Galaxy And Mass Assembly (GAMA)

Driver, S. P.; Baldry, I. K.; Bamford, S.; Bland-Hawthorn, J.; Bridges, T.; Cameron, E.; Conselice, C.; Couche, W. J.; Croom, S.; Cross, N. J. G.; Dunne, L.; Eales, S.; Edmondson, E.; Ellis, E.; Frenk, C. S.; Graham, A. W.; Jones, H.; Hill, H.; Hopkins, A.; van Kampen, E.; Kuijken, E.; Lahav, O.; Liske, J.; Loveday, J.; Nichol, B.; Norberg, B.; Norberg, P.; Oliver, S.; Parkinson, H.; Peacock, J. A.; Phillips, S.; Popescu, C.; Prescott, M.; Proctor, R.; Sharp, R.; Staveley-Smith, L.; Sutherland, W.; Tuffs, R.; Warren, S.

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Galaxy And Mass Assembly (GAMA)

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

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

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Citation

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

Abstract

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 ).