A revised Λ CDM mass model for the Andromeda Galaxy
Corresponding Author
Marc S. Seigar
Department of Physics and Astronomy, University of Arkansas at Little Rock, 2801 S. University Avenue, Little Rock, AR 72204, USA
Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Arkansas Center for Space and Planetary Sciences, 202 Old Museum Building, University of Arkansas, Fayetteville, AR 72701, USA
E-mail: [email protected]Search for more papers by this authorAaron J. Barth
Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Search for more papers by this authorJames S. Bullock
Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Search for more papers by this authorCorresponding Author
Marc S. Seigar
Department of Physics and Astronomy, University of Arkansas at Little Rock, 2801 S. University Avenue, Little Rock, AR 72204, USA
Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Arkansas Center for Space and Planetary Sciences, 202 Old Museum Building, University of Arkansas, Fayetteville, AR 72701, USA
E-mail: [email protected]Search for more papers by this authorAaron J. Barth
Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Search for more papers by this authorJames S. Bullock
Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Search for more papers by this authorABSTRACT
We present an updated mass model for M31 that makes use of a Spitzer 3.6-μm image, a mass-to-light ratio gradient based on the galaxy's B−R colour profile, and observed rotation curve data from a variety of sources. We examine cases where the dark matter follows a pure Navarro, Frenk & White (NFW) profile and where an initial NFW halo contracts adiabatically in response to the formation of the galaxy. We find that both of these scenarios can produce a reasonable fit to the observed rotation curve data. However, a pure NFW model requires a concentration cvir= 51 which is well outside the range predicted in Λcold dark matter cosmology and is therefore disfavoured. An adiabatically contracted NFW halo favours an initial concentration cvir= 20 and virial mass 8.2 × 1011 M⊙, and this is in line with the cosmological expectations for a galaxy of the size of M31. The best-fitting mass is consistent with published estimates from Andromeda Stream kinematics, satellite galaxy radial velocities and planetary nebulae studies. Finally, using the known linear correlation between rotation curve shear and spiral arm pitch angle, we show that the stellar spiral arm pitch angle of M31 (which cannot be deduced from imaging data due to the galaxy's inclination) is P=247 ± 44.
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