期刊
ASTROPHYSICAL JOURNAL
卷 794, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/0004-637X/794/2/151
关键词
Galaxy: general; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure; stars: kinematics and dynamics; stars: statistics
资金
- NSF [AST-0707901, AST-1008784, AST-0551161, AST-1108885]
- Washington NASA Space Grant Consortium
- Michigan Society
- Croatian National Science Foundation [O-1548-2009]
- Hungarian Academy of Sciences [E-1109/6/2012]
- NASA through Hubble Fellowship from the Space Telescope Science Institute [HST-HF-51285.01]
- NASA [NAS5-26555]
- NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center
- National Foundation for Science
- Higher Education and Technological Development of the Republic of Croatia
We present robust constraints from the Sloan Digital Sky Survey (SDSS) on the shape and distribution of the dark matter halo within the Milky Way (MW). Using the number density distribution and kinematics of SDSS halo stars, we probe the dark matter distribution to heliocentric distances exceeding similar to 10 kpc and galactocentric distances exceeding similar to 20 kpc. Our analysis utilizes Jeans equations to generate two-dimensional acceleration maps throughout the volume; this approach is thoroughly tested on a cosmologically derived N-body+SPH simulation of a MW-like galaxy. We show that the known accelerations (gradients of the gravitational potential) can be successfully recovered in such a realistic system. Leveraging the baryonic gravitational potential derived by Bovy & Rix, we show that the gravitational potential implied by the SDSS observations cannot be explained, assuming Newtonian gravity, by visible matter alone: the gravitational force experienced by stars at galactocentric distances of similar to 20 kpc is as much as three times stronger than what can be attributed to purely visible matter. We also show that the SDSS data provide a strong constraint on the shape of the dark matter halo potential. Within galactocentric distances of similar to 20 kpc, the dark matter halo potential is well described as an oblate halo with axis ratio q(DM)(Phi) = 0.7 +/- 0.1; this corresponds to an axis ratio q(DM)(rho) similar to 0.4 +/- 0.1 for the dark matter density distribution. Because of our precise two-dimensional measurements of the acceleration of the halo stars, we can reject several MOND models as an explanation of the observed behavior.
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