Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 420, Issue 3, Pages 1959-1976Publisher
WILEY-BLACKWELL
DOI: 10.1111/j.1365-2966.2011.20012.x
Keywords
galaxies: evolution; galaxies: fundamental parameters; galaxies: kinematics and dynamics; radio lines: galaxies
Categories
Funding
- National Science Foundation [AST-1100968]
- Ana G. Mendez-Universidad Metropolitana
- Universities Space Research Association
- 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)
- MaxPlanck-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
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We present dynamical scaling relations for a homogeneous and representative sample of similar to 500 massive galaxies, selected only by stellar mass (>1010 M?) and redshift (0.025 < z < 0.05) as part of the ongoing GALEX Arecibo SDSS Survey. We compare baryonic TullyFisher (BTF) and FaberJackson (BFJ) relations for this sample, and investigate how galaxies scatter around the best fits obtained for pruned subsets of disc-dominated and bulge-dominated systems. The BFJ relation is significantly less scattered than the BTF when the relations are applied to their maximum samples (for the BTF, only galaxies with H i detections), and is not affected by the inclination problems that plague the BTF. Disc-dominated, gas-rich galaxies systematically deviate from the BFJ relation defined by the spheroids. We demonstrate that by applying a simple correction to the stellar velocity dispersions that depends only on the concentration index of the galaxy, we are able to bring discs and spheroids on to the same dynamical relation in other words, we obtain a generalized BFJ relation that holds for all the galaxies in our sample, regardless of morphology, inclination or gas content, and has a scatter smaller than 0.1 dex. We compare the velocitysize relation for the three dynamical indicators used in this work, i.e. rotational velocity, observed and concentration-corrected stellar dispersion. We find that discs and spheroids are offset in the stellar dispersionsize relation, and that the offset is removed when corrected dispersions are used instead. The generalized BFJ relation represents a fundamental correlation between the global dark matter and baryonic content of galaxies, which is obeyed by all (massive) systems regardless of morphology.
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