Velocities of stars in remote Galactic satellites and the mass of the Galaxy

Details Velocities of stars in remote Galactic satellites and the mass of the Galaxy Velocities of stars in remote Galactic satellites and the mass of the Galaxy

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345..759z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 15, 1989, p. 759-769.

Astronomy and Astrophysics

Astronomy

163

Dark Matter, Dwarf Galaxies, Globular Clusters, Local Group (Astronomy), Milky Way Galaxy, Stellar Motions, Elliptical Galaxies, Halos, Mass, Mass To Light Ratios, Statistical Analysis

Scientific paper

Observations of the two most distant known dwarf spheroidal Galactic satellites, Leo I and II, and of two remote globular clusters, Eridanus and Pal 14, are presented. It is demonstrated that etalon spectra can be used for accurate wavelength calibration across the entire observed spectral range. Measured velocities of three stars in Eridanus, two stars in Pal 14, six stars in Leo I, and five stars in Leo II are used to derive that the heliocentric systemic velocities of these systems are - 21 + or - 4, 72 + or - 4, 285 + or - 3, and 70 + or - 4 km/s, respectively. The value of the velocity for Leo I is in significant disagreement with previously published values. Timing arguments are used to estimate that the mass of the Galaxy is at least 13 x 10 to the 11th solar. This value is valid only if Leo I is gravitationally bound to the Galaxy, and arguments supporting this assumption are presented.

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