AAS 203rd Meeting, January 2004
Session 61 Galaxy Clusters and Large Scale Structure II
Oral, Tuesday, January 6, 2004, 10:00-11:30am, Centennial III

[Previous] | [Session 61] | [Next]

[61.02] An X-ray Study of Gravitational Lenses: Probing AGNs and the Cosmos with the Aid of Lensing

X. Dai (Pennsylvania State University)

Gravitational lensing of distant quasars by intervening galaxies, where multiple images are formed, is a spectacular phenomenon in the universe. With the advent of Chandra, it is possible to resolve for the first time in the X-ray band lensed quasar images with separations greater than about 0.3 arcsec. We use lensing as a tool to study AGN and Cosmology. The X-ray band probes the inner most regions of the central engines of AGN. The lensing flux magnification, ranging from a few to ~100, enables us to obtain high signal-to-noise spectra and light-curves of high redshift quasars with less observing time and allows us to search for changes in quasar spectroscopic properties and X-ray flux variability over three orders of magnitude in intrinsic X-ray luminosity. One surprising result that we found in the sample of radio-quiet, high-redshift lensed quasars is a possible \Gamma-Lx relation, which may indicate that high redshift quasars are accreting close to their Eddington limits. We also use the microlensing effects induced by stars in the lensing galaxies to study the structure of the accretion discs of AGN, which cannot be resolved by current instruments. In the case of Q2237+0305, where an X-ray microlensing event was detected, we concluded that the broad Iron line region which is affected by the GR and SR effects is smaller than the X-ray continuum region. Finally we use gravitational lensing as a tool to study Cosmology. By measuring the time-delays between different lensed images it is possible to constrain the Hubble constant independently from other techniques. We have successfully measured time-delays in two lensed systems and have placed a lower limit in a third one.

We gratefully acknowledge the financial support by NASA grant NAS 8-01128.

The author(s) of this abstract have provided an email address for comments about the abstract: xdai@astro.psu.edu

[Previous] | [Session 61] | [Next]

Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.