The GAMA survey aims to deliver 250,000 optical spectra (3--7Ang resolution)
over 250 sq. degrees to spectroscopic limits of r_{AB} <19.8 and K_{AB}<17.0
mag. Complementary imaging will be provided by GALEX, VST, UKIRT, VISTA,
HERSCHEL and ASKAP to comparable flux levels leading to a definitive
multi-wavelength galaxy database. The data will be used to study all aspects of
cosmic structures on 1kpc to 1Mpc scales spanning all environments and out to a
redshift limit of z ~ 0.4. Key science drivers include the measurement of: the
halo mass function via group velocity dispersions; the stellar, HI, and
baryonic mass functions; galaxy component mass-size relations; the recent
merger and star-formation rates by mass, types and environment. Detailed
modeling of the spectra, broad SEDs, and spatial distributions should provide
individual star formation histories, ages, bulge-disc decompositions and
stellar bulge, stellar disc, dust disc, neutral HI gas and total dynamical
masses for a significant subset of the sample (~100k) spanning both the giant
and dwarf galaxy populations. The survey commenced March 2008 with 50k spectra
obtained in 21 clear nights using the Anglo Australian Observatory's new
multi-fibre-fed bench-mounted dual-beam spectroscopic system (AAOmega).Comment: Invited talk at IAU 254 (The Galaxy Disk in Cosmological Context,
  Copenhagen), 6 pages, 5 figures, high quality PDF version available at
  http://www.eso.org/~jliske/gama

Baldry, I. K.

Bamford, S.

Bland-Hawthorn, J.

Bridges, T.

Cameron, E.

Conselice, C.

Couch, W. J.

Croom, S.

Cross, N. J. G.

Driver, S. P.

Driver, Simon P.

Dunne, L.

Eales, Stephen Anthony

Edmondson, E.

Ellis, S. C.

Frenk, C. S.

Graham, A. W.

Hill, D.

Hopkins, A.

Jones, H.

Kuijken, K.

Lahav, O.

Liske, J.

Loveday, J.

Nichol, B.

Norberg, P.

Nordstrom, B.

Oliver, S.

Parkinson, H.

Peacock, J. A.

Phillipps, S.

Popescu, C. C.

Prescott, M.

Proctor, R.

Sharp, R.

Staveley-Smith, L.

Sutherland, W.

Tuffs, R. J.

van Kampen, E.

Warren, S.

English

arXiv

The GAMA survey aims to deliver 250,000 optical spectra (3–7°A resolution) over 250 sq. degrees to spectroscopic limits of rAB < 19.8 and KAB < 17.0 mag. Complementary imaging will be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and ASKAP to comparable flux levels leading to a definitive multi-wavelength galaxy database. The data will be used to study all aspects of cosmic structures on 1kpc to 1Mpc scales spanning all environments and out to a redshift limit of z 0.4. Key science drivers include the measurement of: the halo mass function via group velocity dispersions; the stellar, HI, and baryonic mass functions; galaxy component mass-size relations; the recent merger and star-formation rates by mass, types and environment. Detailed modeling of the spectra, broad SEDs, and spatial distributions should provide individual star formation histories, ages, bulge-disc decompositions and stellar bulge, stellar disc, dust disc, neutral HI gas and total dynamical masses for a significant subset of the sample ( 100k) spanning both the giant and dwarf galaxy populations. The survey commenced March 2008 with 50k spectra obtained in 21 clear nights using the Anglo Australian Observatory’s new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AA )

Driver, S.

Baldry, I.

Couche, W.

Cross, N.

Eales, S.

Ellis, E.

Frenk, C.

Graham, A.

Hill, H.

Kuijken, E.

Norberg, B.

Peacock, J.

Phillips, S.

Popescu, C.

Tuffs, R.

MPG.PuRe

Galaxy And Mass Assembly (GAMA)

The GAMA survey aims to deliver 250,000 optical spectra (3–7 Å resolution) over 250 sq. degrees to spectroscopic limits of r(AB) < 19.8 and K(AB) < 17.0 mag. Complementary imaging will be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and ASKAP to comparable flux levels leading to a definitive multi-wavelength galaxy database. The data will be used to study all aspects of cosmic structures on 1kpc to 1Mpc scales spanning all environments and out to a redshift limit of z ≈ 0.4. Key science drivers include the measurement of: the halo mass function via group velocity dispersions; the stellar, HI, and baryonic mass functions; galaxy component mass-size relations; the recent merger and star-formation rates by mass, types and environment. Detailed modeling of the spectra, broad SEDs, and spatial distributions should provide individual star formation histories, ages, bulge-disc decompositions and stellar bulge, stellar disc, dust disc, neutral HI gas and total dynamical masses for a significant subset of the sample (~ 100k) spanning both the giant and dwarf galaxy populations. The survey commenced March 2008 with 50k spectra obtained in 21 clear nights using the Anglo Australian Observatory's new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AA

