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A New Mass Model for M31

Published online by Cambridge University Press:  01 August 2006

Marc S. Seigar ,
Aaron J. Barth  and
James S. Bullock
Marc S. Seigar
Affiliation:
Center for Cosmology, Department of Physics & Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
Aaron J. Barth
Affiliation:
Center for Cosmology, Department of Physics & Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
James S. Bullock
Affiliation:
Center for Cosmology, Department of Physics & Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA
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Abstract

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A new mass model for M31 is presented. The best possible baryonic mass profile for M31 is derived from the 2MASS Ks-band image and M/L ratios from Bell et al. (2003). The best fitting rotation curve is then found within the context of ΛCDM disk galaxy formation. We find that M31 is well-described by a model that includes an adiabatically contracted halo, with an initial NFW concentration, c = 20. Models without adiabatic contraction fail to reproduce the observed rotation curve at r>15 kpc. The derived halo virial mass is Mvir = (9.4 ± 0.8) × 1011M⊙, consistent with masses derived from other observational methods.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 135
Copyright
Copyright © International Astronomical Union 2007

References

Bell, E.F., McIntosh, D.H., Katz, N., & Weinberg, M.D. 2003, ApJ 585, 117.CrossRefGoogle Scholar
Côté, P., Mateo, M., Sargent, W.L.W., & Olszewski, E.W. 2000, ApJ 537, L91.CrossRefGoogle Scholar
Seigar, M.S., Barth, A.J., & Bullock, J.S. 2006, ApJ submitted.Google Scholar