Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 412, Issue 2, Pages 765-799Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2010.17950.x
Keywords
methods: data analysis; methods: observational; techniques: image processing; techniques: photometric; surveys; galaxies: fundamental parameters
Categories
Funding
- STFC
- Australian Research Council [DP0557850]
- Alfred P. Sloan Foundation
- National Science Foundation
- US 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
- Australian Research Council [DP0557850] Funding Source: Australian Research Council
- STFC [ST/H007156/1, ST/H00131X/1, ST/H00047X/1, ST/H008578/1, ST/G001995/1, ST/F002300/1, ST/H004211/1, ST/H002391/1, ST/J002291/1, PP/E001149/1, ST/G001987/1, ST/H000496/1, ST/H008519/1, ST/F002289/1, ST/G001979/1, ST/I003088/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F002289/1, ST/H00131X/1, ST/F002300/1, PP/E001149/1, ST/G001995/1, ST/H008578/1, ST/G001979/1, ST/H007156/1, ST/H002391/1, ST/H004211/1, ST/H00047X/1, ST/H000496/1, ST/H008519/1, ST/G001987/1, ST/I003088/1] Funding Source: researchfish
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In order to generate credible 0.1-2 mu m spectral energy distributions, the Galaxy and Mass Assembly (GAMA) project requires many gigabytes of imaging data from a number of instruments to be reprocessed into a standard format. In this paper, we discuss the software infrastructure we use, and create self-consistent ugrizYJHK photometry for all sources within the GAMA sample. Using UKIDSS and SDSS archive data, we outline the pre-processing necessary to standardize all images to a common zero-point, the steps taken to correct for the seeing bias across the data set and the creation of gigapixel-scale mosaics of the three 4 x 12 deg2 GAMA regions in each filter. From these mosaics, we extract source catalogues for the GAMA regions using elliptical Kron and Petrosian matched apertures. We also calculate Sersic magnitudes for all galaxies within the GAMA sample using sigma, a galaxy component modelling wrapper for galfit 3. We compare the resultant photometry directly and also calculate the r-band galaxy luminosity function for all photometric data sets to highlight the uncertainty introduced by the photometric method. We find that (1) changing the object detection threshold has a minor effect on the best-fitting Schechter parameters of the overall population (M* +/- 0.055 mag, alpha +/- 0.014, phi* +/- 0.0005 h3 Mpc-3); (2) there is an offset between data sets that use Kron or Petrosian photometry, regardless of the filter; (3) the decision to use circular or elliptical apertures causes an offset in M* of 0.20 mag; (4) the best-fitting Schechter parameters from total-magnitude photometric systems (such as SDSS modelmag or Sersic magnitudes) have a steeper faint-end slope than photometric systems based upon Kron or Petrosian measurements; and (5) our Universe's total luminosity density, when calculated using Kron or Petrosian r-band photometry, is underestimated by at least 15 per cent.
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