Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 430, Issue 3, Pages 2047-2066Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt030
Keywords
galaxies: evolution; galaxies: formation; galaxies: general
Categories
Funding
- Australian Research Council [FS100100065, FS110200023]
- Science and Technology Facilities Council [ST/I000976/1]
- Marie Curie Actions of the European Commission
- Royal Society URF
- ERC StG grant [DEGAS-259586]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max-Planck-Institute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
- STFC (UK)
- ARC (Australia)
- AAO
- Science and Technology Facilities Council [ST/F002289/1, ST/I00162X/1, ST/I003088/1, ST/I000976/1, ST/G001987/1, ST/H008519/1, ST/H000496/1, ST/L001136/1, ST/H00047X/1, ST/J001465/1, ST/K00090X/1, ST/H004211/1, ST/J001422/1, ST/H002391/1, ST/I505905/1, ST/H007156/1, ST/K000845/1, ST/I001166/1, ST/H004548/1, ST/G002630/1, ST/K001116/1, ST/H008578/1, ST/G001995/1, ST/J002291/1, ST/H00131X/1, ST/J001546/1, ST/K003577/1, ST/I50563X/1, ST/J001414/1, PP/E001149/1, ST/J001651/1, ST/I001212/1] Funding Source: researchfish
- STFC [ST/K003577/1, ST/H004211/1, ST/J001465/1, ST/K000845/1, ST/H002391/1, ST/J002291/1, PP/E001149/1, ST/G002630/1, ST/G001987/1, ST/H000496/1, ST/I001166/1, ST/I00162X/1, ST/H008519/1, ST/J001651/1, ST/I001212/1, ST/K00090X/1, ST/F002289/1, ST/K001116/1, ST/H007156/1, ST/H004548/1, ST/J001546/1, ST/I505905/1, ST/J001422/1, ST/H001530/1, ST/I000976/1, ST/H00047X/1, ST/J001414/1, ST/G001995/1, ST/L001136/1, ST/I50563X/1] Funding Source: UKRI
- Australian Research Council [FS100100065, FS110200023] Funding Source: Australian Research Council
Ask authors/readers for more resources
The Galaxy And Mass Assembly (GAMA) survey is a multiwavelength photometric and spectroscopic survey, using the AAOmega spectrograph on the Anglo-Australian Telescope to obtain spectra for up to similar to 300 000 galaxies over 280 deg(2), to a limiting magnitude of r(pet) < 19.8 mag. The target galaxies are distributed over 0 < z less than or similar to 0.5 with a median redshift of z approximate to 0.2, although the redshift distribution includes a small number of systems, primarily quasars, at higher redshifts, up to and beyond z = 1. The redshift accuracy ranges from sigma(v) approximate to 50 km s(-1) to sigma(v) approximate to 100 km s(-1) depending on the signal-to-noise ratio of the spectrum. Here we describe the GAMA spectroscopic reduction and analysis pipeline. We present the steps involved in taking the raw two-dimensional spectroscopic images through to flux-calibrated one-dimensional spectra. The resulting GAMA spectra cover an observed wavelength range of 3750 less than or similar to lambda less than or similar to 8850 angstrom at a resolution of R approximate to 1300. The final flux calibration is typically accurate to 10-20 per cent, although the reliability is worse at the extreme wavelength ends, and poorer in the blue than the red. We present details of the measurement of emission and absorption features in the GAMA spectra. These measurements are characterized through a variety of quality control analyses detailing the robustness and reliability of the measurements. We illustrate the quality of the measurements with a brief exploration of elementary emission line properties of the galaxies in the GAMA sample. We demonstrate the luminosity dependence of the Balmer decrement, consistent with previously published results, and explore further how Balmer decrement varies with galaxy mass and redshift. We also investigate the mass and redshift dependencies of the [N II]/H alpha versus [O III]/H beta spectral diagnostic diagram, commonly used to discriminate between star forming and nuclear activity in galaxies.
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