期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 425, 期 4, 页码 2741-2765出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2012.21290.x
关键词
surveys; galaxies: fundamental parameters; galaxies: kinematics and dynamics; galaxies: photometry; galaxies: spiral; galaxies: structure
资金
- Natural Sciences and Engineering Research Council of Canada
- CITA National Fellowship
- NASA through SAO Award [2834-MIT-SAO-4018, NAS8-03060]
- 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
- Max Planck Institute for Astrophysics
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
We have compiled a sample of 3041 spiral galaxies with multiband gri imaging from the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7; Abazajian et al. 2009) and available galaxy rotational velocities, V, derived from HI linewidths. We compare the data products provided through the SDSS imaging pipeline with our own photometry of the SDSS images, and use the velocities, V, as an independent metric to determine ideal galaxy sizes (R) and luminosities (L). Our radial and luminosity parameters improve upon the SDSS DR7 Petrosian radii and luminosities through the use of isophotal fits to the galaxy images. This improvement is gauged via VL and RV relations whose respective scatters are reduced by similar to 8 and similar to 30 per cent with our parameters compared to similar relations built with SDSS parameters. The tightest VRL relations are obtained with the i-band radius, R-23.5,R-i, measured at 23.5 mag arcsec(-2), and the luminosity L-23.5,L-i, measured within R-23.5,R-i. Our VRL scaling relations compare well, both in scatter and slope, with similar studies (though such comparisons depend sensitively on the nature and size of the compared samples). The typical slopes, b, and observed scatters, sigma, of the i-band VL, RL and RV relations are b(VL) = 0.27 +/- 0.01, b(RL) = 0.41 +/- 0.01, b(RV) = 1.52 +/- 0.07, and sigma(VL) = 0.074, sigma(RL) = 0.071, sigma(RV) = 0.154, respectively. Similar results for the SDSS g and r bands are also provided. Smaller scatters may be achieved with more pruned samples. We also compute scaling relations in terms of the baryonic mass (stars + gas), M-bar, ranging from M-bar similar or equal to 10(8.7) to 10(11.6) M-circle dot. Our baryonic velocity-mass (VM) relation has slope 0.29 +/- 0.01 and a measured scatter sigma(meas) = 0.076 dex.
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