B. McKernan, K. E. S. Ford, B. Kocsis, Z. Haiman
(abridged) When a sufficiently massive satellite (or secondary) black hole is embedded in a gas disk around a (primary) supermassive black hole, it can open an empty gap in the disk. A gap-opening secondary close to the primary will leave an imprint in the broad component of the FeKa emission line, which varies in a unique and predictable manner. If the gap persists into the innermost disk, the effect consists of a pair of dips in the broad line which ripple blue-ward and red-ward from the line centroid energy respectively, as the gap moves closer to the primary. This ripple effect could be unambiguously detectable and allow an electromagnetic monitoring of massive black hole mergers as they occur. As the mass ratio of the secondary to primary black hole increases to q>0.01, we expect the gap to widen, possibly clearing a central cavity in the inner disk, which shows up in the broad FeKa line component. If the secondary stalls at >100r_{g} in its in-migration, due to low co-rotating gas mass, a detectable ripple effect occurs in the broad line component on the disk viscous timescale as the inner disk drains and the outer disk is dammed. If the secondary maintains an accretion disk within a central cavity, due to dam bursting or leakage, a periodic 'see-saw' oscillation effect is exhibited in the observed line profile. Here we demonstrate the range of ripple effect signatures potentially detectable with Astro-H and IXO/Athena, and oscillation effects potentially detectable with XMM or LOFT for a wide variety of merger and disk conditions. Observations of the ripple effect and periodic oscillations can be used to provide an early warning of gravitational radiation emission from the AGN.
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http://arxiv.org/abs/1303.7206
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