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THE QUASAR ACCRETION DISK SIZE-BLACK HOLE MASS RELATION

Christopher W. MorganDepartment of Physics, United States Naval Academy, 572C Holloway Road, Annapolis, MD 21402, USA; [email protected]C. S. KochanekDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210-1173, USA; [email protected], [email protected]Nicholas D. MorganDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210-1173, USA; [email protected], [email protected]Emilio E. FalcoHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]

2010en

ABI

Annotatsiya

We use the microlensing variability observed for nine gravitationally lensed quasars to show that the accretion disk size at 2500 Angstroms is related to the black hole mass by log(R_2500/cm) = (15.6+-0.2) + (0.54+-0.28)log(M_BH/10^9M_sun). This scaling is consistent with the expectation from thin disk theory (R ~ M_BH^(2/3)), but it implies that black holes radiate with relatively low efficiency, log(eta) = -1.29+-0.44 + log(L/L_E) where eta=L/(Mdot c^2). These sizes are also larger, by a factor of ~3, than the size needed to produce the observed 0.8 micron quasar flux by thermal radiation from a thin disk with the same T ~ R^(-3/4) temperature profile. More sophisticated disk models are clearly required, particularly as our continuing observations improve the precision of the measurements and yield estimates of the scaling with wavelength and accretion rate.

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DOI: 10.1088/0004-637x/712/2/1129

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