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Galaxy and Mass Assembly (GAMA) Survey

Galaxy and Mass Assembly (GAMA) Survey . Sarah Brough. GAMA Team:. 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

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Galaxy and Mass Assembly (GAMA) Survey

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

  2. GAMA Team: Sarah Brough - Australian Astronomical Observatory

  3. 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

  4. GAMA II Baldry et al. 2010, MNRAS Sarah Brough - Australian Astronomical Observatory

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

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

  7. 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. Sarah Brough - Australian Astronomical Observatory

  8. 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:1106.1994) • 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

  9. Robotham et al. 2011, arXiv:1106.1994

  10. Robothamet al. 2011, arXiv:1106.1994 Sarah Brough - Australian Astronomical Observatory

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

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

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

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

  15. The Ultimate Galaxy Database GMRT/ASKAP VST/VISTA Radio Cont. 90cm Opt/near-IR imaging 20cm HI AGN v SFR W21 Stellar Mass HI Mass Nucleus Bar GALEX GALFIT CAS Dynamical Mass Bulge Mass Disc Mass UV Far-IR AAT Sersic index Colour Scalelength HERSCHEL Dust Mass Optical spectra Popescu & Tuffs SMBH mass Trunc. rad Dust Geom. AGN SFR Attenuation Winds  Unif. Age Metal. GANDALF

  16. 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

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