Hostname: page-component-848d4c4894-x5gtn Total loading time: 0 Render date: 2024-06-06T04:27:48.163Z Has data issue: false hasContentIssue false
  • English
  • Français

Dark matter inner slope and concentration in galaxies: from the Fornax dwarf to M87

Published online by Cambridge University Press:  10 April 2015

G. A. Mamon ,
J. Chevalier ,
A. J. Romanowsky  and
R. Wojtak
G. A. Mamon
Affiliation:
Institut d'Astrophysique de Paris, UMR 7095 (CNRS & UPMC), 98 bis Bd Arago, F-75014 Paris, France, email: gam@iap.fr, jill.chevalier@gmail.com
J. Chevalier
Affiliation:
Institut d'Astrophysique de Paris, UMR 7095 (CNRS & UPMC), 98 bis Bd Arago, F-75014 Paris, France, email: gam@iap.fr, jill.chevalier@gmail.com
A. J. Romanowsky
Affiliation:
Dept. of Physics and Astronomy, San Josè State University, San Josè, CA 95192, USA Univ. of California Observatories, Santa Cruz, CA 95064, USA, email: romanow@ucolick.org
R. Wojtak
Affiliation:
Dark Cosmology Centre, DK-2100 Copenhagen, Denmark, email: wojtak@stanford.edu
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We apply two new state-of-the-art methods that model the distribution of observed tracers in projected phase space to lift the mass / velocity anisotropy (VA) degeneracy and deduce constraints on the mass profiles of galaxies, as well as their VA. We first show how a distribution function based method applied to the satellite kinematics of otherwise isolated SDSS galaxies shows convincing observational evidence of age matching: red galaxies have more concentrated dark matter (DM) halos than blue galaxies of the same stellar or halo mass. Then, applying the MAMPOSSt technique to M87 (traced by its red and blue globular clusters) we find that very cuspy DM is favored, unless we release priors on DM concentration or stellar mass (leading to unconstrained slope). For the Fornax dwarf spheroidal (traced by its metal-rich and metal-poor stars), the inner DM slope is unconstrained, with weak evidence for a core if the stellar mass is fixed. This highlights how priors are crucial for DM modeling. Finally, we find that blue GCs around M87 and metal-rich stars in Fornax have tangential outer VA.

Keywords

galaxies: elliptical and lenticularcD – dark matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S311: Galaxy Masses as Constraints of Formation Models , July 2014 , pp. 16 - 19
Copyright
Copyright © International Astronomical Union 2015 

References

Agnello, A., Evans, N. W., Romanowsky, A. J., & Brodie, J. P., 2014, MNRAS, 442, 3299Google Scholar
Amorisco, N. C., Agnello, A., & Evans, N. W., 2013, MNRAS, 429, L89Google Scholar
Battaglia, G.et al., 2006, A&A, 459, 423Google Scholar
Breddels, M. A., et al., 2013, MNRAS, 433, 3173Google Scholar
Courteau, S.et al., 2014, Reviews of Modern Physics, 86, 47Google Scholar
Dejonghe, H. & Merritt, D., 1992, ApJ, 391, 531CrossRefGoogle Scholar
Di Cintio, A., Brook, C. B., Macciò, A. V., et al., 2014, MNRAS, 437, 415Google Scholar
Dutton, A. A. & Macciò, A. V., 2014, MNRAS, 441, 3359CrossRefGoogle Scholar
Hearin, A. P. & Watson, D. F., 2013, MNRAS, 435, 1313Google Scholar
Jardel, J. R. & Gebhardt, K., 2012, ApJ, 746, 89CrossRefGoogle Scholar
Kazantzidis, S., Mayer, L., Mastropietro, C., et al., 2004, ApJ, 608, 663CrossRefGoogle Scholar
Łokas, E. L., 2009, MNRAS, 394, L102Google Scholar
Mamon, G. A., Biviano, A., & Boué, G., 2013, MNRAS, 429, 3079Google Scholar
Murphy, J. D., Gebhardt, K., & Adams, J. J., 2011, ApJ, 729, 129Google Scholar
Navarro, J. F.et al., 2004, MNRAS, 349, 1039CrossRefGoogle Scholar
Pontzen, A. & Governato, F., 2012, MNRAS, 421, 3464CrossRefGoogle Scholar
Richardson, T. & Fairbairn, M., 2013, MNRAS, 432, 3361CrossRefGoogle Scholar
Richardson, T. & Fairbairn, M., 2014, MNRAS, 441, 1584CrossRefGoogle Scholar
Strader, J.et al., 2011, ApJS, 197, 33Google Scholar
Tiret, O., Combes, F., Angus, G. W., Famaey, B., & Zhao, H. S., 2007, A&A, 476, L1Google Scholar
Walker, M. G., Mateo, M., & Olszewski, E. W., 2009, AJ, 137, 3100Google Scholar
Walker, M. G. & Peñarrubia, J., 2011, ApJ, 742, 20Google Scholar
Wojtak, R., Łokas, E. L., Mamon, G. A., et al. 2009, MNRAS, 399, 812Google Scholar
Wojtak, R., Łokas, E. L., Mamon, G. A., et al., 2008, MNRAS, 388, 815Google Scholar
Wojtak, R. & Mamon, G. A., 2013, MNRAS, 428, 2407Google Scholar
Wolf, J., Martinez, G. D., Bullock, J. S., et al., 2010, MNRAS, 406, 1220Google Scholar