期刊
ASTROPHYSICAL JOURNAL
卷 768, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/768/1/50
关键词
galaxies: dwarf; galaxies: individual (And XXVIII, And XXIX, M31); galaxies: kinematics and dynamics; Local Group
资金
- W. M. Keck Foundation
- NASA by the Space Telescope Science Institute [51316.01]
- NASA [NAS 5-26555]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica deCanarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1009973] Funding Source: National Science Foundation
We present Keck/DEIMOS spectroscopy of resolved stars in the M31 satellites And XXVIII and And XXIX. We show that these are likely self-bound galaxies based on 18 and 24 members in And XXVIII and And XXIX, respectively. And XXVIII has a systemic velocity of -331.1 +/- 1.8 km s(-1) and a velocity dispersion of 4.9 +/- 1.6 km s(-1), implying a mass-to-light ratio (within r(1/2)) of similar to 44 +/- 41. And XXIX has a systemic velocity of -194.4 +/- 1.5 km s(-1) and velocity dispersion of 5.7 +/- 1.2 km s(-1), implying a mass-to-light ratio (within r(1/2)) of similar to 124 +/- 72. The internal kinematics and implied masses of And XXVIII and And XXIX are similar to those of dwarf spheroidals (dSphs) of comparable luminosities, implying that these objects are dark-matter-dominated dwarf galaxies. Despite the large projected distances from their host (380 and 188 kpc), the kinematics of these dSph suggest that they are bound M31 satellites.
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