SIMBAD references

We analyze V-, I-, and H-band HST images and two seasons of R-band monitoring data for the gravitationally lensed quasar SDSS 0924+0219. We clearly see that image D is a point-source image of the quasar at the center of its host galaxy. We can easily track the host galaxy of the quasar close to image D because microlensing has provided a natural coronograph that suppresses the flux of the quasar image by roughly an order of magnitude. We observe low-amplitude, uncorrelated variability between the four quasar images due to microlensing, but no correlated variations that could be used to measure a time delay. Monte Carlo models of the microlensing variability provide estimates of the mean stellar mass in the lens galaxy (0.03 h² M_☉≲<M>≲2.0 h² M_☉), the accretion disk size (the disk temperature is 5x10⁴ K at 1.3x10¹⁴ h^–1 cm≲r_s≲4.7x10¹⁴ h^–1 cm), and the black hole mass (6.6x10⁶ M_☉≲M_BHh^3/2 η^–1/2_0.1(L/L_Edd)^1/2≲4.4x10⁷ M_☉), all at 68% confidence. The black hole mass estimate based on microlensing is mildly inconsistent with an estimate of M_BH=(2.8±0.9)x10⁸ M_☉ from the Mg II emission-line width. If we extrapolate the best-fitting light curve models into the future, we expect images A and B to fade and images C and D to brighten. In particular, we estimate that image D has a roughly 16% probability of brightening by a factor of 2 during the next year and a 40% probability of brightening by an order of magnitude over the next decade.