Sarah Brough - Australian Astronomical Observatory

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.

Sarah Brough - Australian Astronomical Observatory

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.

Robotham et al. 2011, arXiv:1106.1994

Sarah Brough - Australian Astronomical Observatory

Robotham et al. 2011, arXiv:1106.1994

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

Sarah Brough - Australian Astronomical Observatory

First Data Release (Driver et al., MNRAS, 2011):• http://gama-survey.org/• ~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

(<z> ~ 0.2)

Sarah Brough - Australian Astronomical Observatory

More science on its way, keep a look out!

The Ultimate Galaxy Database

Opt/near-IR imaging

Stellar MassNucleus Bar

Bulge Mass Disc Mass

Scalelength

Trunc. rad

ColourSersic index

SMBH mass

Opticalspectra

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

W21

VST/VISTA

GALEX

AAT HERSCHEL

GMRT/ASKAP

Sarah Brough - Australian Astronomical Observatory

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!