Galaxy and Mass Assembly (GAMA) Survey
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Transcript of Galaxy and Mass Assembly (GAMA) Survey
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Sarah Brough - Australian Astronomical Observatory
Galaxy and Mass Assembly (GAMA) Survey
Sarah Brough
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Sarah Brough - Australian Astronomical Observatory
GAMA Team:
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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)
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Sarah Brough - Australian Astronomical Observatory
Baldry et al. 2010, MNRAS
GAMA II
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Sarah Brough - Australian Astronomical Observatory
Credit: Rob Sharp (Mount Stromlo)
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Sarah Brough - Australian Astronomical Observatory
Driver et al 2009, A&G, 50, 5.12; Driver et al 2011, MNRAS, 413, 971
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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.
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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.
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Robotham et al. 2011, arXiv:1106.1994
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Sarah Brough - Australian Astronomical Observatory
Robotham et al. 2011, arXiv:1106.1994
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Sarah Brough - Australian Astronomical Observatory
Gunawardhana et al. (2011)
Varying IMF?
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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
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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)
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Sarah Brough - Australian Astronomical Observatory
More science on its way, keep a look out!
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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
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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!