Galaxy and Mass Assembly (GAMA) Survey Sarah Brough Sarah Brough - Australian Astronomical Observatory

GAMA Team: Sarah Brough - Australian Astronomical Observatory

An r-band selected redshift survey: – r < 19.8mag – Six regions each ~5x12 deg – ~1000 redshift targets per sq deg (2dFGRS~120, SDSS~70) – 96% complete in redshifts – Testing ΛCDM via halo mass function, galaxy merger rates, and star formation efficiency – Total allocation 178 nights A multi-wavelength study of galaxies: – FUV,NUV,ugrizYJHK,mid-IR,far-IR,20cm,21cm,1m (AGN, stars, gas, dust) – 1kpc resolution in ugrizYJHK to z<0.1 (structural analysis) – Robust halo masses (internal/external environmental markers) Sarah Brough - Australian Astronomical Observatory

Baldry et al. 2010, MNRAS GAMA II

Sarah Brough - Australian Astronomical Observatory Credit: Rob Sharp (Mount Stromlo)

Sarah Brough - Australian Astronomical Observatory Driver et al 2009, A&G, 50, 5.12; Driver et al 2011, MNRAS, 413, 971

Sarah Brough - Australian Astronomical Observatory The GAMA footprint (black rectangles). 2dFGRS (Green), SDSS (grey), WiggleZ (red), Herschel ATLAS (yellow), and VISTA VIKING (purple). Blue circles are NVSS radio continuum sources.

Key Science: A measurement of the dark matter halo mass function of groups and clusters using group velocity dispersion measurements. (Robotham et al. 2011, arXiv: ) A comprehensive determination of the galaxy stellar mass function to Magellanic Cloud masses to constrain baryonic feedback processes. (Taylor et al. submitted; Baldry et al. in prep) A direct measurement of the recent galaxy merger rates as a function of mass, mass ratio, local environment and galaxy type. Sarah Brough - Australian Astronomical Observatory

Robotham et al. 2011, arXiv:

Sarah Brough - Australian Astronomical Observatory Robotham et al. 2011, arXiv:

Sarah Brough - Australian Astronomical Observatory Gunawardhana et al. (2011) Varying IMF?

Sarah Brough - Australian Astronomical Observatory Baldry et al. (in prep) Steep upturn seen in stellar mass function even before we get deep VST data Stellar Mass Function

First Data Release (Driver et al., MNRAS, 2011): ~110,000 ugrizYHK photometric objects, to r<19.4 and r<19.8 ~50,000 with redshifts & spectra available in DR1, out to z~0.6 ( ~ 0.2) Sarah Brough - Australian Astronomical Observatory

More science on its way, keep a look out! Sarah Brough - Australian Astronomical Observatory

The Ultimate Galaxy Database Opt/near-IR imaging Stellar Mass NucleusBar Bulge MassDisc Mass Scalelength Trunc. rad ColourSersic index SMBH mass Optical spectra SFRAGN Age Metal.  Winds Far-IR Dust Mass Dust Geom. Attenuation Radio HI Cont. HI Mass Dynamical Mass AGN v SFR 20cm 90cm Unif. GANDALF GALFIT CAS UV Popescu & Tuffs W 21 VST/VISTA GALEX AAT HERSCHEL GMRT/ASKAP

SURVEY PAPERS: (Driver et al 2009, Robotham et al 2010, Baldry et al 2010, Hill et al. 2011) SCIENCE: Galaxy evolution: SFR dependence on environment, merger rate, galaxy type/morphology, mass, etc. (Brough et al. 2011, Prescott et al. submitted) Obscuration, radiation balance between UV/IR, dependence on other galaxy properties, evolution. (Wijesinghe et al. 2011a,b) IMF variations? (Gunawardhana et al. 2011) Metallicity evolution, dependence on galaxy properties, environment, etc. Cluster/group properties, evolution, role in galaxy evolution. Relationship between single-fibre galaxy properties and resolved spectroscopic properties from integral-field spectroscopic measurements. Stellar/gas inter-relationships (GAMA+DINGO): galaxy fueling/stripping/feedback, etc. Stellar mass function, HI mass function, baryonic mass function. AGN evolution, feedback mechanisms, (radio continuum from EMU). And much, much more! Sarah Brough - Australian Astronomical Observatory