1994/09/01 by Andrew Gould, Gould, Andrew
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #History and Developments in Astronomy #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9409001
15 pages, no figures, PostScript file, or request PostScript file to [email protected], OSU-TA-17/94
arxiv created 1994/09/01 · openalex publication_date 1994/09/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The transverse velocity of a spiral galaxy can be measured to an accuracy ∼ 60 \kms by making parallax observations of quasars being microlensed by stars in the disk of the galaxy. To make the measurement, a quasar must be located behind the disk of the galaxy between about 1 and 2 scale lengths from the center. The quasar must then be monitored for microlensing events and the events followed simultaneously from the Earth and a satellite in solar orbit, preferably at ∼ 30 AU. A systematic search in a volume within 21,000 \kms could locate quasars with B<23 behind a total of ∼ 1900 galaxies. The rate of lensing events (and hence galaxy velocity measurements) would be ∼ 3 \rm yr-1. The events would have typical characteristic times ω-1∼ 3 yr. Under the assumption that the mass spectrum of lensing objects is the same in other spiral galaxies as in our own, the observations could be used to measure the Hubble parameter to an accuracy of 5%.