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All prior work on measuring the spins of stellar-mass black holes via theX-ray continuum-fitting method has relied on the use of weakly-Comptonizedspectra obtained in the thermal dominant state. Using a self-consistentComptonization model, we show that one can analyze spectra that exhibit strongpower-law components and obtain values of the inner disk radius, and hencespin, that are consistent with those obtained in the thermal dominant state.Specifically, we analyze many RXTE spectra of two black hole transients,H1743-322 and XTE J1550-564, and we demonstrate that the radius of the inneredge of the accretion disk remains constant to within a few percent as thestrength of the Comptonized component increases by an order of magnitude, i.e.,as the fraction of the thermal seed photons that are scattered approaches 25%.We conclude that the continuum-fitting method can be applied to a much widerbody of data than previously thought possible, and to sources that have neverbeen observed to enter the thermal dominant state (e.g., Cyg X-1).

Measuring Black Hole Spin via the X-ray Continuum Fitting Method: Beyond the Thermal Dominant State