Mass estimate of black hole candidates GRS 1758-258 and GX 339-4 based on a transition layer model of the accretion disk and a search for x-ray jets in GRS 1758-258

Recently, the "Transition Layer Model" has been proposed as a new method for determining a compact object's mass. In this method, the unknown mass of a compact object may be determined by shifting to its PLI-QPO curve from the PLI-QPO curve of a source with a known mass. The PLI-QPO curve of a compact object relates an object's energy spectrum power-law indices (PLI) to the central frequencies of its quasi-periodic oscillations (QPO). The Transition Layer Model predicts that the black hole candidate GRS 1758-258 has a mass of 6.0 + 3.4-1.45 M⊙ and that the black hole candidate GX 339-4 is either a neutron star or black hole. We conclude that simple shifts between PLI-QPO curves of black holes does not depend on the masses of the black holes alone; the relationship between the optical depth of the corona around a black hole to the Reynolds number of the black hole's accretion disk also influences shifting between PLI-QPO curves. Also, we conclude that GRS 1758-258 does not have X-ray jets that can be detected with Chandra. We also determine what the properties of a GRS 1758-258 X-ray jet should be if GRS 1758-258 is similar to other black hole systems.