Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 425, Issue 4, Pages 2610-2640Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2012.21472.x
Keywords
gravitational lensing: weak; galaxies: kinematics and dynamics; galaxies: spiral
Categories
Funding
- US Department of Energy [DE-FG03-02-ER40701]
- David & Lucile Packard Foundation
- 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
- Cambridge University
- 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
- Division Of Physics
- Direct For Mathematical & Physical Scien [1125897] Funding Source: National Science Foundation
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In this paper, we measure the optical-to-virial velocity ratios V-opt/V-200c of disc galaxies in the Sloan Digital Sky Survey (SDSS) at a mean redshift of < z > = 0.07 and with stellar masses 10(9) < M-* < 10(11) M-circle dot. V-opt/V-200c, the ratio of the circular velocity measured at the optical radius of the disc (similar to 10 kpc) to that at the virial radius of the dark matter halo (similar to 150 kpc), is a powerful observational constraint on disc galaxy formation. It links galaxies to their dark matter haloes dynamically and constrains the total mass profile of disc galaxies over an order of magnitude in length scale. For this measurement, we combine V-opt derived from the Tully-Fisher relation (TFR) from Reyes et al. with V-200c derived from halo masses measured with galaxy-galaxy lensing. In anticipation of this combination, we use similarly selected galaxy samples for both the TFR and lensing analysis. For three M-* bins with lensing-weighted mean stellar masses of 0.6, 2.7 and 6.5 x 10(10) M-circle dot, we find halo-to-stellar mass ratios M-200c/M-* = 41, 23 and 26, with 1 sigma statistical uncertainties of around 0.1 dex, and V-opt/V-200c = 1.27 +/- 0.08, 1.39 +/- 0.06 and 1.27 +/- 0.08 (1 sigma), respectively. Our results suggest that the dark matter and baryonic contributions to the mass within the optical radius are comparable, if the dark matter halo profile has not been significantly modified by baryons. The results obtained in this work will serve as inputs to and constraints on disc galaxy formation models, which will be explored in future work. Finally, we note that this paper presents a new and improved galaxy shape catalogue for weak lensing that covers the full SDSS Data Release 7 footprint.
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