The Masses for ultraluminous X-ray sources

Details The Masses for ultraluminous X-ray sources The Masses for ultraluminous X-ray sources

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006hst..prop10814b&link_type=abstract

HST Proposal ID #10814. Cycle 15

Computer Science

Scientific paper

Ultraluminous X-ray sources are non-nuclear sources in normal disk galaxies that are either stellar mass black holes that are super-Eddington emitters, or 1E3-1E4 Msolar black holes emitting normally. We can distinguish between these models by obtaining constraints for the mass of the primary, which can be accomplished through UV objective prism spectra. This strategy begins with the optical identification of the secondary and identification of its spectral type in order to determine its mass and the Roche Lobe radius. Secondly, we need to determine whether an accretion disk is present and if its high ionization UV line luminosities point to a stellar mass black hole or a more massive object. Finally, if the black hole is 1E3-1E4 Msolar, the orbital velocity of the secondary is so large that a Doppler shift will be detectable, even at the modest resolution of the prism.

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