期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 462, 期 4, 页码 4336-4348出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw1861
关键词
galaxies: elliptical and lenticular, cD; galaxies: fundamental parameters; galaxies: luminosity function, mass function; galaxies: spiral; galaxies: statistics
资金
- Australian Research Council [130103505]
- STFC (UK)
- ARC (Australia)
- AAO
- 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
- La Silla Paranal Observatory [179.A-2004]
We build on a recent photometric decomposition analysis of 7506 Galaxy and Mass Assembly (GAMA) survey galaxies to derive stellar mass function fits to individual spheroid and disc component populations down to a lower mass limit of log(M*/M-circle dot) = 8. We find that the spheroid/ disc mass distributions for individual galaxy morphological types are well described by single Schechter function forms. We derive estimates of the total stellar mass densities in spheroids (rho(spheroid) = 1.24 +/- 0.49 x 10(8) M-circle dot Mpc (-3)h(0.7)) and discs (rho(disc) = 1.20 +/- 0.45 x 10(8)M(circle dot) Mpc (-3)h(0.7)), which translates to approximately 50 per cent of the local stellar mass density in spheroids and 48 per cent in discs. The remaining stellar mass is found in the dwarf 'little blue spheroid' class, which is not obviously similar in structure to either classical spheroid or disc populations. We also examine the variation of component mass ratios across galaxy mass and group halo mass regimes, finding the transition from spheroid to disc mass dominance occurs near galaxy stellar mass similar to 10(11)M(circle dot) and group halo mass similar to 10(12.5)M(circle dot) h(-1). We further quantify the variation in spheroid-to-total mass ratio with group halo mass for central and satellite populations as well as the radial variation of this ratio within groups.
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