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Conference Paper

Galaxy And Mass Assembly (GAMA)


Baldry,  I. K.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;


Tuffs,  R.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Driver, S. P., Baldry, I. K., Bamford, S., Bland-Hawthorn, J., Bridges, T., Cameron, E., et al. (in press). Galaxy And Mass Assembly (GAMA).

Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-7B42-D
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 ).