Journal
ASTROPHYSICAL JOURNAL
Volume 761, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/761/2/186
Keywords
galaxies: dwarf; galaxies: evolution; galaxies: individual (M101); galaxies: interactions; galaxies: ISM
Categories
Funding
- NSF [AST-0607526, AST-1108964, AST-0807873, 1066293, AST-1149491]
- NRC
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max Planck Institute for Astronomy (MPIA)
- Max Planck Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1108964] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0847696, 1149491] Funding Source: National Science Foundation
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We present a wide (8 degrees.5 x 6 degrees.7, 1050 x 825 kpc), deep (sigma(NHI) = 10(16.8)-10(17.5) cm(-2)) neutral hydrogen (H I) map of the M101 galaxy group. We identify two new Hi sources in the group environment, one an extremely low surface brightness (and hitherto unknown) dwarf galaxy, and the other a starless Hi cloud, possibly primordial in origin. Our data show that M101' s extended Hi envelope takes the form of a similar to 100 kpc long tidal loop or plume of Hi extending to the southwest of the galaxy. The plume has an Hi mass of similar to 10(8) M-circle dot and a peak column density of N-HI = 5 x 10(17) cm(-2), and while it rotates with the main body of M101, it shows kinematic peculiarities suggestive of a warp or flaring out of the rotation plane of the galaxy. We also find two new H I clouds near the plume with masses similar to 10(7) M-circle dot, similar to H I clouds seen in the M81/M82 group, and likely also tidal in nature. Comparing to deep optical imaging of the M101 group, neither the plume nor the clouds have any extended optical counterparts down to a limiting surface brightness of mu(B) = 29.5. We also trace Hi at intermediate velocities between M101 and NGC 5474, strengthening the case for a recent interaction between the two galaxies. The kinematically complex Hi structure in the M101 group, coupled with the optical morphology of M101 and its companions, suggests that the group is in a dynamically active state that is likely common for galaxies in group environments.
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