Determining Accurate Distances to Nearby Galaxies

Details Determining Accurate Distances to Nearby Galaxies Determining Accurate Distances to Nearby Galaxies

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.7304b&link_type=abstract

American Astronomical Society Meeting 205, #73.04; Bulletin of the American Astronomical Society, Vol. 36, p.1469

Astronomy and Astrophysics

Astronomy

Scientific paper

Distances to nearby galaxies are only known with an accuracy of 10-15%. The current anchor galaxy of the extragalactic distance scale is the Large Magellanic Cloud, which has large (10-15%) systematic uncertainties associated with it, because of its morphology, its non-uniform reddening and the unknown metallicity dependence of the Cepheid period-luminosity relation. The DIRECT Project aims to obtain a new anchor galaxy for the distance scale by measuring direct, accurate (to 5%) distances to two Local Group galaxies, M31 and M33 with detached eclipsing binaries and the Baade-Wesselink method for Cepheids. It involves a massive variability survey of these galaxies and subsequent photometric and spectroscopic follow-up of the detached binaries and Cepheids. I will describe the progress on obtaining the direct distance to a detached eclipsing binary in M33. I will also present the results of the first CCD variability study of the Draco Dwarf Spheroidal galaxy and the RR Lyrae distance derived. Finally, I will describe a "hybrid" method of discovering Cepheids with ground-based telescopes using image subtraction and then following them up with the HST to derive Cepheid period-luminosity distances.

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