Online Research @ Cardiff

The Galaxy Disk in Cosmological ContextProceedings IAU Symposium No. 254, 2008J. Andersen, J. Bland-Hawthorn & B. Nordström, eds.c© 2009 International Astronomical Uniondoi:10.1017/S1743921308027981Galaxy And Mass Assembly (GAMA)Simon P. Driver1 and the GAMA team†1 (SUPA) School of Physics and Astronomy, University of St AndrewsSt Andrews, Fife, KY16 8RS, Scotlandemail: spd3@st-and.ac.ukAbstract. The GAMA survey aims to deliver 250,000 optical spectra (3–7Å resolution) over 250sq. degrees to spectroscopic limits of rA B < 19.8 and KA B < 17.0 mag. Complementary imagingwill be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and ASKAP to comparableflux levels leading to a definitive multi-wavelength galaxy database. The data will be usedto study all aspects of cosmic structures on 1kpc to 1Mpc scales spanning all environmentsand out to a redshift limit of z ≈ 0.4. Key science drivers include the measurement of: thehalo mass function via group velocity dispersions; the stellar, HI, and baryonic mass functions;galaxy component mass-size relations; the recent merger and star-formation rates by mass,types and environment. Detailed modeling of the spectra, broad SEDs, and spatial distributionsshould provide individual star formation histories, ages, bulge-disc decompositions and stellarbulge, stellar disc, dust disc, neutral HI gas and total dynamical masses for a significant subsetof the sample (∼ 100k) spanning both the giant and dwarf galaxy populations. The surveycommenced March 2008 with 50k spectra obtained in 21 clear nights using the Anglo AustralianObservatory’s new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AAΩ).Keywords. galaxies: general, galaxies: structure, galaxies: formation, galaxies: evolution1. GAMA MotivationGalaxy And Mass Assembly (GAMA) is a major expansion of the Millennium GalaxyCatalogue (MGC) survey (Liske et al. 2003; Allen et al. 2006, Driver et al. (2005) anda natural extension of the extremely productive nearby “Legacy” surveys (e.g., SDSS,2MASS, HIPASS etc). In comparison to the superb SDSS survey GAMA will only sample250 sq degrees of sky but will extend to significantly fainter spectroscopic limits (12×the redshift density of SDSS main, 5× stripe 82), to higher spatial (0.6′′ FWHM) andspectral (3–7Å) resolutions, as well as moving to a far broader wavelength coverage (UVto Radio). GAMA has come about by parallel technological developments leading to asuite of new facilities whose survey sensitivities, resolutions, and capabilities are reason-ably well matched. Until now the study of galaxies has generally been restricted to eitherlarge samples of limited wavelength data or multi-wavelength studies of small (and oftenbiased) samples. However galaxy systems are extremely complex and diverse, exhibit-ing strong environmental and mass dependencies and containing distinct but interlinked† I.K. Baldry (LJMU), S. Bamford (Nott), J. Bland-Hawthorn (USyd), T. Bridges (AAO),E. Cameron (StA), C. Conselice (Nott), W.J. Couch (Swinburne), S. Croom (USyd), N.J.G.Cross (Edin), S.P. Driver (StA), L. Dunne (Nott.), S. Eales (Cardiff), E. Edmondson (Ports),S.C. Ellis (USyd), C.S. Frenk (Durham), A.W. Graham (Swinburne), H. Jones (AAO), D. Hill(StA), A. Hopkins (USyd), E. van Kampen (Inns), K. Kuijken (Leiden), O. Lahav (UCL), J.Liske (ESO), J. Loveday (Sussex), B. Nichol (Ports.), P. Norberg (Edin), S. Oliver (Sussex),H. Parkinson (Edin), J.A. Peacock (Edin), S. Phillipps (Bristol), C.C. Popescu (UCLan), M.Prescott (LJMU), R. Proctor (Swinburne), R. Sharp (AAO), L. Staveley-Smith (UWA), W.Sutherland (QMW), R.J. Tuffs (MPIK), S. Warren (Imperial).469470 S. P. Driver and the GAMA teamFigure 1. Facilities contributing to the final GAMA database.components (AGN, nucleus, bulge, pseudo-bulge, bar, disc etc) and constituents (SMBH,plasma, stars, gas, dust etc). It then follows that a clear understanding of galaxy forma-tion and evolution may only come about via the construction of a comprehensive surveywhich simultaneously samples all of these facets. The GAMA team aims to provide thisdata. In addition to the