| Proper Motions of Dwarf Spheroidal Galaxies from Hubble Space Telescope Imaging: III. Measurement for URSA Minor (1998) | |||||||||||
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| This article presents a measurement of the proper motion of the Ursa Minor dwarf spheroidal galaxy determined from images taken with the Hubble Space Telescope in two distinct fields. Each field contains a quasi-stellar object that serves as the reference point. Integrating the motion of Ursa Minor in a realistic potential for the Milky Way produces orbital elements. The perigalacticon and apogalacticon are 40 (10, 76) and 89 (78, 160) kpc, respectively, where the values in the parentheses represent the 95% confidence intervals derived from Monte Carlo experiments. The eccentricity of the orbit is 0.39 (0.09, 0.79), and the orbital period is 1.5 (1.1, 2.7) Gyr. The orbit is retrograde and inclined by 124 degrees (94 deg, 36 deg ) to the Galactic plane. Ursa Minor is not a likely member of a proposed stream of galaxies on similar orbits around the Milky Way, nor is the plane of its orbit coincident with a recently proposed planar alignment of galaxies around the Milky Way. Comparing the orbits of Ursa Minor and Carina shows no reason for the different star formation histories of these two galaxies. Ursa Minor must contain dark matter to have a high probability of having survived disruption by the Galactic tidal force until the present.. Pub. in The Astronomical Jnl., v130 p95-115, Jul 2005. Prepared in cooperation with The State University of New Jersey, Rutgers; Space Telescope European Coordinating Facility, Germany; University of Arizona, Tucson; University of Michigan, Ann Arbor; Universidad Catolica de Chile, Santiago; and Anglo-Australian Observatory, Australia. Prepared in collaboration with U.S. Naval Observatory, Flagstaff Station, Flagstaff, AZ. Sponsored in part by the National Science Foundation under grant nos. AST 96-19524, AST 00-98518, and AST 00-98661. | |||||||||||
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