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Gas kinematics in M31

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Abstract

The systemic velocity of M31, rotation and expansion velocities as functions of galactocentric distance have been derived from all data available on the radial velocity field of the Andromeda galaxy. The bending of the outer parts of the M31 disk has been considered. The calculations confirm the existence of gas outflow from the central parts of the galaxy. The obtained rotation curve is rather flat from 5 to 37 kpc. The spiral arms cause the waves both in the rotation and expansion curve. The new rotation curve is given in Table III.

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Authors and Affiliations

  1. W. Struve Astrophysical Observatory, Tôravere, Estonia, USSR

    Urmas Haud

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  1. Urmas Haud
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Haud, U. Gas kinematics in M31. Astrophys Space Sci 76, 477–490 (1981). https://doi.org/10.1007/BF00687507

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  • DOI: https://doi.org/10.1007/BF00687507

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