provision of a generic galaxy database, the GAMA project alsoincludes a number of more focussed science goals, in particular:1. Measurement of the Halo Mass Function via virialised group velocity dispersionsto directly test the numerical prediction from CDM (and WDM) simulations.2. Measurement of the dynamic, baryonic, HI and stellar mass functions to LMCmasses versus redshift, environment, type, and component (as well as higher order rela-tions, e.g., mass-spin [M − λ]).3. Measurement of the recent merger rates and star formation rates versus type, massand environment over a 3–4 Gyr baseline.2. Facilities Contributing to GAMAFig. 1 shows the facilities currently contributing to the GAMA project along with theapproximate time allocations within the GAMA sky regions (see Fig. 2 and Tables 1 & 2).The expected source resolution and detection sensitivities (5σ point source) are shownin Fig. 3 (upper and lower) in arcseconds and milliJanskys. Overlaid on the lower panelis the modelled NGC891 spectra (Popescu et al. 2000) with a weak AGN added andtransposed to z ≈ 0.1. The UKIRT data is provided courtesy of the UKIDSS LAS PublicGAMA 471Figure 2. (black rectangles) Survey regions of first year data obtained in 21 clear nights ascompared to the 2dFGRS (green outline) and MGC (blue band) surveys. Also shown are galaxieswithin 10Mpc (red dots), abell clusters (yellow), bright stars (cyan) and the NGC catalogue(magenta). The dashed regions show the final GAMA survey extent.Survey while the VST and VISTA data are provided via the KIDS and VIKING ESOPublic Surveys (whose teams include GAMA members). The Herschel data is providedas part of the broader Herschel-ATLAS survey and a proposal is currently pending tocomplete GALEX medium depth observations of the GAMA regions (∼50% already cov-ered with MIS). A major advancement over previous surveys will be the inclusion ofradio data via ASKAP (Australian Square Kilometer Array Pathfinder, see Johnstonet al. 2007) which should allow HI mass, dynamical mass and continuum measurementsfor all GAMA galaxies with high or normal neutral gas content. The deep ASKAP point-ing (a single 6o × 6o field of 1 year integration) is predicted to have an n(z) distributioncomparable to that derived for GAMA (see Fig. 4). While the exact location of theASKAP deep pointing has not been finalised it is highly likely, given the similarity inthe n(z) distributions that one of the GAMA fields will be adopted (nominally the 12hrfield).Table 1. The current extent of the GAMA survey showing the year 1 regions and two possibleexpansion options currently under consideration.GAMA Year 1 Regions Extension 1 Extension 2Field ID RA(deg) δ(deg) RA(deg) δ(deg) RA(deg) δ(deg)G09 129.0 – 141.0 -1 – +2 129.0 – 141.0 -1 – +3 129.0 – 141.0 -3 – +3G12 174.0 – 186.0 -2 – +1 174.0 – 186.0 -2 – +2 129.0 – 186.0 -3 – +3G14 211.5 – 223.5 -1 – +2 211.5 – 223.5 -2 – +2 211.5 – 223.5 -3 – +3G03 – – 45.0 – 57.0 -28 – -31 – –G22 – – 348.0 – 360.0 -28 – -31 – –472 S. P. Driver and the GAMA teamFigure 3. (lower) Spectroscopic, photometric and (upper) resolution sensitivities in mJsy andarcseconds respectively. Overlaid are the typical AGN (green), stellar (blue) and dust emissions(red; based on NGC891 at z ≈ 0.1 with weak AGN added).3. First LightThe survey commenced March 2008 with 50k spectra obtained in 21 clear nights us-ing the Anglo Australian Observatory’s new multi-fibre-fed bench-mounted dual-beamspectroscopic system (AAΩ). Fig. 5 shows the areas of sky surveyed (upper) and theresulting cone plot (lower). This includes the existing 25k redshifts within these regionsfrom the MGC, SDSS and 2dFGRS. AAΩ represents an upgrade of the pre-existing 2dFsystem using the same fibre positioner/tumbler but replacing the two telescope mountedspectrographs with a single bench-mounted, double-beam spectrograph (see Sharp et al.2006 or the AAO website). The facility can be used for both multi-fibre and integral fieldspectroscopy and in multi-fibre mode is capable of obtaining 350–400 spectra in a single2o diameter field. During an 8hr observation period the system is capable of