Galaxy And Mass Assembly (GAMA)

TL;DR

The GAMA survey provides a comprehensive multi-wavelength galaxy database with 250,000 spectra and imaging, enabling detailed studies of galaxy properties, structures, and evolution across various environments up to redshift 0.4.

Contribution

This paper introduces the GAMA survey, a large-scale, multi-wavelength spectroscopic and imaging dataset designed for detailed galaxy analysis and cosmological studies.

Findings

Collected 50,000 spectra in initial phase

Established a multi-wavelength galaxy database

Enabled studies of galaxy mass functions and structures

Abstract

The GAMA survey aims to deliver 250,000 optical spectra (3--7Ang resolution) over 250 sq. degrees to spectroscopic limits of r_{AB} <19.8 and K_{AB}<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 (AAOmega).