PROBING THE DARK MATTER RADIAL PROFILE IN LENS GALAXIES AND THE SIZE OF X-RAY EMITTING REGION IN QUASARS WITH MICROLENSING

ABSTRACT We use X-ray and optical microlensing measurements to study the shape of the dark matter density profile in the lens galaxies and the size of the (soft) X-ray emission region. We show that single epoch X-ray microlensing is sensitive to the source size. Our results, in good agreement with p...

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Bibliographic Details
Published in:The Astrophysical journal 2015-06, Vol.806 (2), p.1-7
Main Authors: Jiménez-Vicente, J., Mediavilla, E., Kochanek, C. S., Muñoz, J. A.
Format: Article
Language:English
Subjects:
ACCRETION DISKS
accretion, accretion disks
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BLACK HOLES
Dark matter
Density
EMISSION
GALAXIES
galaxies: stellar content
GRAVITATIONAL LENSES
gravitational lensing: micro
Lenses
MASS
NONLUMINOUS MATTER
QUASARS
quasars: general
SOFT X RADIATION
STARS
Stellar mass
X-rays
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Summary:ABSTRACT We use X-ray and optical microlensing measurements to study the shape of the dark matter density profile in the lens galaxies and the size of the (soft) X-ray emission region. We show that single epoch X-ray microlensing is sensitive to the source size. Our results, in good agreement with previous estimates, show that the size of the X-ray emission region scales roughly linearly with the black hole mass, with a half-light radius of where . This corresponds to a size of or ∼1 lt-day for a black hole mass of . We simultaneously estimated the fraction of the local surface mass density in stars, finding that the stellar mass fraction is = 0.20 0.05 at an average radius of , where Re is the effective radius of the lens. This stellar mass fraction is insensitive to the X-ray source size and in excellent agreement with our earlier results based on optical data. By combining X-ray and optical microlensing data, we can divide this larger sample into two radial bins. We find that the surface mass density in the form of stars is = 0.31 0.15 and = 0.13 0.05 at and , respectively, in good agreement with expectations and some previous results.
ISSN:0004-637X
1538-4357
1538-4357
DOI:10.1088/0004-637X/806/2/251