obtaining∼3000 spectra. Data are reduced in real-time and redshifts also obtained in real-timevia cross-correlation with a template library. All data are later re-reduced and processedwith GANDALF (see Schawinski et al. 2007) to obtain line indices and velocity disper-sion measurements. The GAMA survey at the AAT uses the 580V and 385R gratingsyielding a resolution of 1300 or 3–7ÅFWHM.GAMA 473Figure 4. The GAMA n(z) distribution compared to that expected by the ASKAP 1 yeardeep stare, aribtrarily normalised to give a comparable height peak.Table 2. Time allocations, resolutions and sensitivities of the facilities contributing to theGAMA survey. Limits are for 5σ detections in AB mag or mJsky (1Jsky = 3631 × 10−0 .4m A B ).Window Facility Collab.(Time) Detection limits Resol. GAMA FieldsUV GALEX MIS + FUV NUV FUV/NUV G09,G12,G1525hrs pend. 23.0 23.0 4–5′′Opt SDSS DR6 u g r i z u-z G09,G12,G1522.0 22.0 22.2 21.3 20.5 1.0′′-2.5′′VST KIDS (70n) 24.8 25.4 25.2 24.2 – 0.6′′ – 1.0′′ AllNear-IR UKIRT LAS (10n) Z Y J H K Z-K G09,G12,G15– 20.9 20.6 20.3 20.1 0.6′′-1.0′′VISTA VIKING (40n) 23.1 22.3 22.1 21.5 21.1 0.6′′–0.8′′ AllFar-IR Herschel ATLAS (200hrs) 110μm 170μm 250μm 350μm 500μm 110–500μm67mJ 94mJ 45mJ 62mJ 53mJ 8–35′′ AllRadio ASKAP DEEP (1 year) 0.7-1.8 GHz 0.7-1.8GHz G12?10μJ ∼10′′4. SummaryThe GAMA project has commenced with data flows imminent from a number of in-ternational facilities. The survey will allow for a comprehensive study of structure on1kpc to 1Mpc scales as well as the subdivision of the galaxy population into its distinct474 S. P. Driver and the GAMA teamFigure 5. (upper panel) The GAMA sky coverage and (lower panel) cone plot from the firstyear of GAMA observations at the AAT.components and constituents. Progress and data releases (1st data release forecast for Dec2009) can be monitored via the GAMA website: http://www.eso.org/∼jliske/gama/ andanyone interested in further details should contact Simon Driver at spd3@st-and.ac.uk.The GAMA team acknowledges all staff of the Anglo Australian Observatory for provi-sion of the superb AAΩ facility and the continued smooth running of the Anglo AustralianTelescope. SPD thanks the IAU254 organisers for a most enjoyable meeting.ReferencesAllen, P. D., Driver, S. P., Graham, A. W., et al., 2006, MNRAS, 371, 2Driver, S. P., Liske, J., Cross, N. J. G., et al., 2005, MNRAS, 360, 81Driver, S. P., Popescu, C. C., Tuffs, R. J., et al., 2008, ApJL, 678, 101Johnston, S., et al., 2007, PASA, 24, 174Liske, J., Lemon, D. J., Driver, S. P., et al., 2003, MNRAS, 344, 307Popescu, C. C., Misiriotis, A., Kylafis, N. D., et al., 2000, A&A, 362, 138Sharp, R., et al., 2006, SPIE, 6269, 14Schawinski, K., Thomas, D., Sarzi, M., et al., 2007, MNRAS, 382, 1415

Galaxy and mass assembly (GAMA)

The GAMA survey aims to deliver 250,000 optical spectra (3–7°A resolution) over 250 sq. degrees to spectroscopic limits of rAB < 19.8 and KAB < 17.0 mag. Complementary imaging will be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and ASKAP to comparable flux levels leading to a definitive multi-wavelength galaxy database. The data will be used to study all aspects of cosmic structures on 1kpc to 1Mpc scales spanning all environments and out to a redshift limit of z   0.4. Key science drivers include the measurement of: the halo mass function via group velocity dispersions; the stellar, HI, and baryonic mass functions; galaxy component mass-size relations; the recent merger and star-formation rates by mass, types and environment. Detailed modeling of the spectra, broad SEDs, and spatial distributions should provide individual star formation histories, ages, bulge-disc decompositions and stellar bulge, stellar disc, dust disc, neutral HI gas and total dynamical masses for a significant subset of the sample (  100k) spanning both the giant and dwarf galaxy populations. The survey commenced March 2008 with 50k spectra obtained in 21 clear nights using the Anglo Australian Observatory’s new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AA )

Galaxy And Mass Assembly (GAMA)

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