Constraints on the mass distribution near the centers of M31 and M32

Details Constraints on the mass distribution near the centers of M31 and M32 Constraints on the mass distribution near the centers of M31 and M32

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...353..118r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 353, April 10, 1990, p. 118-122.

Astronomy and Astrophysics

Astronomy

52

Andromeda Galaxy, Elliptical Galaxies, Galactic Nuclei, Mass Distribution, Astronomical Models, Astronomical Spectroscopy, Black Holes (Astronomy)

Scientific paper

Spectroscopic data on the motions of stars near the centers of M31 and M32 are reinterpreted. The mass distribution near the centers of each of these galaxies must be more concentrated than the light. Models are constructed containing black holes in the mass range (4-5) x 10 to the 7th solar mass for M31 and (0.7-3) x 10 to the 6th solar mass for M32. Extended models of the unseen mass must have core radii less than 0.4 arcsec and must contain about 10 to the 8th solar mass for M31 and about 10 to the 7th solar mass for M32. There are two astrophysical constraints on extended models: (1) the objects that comprise them must not collide frequently; and (2) the two-body relaxation time must be long enough that the nuclei have not already collapsed.

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