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We have analyzed a ~130 ks XMM-Newton observation of the dynamicallyconfirmed black hole + Wolf-Rayet (BH+WR) X-ray binary (XB) IC10 X-1, covering~1 orbital cycle. This system experiences periodic intensity dips every ~35hours. We find that energy-independent evolution is rejected at a >5 sigmalevel. The spectral and timing evolution of IC10 X-1 are best explained by acompact disk blackbody and an extended Comptonized component, where the thermalcomponent is completely absorbed and the Comptonized component is partiallycovered during the dip. We consider three possibilities for the absorber: coldmaterial in the outer accretion disk, as is well documented for Galacticneutron star (NS) XBs at high inclination; a stream of stellar wind that isenhanced by traveling through the L1 point; and a spherical wind. We estimatedthe corona radius (r_ADC) for IC10 X-1 from the dip ingress to be ~1 E+6 km,assuming absorption from the outer disk, and found it to be consistent with therelation between r_m ADC and 1--30 keV luminosity observed in Galactic NS XBsthat spans 2 orders of magnitude. For the other two scenarios, the corona wouldbe larger. Prior BH mass (M_BH) estimates range over 23--38 M_Sun, depending onthe inclination and WR mass. For disk absorption, the inclination, i, is likelyto be ~60--80 degrees, with M_BH ~24--41 M_Sun. Alternatively, the L1-enhancedwind requires i ~80 degrees, suggesting ~24--33 M_Sun. For a sphericalabsorber, i ~ 40 degrees, and M_BH ~50--65 M_Sun.

Energy-dependent evolution in IC10 X-1: hard evidence for an extended corona, and implications