THE STRUCTURE OF THE X-RAY AND OPTICAL EMITTING REGIONS OF THE LENSED QUASAR Q 2237+0305

• Published in: The Astrophysical journal Vol. 769; no. 1; pp. 1 - 8
• Main Authors: Mosquera, A M, Kochanek, C S, Chen, B, Dai, X, Blackburne, J A, Chartas, G
• Format: Journal Article
• Language: English
• Published: United States 20-05-2013
• Subjects: ACCRETION DISKS; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; Asymptotic properties; BLACK HOLES; EMISSION; Frames; GRAVITATIONAL LENSES; HARD COMPONENT; KEV RANGE; Lenses; MASS; QUASARS; Rest; Texts; X RADIATION; X-rays
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/769/1/53

(ProQuest: ... denotes formulae and/or non-USASCII text omitted) We use gravitational microlensing to determine the size of the X-ray and optical emission regions of the quadruple lens system Q 2237+0305. The optical half-light radius, log(R sub(1/2,)V /cm) = 16.41 + or - 0.18 (at [lambda] sub(rest) = 2018 [Angstrom]), is significantly larger than the observed soft, log(R sub(1/2,soft)/cm) = ... (1-1-3.5 keV in the rest frame), and hard, log(R sub(1/2,hard)/cm) = ... (3.5-21.5 keV in the rest frame), band X-ray emission. There is weak evidence that the hard component is more compact than the soft, with log(R sub(1/2,soft)/R sub(1/2,hard)) [Asymptotically = to] ... This wavelength-dependent structure agrees with recent results found in other lens systems using microlensing techniques, and favors geometries in which the corona is concentrated near the inner edge of the accretion disk. While the available measurements are limited, the size of the X-ray emission region appears to be roughly proportional to the mass of the central black hole.