Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....75...97v&link_type=abstract
Astronomy and Astrophysics, vol. 75, no. 1-2, May 1979, p. 97-111.
Astronomy and Astrophysics
Astrophysics
81
Galactic Structure, Hydrogen Clouds, Interstellar Gas, Kinematics, Neutral Gases, Spiral Galaxies, Continuous Radiation, Data Reduction, Distribution (Property), Gas Density, Radial Velocity, Velocity Distribution
Scientific paper
The region between M81 and NGC 3077 has been observed with the Westerbork Synthesis Radio Telescope in the 21-cm line of neutral hydrogen (H I) to investigate the distribution and kinematics of intergalactic H I in the southern part of the triplet H I envelope. M81 and NGC 3077 are linked by a hydrogen bridge which is at least in part a continuation of the outer H I spiral structure of M81. NGC 3077 displays an H I tail extending northward and a large concentration of H I to the southeast beyond the Holmberg radius. The hydrogen concentration within these features is nonhomogeneous; radial velocities in the H I bridge and tail have a regular velocity gradient. A marked similarity between H I parameters observed for M81 and NGC 3077 and those reported for the Magellanic Stream and NGC 4631/56 suggests that their H I features were formed by similar mechanisms. An examination of the galactic wake hypothesis (requiring the presence of a hot halo around M81 extending to at least 46 kpc), the hypothesis suggesting that the ages of the intergalactic HI features in the M81 triplet are of the order of a Hubble time, and the tidal interaction hypothesis in the context of the present observations indicates that gravitational interaction between M81, M82 and NGC 3077 is the most likely mechanism for the formation of the H I bridge and tail.
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