Author ORCID Identifier
Document Type
Article
Publication Date
4-10-2007
Abstract
We examine the amplitude of the rotation velocity that can be attributed to the dark matter halos of disk galaxies, focusing on well-measured intermediate radii. The data for 60 galaxies spanning a large range of mass and Hubble types, taken together, are consistent with a dark halo velocity log Vh = C + B log R with C = 1.47-0.19+0.15 and B ≈1/2 over the range of 1 < R < 74 kpc. The range in C stems from different choices of the stellar mass estimator, from minimum to maximum disk. For all plausible choices of stellar mass, the implied densities of the dark halos are lower than expected from structure formation simulations in ACDM, which anticipate C > 1.6. This problem is not specific to a particular type of galaxy or to the innermost region of the halo (cusp or core); the velocity attributable to dark matter is too low at all radii. © 2007. The American Astronomical Society. All rights reserved.
Keywords
dark matter, galaxies: kinematics and dynamics, galaxies: spiral
Language
English
Publication Title
Astrophysical Journal
Grant
505956
Rights
© The American Astronomical Society. All rights reserved. This content is free to access, download, and share. For all other uses, you must obtain permission to reuse content: https://journals.aas.org/article-charges-and-copyright/#AAS_material
Recommended Citation
S. S. McGaugh et al 2007. The Rotation Velocity Attributable to Dark Matter at Intermediate Radii in Disk Galaxies. ApJ 659 149
Manuscript Version
Final Publisher Version