysis products (including ugrizYJHK photometry, S´ersic profiles and photometric redshifts), observing mask and construction of our core survey catalogue (GamaCore). From this we create three science-ready catalogues: GamaCoreDR1 for public release, which includes data acquired during year 1 of operations within specified magnitude limits (2008 February to April); GamaCoreMainSurvey containing all data above our survey limits for use by the GAMA Team and collaborators; and GamaCore-AtlasSV containing year 1, 2 and 3 data matched to Herschel-ATLAS science demonstration data. These catalogues along with the associated spectra, stamps and profiles can be accessed via the GAMA website: http://www.gama-survey.org/

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a9b435f0ecac17d38804e961d3c9073fde7d319c

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Citations in the corpus

The first and second data releases of the Kilo-Degree Survey (2015, methodology): “To maximize the synergy with existing spectroscopic surveys and between KiDS and VIKING early on, the latter surveys both prioritize the observations in the Galaxy And Mass Assembly (GAMA, Driver et al. 2011) fields G9, G12, G15 and G23.”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, methodology): “The Galaxy and Mass Assembly survey (Driver et al. 2011) includes the largest bulge/disk decomposition survey to date using the Viking K-band imaging survey of 4,300 disk galaxies (Lange et al. 2015).”
The massive end of the luminosity and stellar mass functions: Dependence on the fit to the light profile (2013, methodology): “Using the GAMA DR1 data release (Driver et al. 2011), we compare PyMorph, Simard, and GAMA values for the 7335 galaxies for which all three reductions are available.”
The Sydney-AAO Multi-object Integral field spectrograph (2011, methodology): “Surveys such as the Galaxy And Mass Assembly (GAMA) survey (Driver et al. 2011) and the Cosmic Evolution Survey (COSMOS; Scoville et al. 2007) show the value of this multi-wavelength approach.”
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).”
Colours and luminosities of z = 0.1 galaxies in the eagle simulation (2015, methodology): “In what follows we compare to photometric data from the Galaxy And Mass Assembly survey (GAMA; Driver et al. 2011).”
The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, result): “Using this technique, Hoversten & Glazebrook (2008) inferred a variation of the IMF with more massive galaxies having a more top-heavy IMF than Salpeter, a result confirmed under the same assumptions (Gunawardhana et al. 2011) by the Galaxy and Mass Assembly (GAMA) survey (Driver et al. 2011).”
EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, background): “A different option has emerged with the advent of data sets from large galaxy surveys (York et al. 2000; Colless et al. 2001; Lilly et al. 2007; Driver et al. 2011; Grogin et al. 2011; McCracken et al. 2012) and avoids explicitly modelling the baryonic physics.”
Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions (2011, methodology): “7 of Driver et al. (2011) shows that the redshift-error distribution for GAMA is essentially zero by cz = 600 km/s.”
The VIMOS Public Extragalactic Redshift Survey (VIPERS) - an unprecedented view of galaxies and large-scale structure at 0.5 < z < 1.2 (2013, methodology): “This approach has been taken by the GAMA survey (Driver et al. 2011), which aims to achieve similar numbers of redshifts to the 2dFGRS (∼200 000), but working to r < 19.8 and out to z ' 0.5.”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, methodology): “These Science Demonstration Phase (SDP) observations are centred on the 9h field of the Galaxy And Mass Assembly (GAMA; Driver et al. 2011) survey.”
KiDS+VIKING-450: Cosmic shear tomography with optical and infrared data (2018, methodology): “GAMA-G15Deep (Kafle et al. 2018): An area of ∼1 deg2 was observed to greater depth in the GAMA survey (Driver et al. 2011).”
How to Measure Galaxy Star Formation Histories. II. Nonparametric Models (2018, methodology): “Fitting UV-IR galaxy photometry from GAMA The photometry is taken from DR3 of the Galaxy and Mass Assembly (GAMA) survey (Driver et al. 2011; Baldry et al. 2018).”
Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function at z < 0.06 (2011, methodology): “The first three years of the redshift survey have been completed (Driver et al. 2011) and these data are used here.”
Stellar masses of SDSS-III/BOSS galaxies at z ∼ 0.5 and constraints to galaxy formation models (2012, positive): “The observational tracing of the galaxy mass growth as a function of redshift is a powerful diagnostic of the galaxy formation process, which has been investigated by many groups, throug large galaxy surveys (e.g. the Sloan Digital Sky Survey, SDS, York et al. 2000; COMBO-17, Wolf et al. 2001; MUNIC”
KiDS-450: cosmological parameter constraints from tomographic weak gravitational lensing (2016, methodology): “Even though KiDS currently extends beyond the GAMA regions, we continue to group the tiles in five ‘patches’, which we call G9, G12, G15, G23, and GS, following the convention of the GAMA survey, with each patch indicated by the letter ‘G’ and a rough RA (hour) value.”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, methodology): “The agreement between our SMF and the recent measurement by Baldry et al. (2012), who analyzed a sample of ∼ 105 galaxies at z < 0.06 over 143 deg2 with spectroscopic redshifts from the SDSS and GAMA (Driver et al. 2011) surveys, is especially good.”
The fourth data release of the Kilo-Degree Survey: ugri imaging and nine-band optical-IR photometry over 1000 square degrees (2019, background): “The Northern patch, KiDS-N, contains two additional smaller areas: KiDS-N-W2, which coincides with the G9 patch of the GAMA survey (Driver et al. 2011), and KiDS-N-D2, a single pointing on the COSMOS field.”