SDSS J092712.65+294344.0: Recoiling Black Hole or A Sub-parsec Binary Candidate?

Details SDSS J092712.65+294344.0: Recoiling Black Hole or A Sub-parsec Binary Candidate? SDSS J092712.65+294344.0: Recoiling Black Hole or A Sub-parsec Binary Candidate?

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21332801b&link_type=abstract

American Astronomical Society, AAS Meeting #213, #328.01; Bulletin of the American Astronomical Society, Vol. 41, p.384

Astronomy and Astrophysics

Astronomy

Scientific paper

A search for recoiling supermassive black hole candidates recently yielded the best candidate thus far, SDSS J092712.65+294344.0 reported by Komossa et al. We propose the alternative hypothesis that this object is a supermassive black hole binary. From the velocity shift imprinted in the emission-line spectrum we derive the orbital period of 190 years for a binary mass ratio of 0.1, a secondary black hole mass of 100 million solar masses, and binary inclination and orbital phase angles of 45 degrees. In this model the origin of the blueshifted narrow emission lines is explained in the context of an accretion stream within the inner rim of the circumbinary disk. Within the uncertainties, this binary system can be long lived and thus, is not observed in a special moment in time. The orbital motion of the binary can potentially be observed with the VLBA if at least the secondary black hole is a radio emitter. In addition, for the parameters quoted above, the orbital motion will result in a 100 km/s velocity shift of the emission lines on a time scale of 10 yr providing a direct observational test for the binary hypothesis.

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