Beyond the Disk and Bulge of M31: Tracing the Transition to the Dark Halo

Details Beyond the Disk and Bulge of M31: Tracing the Transition to the Dark Halo Beyond the Disk and Bulge of M31: Tracing the Transition to the Dark Halo

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009xmm..prop...97d&link_type=abstract

XMM-Newton Proposal ID #06525003

Computer Science

Galaxies, Galactic Surveys, M31 Fov I, M31 Fov Ii, M31 Fov Iii

Scientific paper

Although they have large mass-to-light ratios, galaxy halos host many stars. The stars, which are typically old and optically dim, encode information about the halos and the process of galaxy assembly. Some stars, however, are in bright X-ray binaries (XRBs). Those XRBs in M31's halo can be detected over vast volumes with XMM-Newton. By using data from previous successful XMM-Newton programs, we need only six 20-ksec exposures to measure the gradient of XRBs beyond the D25 isophote along both the major and minor galaxy axis. By making complementary optical observations to identify counterparts, we will trace how the stellar population diminishes across the transition region connecting relatively bright areas to the outer halo, with its high ratio of mass to light.

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