Caught in the Act; Chandra Observations of Microlensing of the Radio-Loud Quasar MG J0414+0534

Details Caught in the Act; Chandra Observations of Microlensing of the Radio-Loud Quasar MG J0414+0534 Caught in the Act; Chandra Observations of Microlensing of the Radio-Loud Quasar MG J0414+0534

2001-12-05

arxiv.org/abs/astro-ph/0112112v1

Astronomy and Astrophysics

Astrophysics

27 pages, includes 11 figures, Accepted for publication in ApJ

Scientific paper

10.1086/339162

We present results from monitoring of the distant (z = 2.64), gravitationally lensed quasar MG J0414+0534 with the Chandra X-ray Observatory. An Fe Ka line at 6.49 +/- 0.09 keV (rest-frame) with an equivalent width of ~ 190eV consistent with fluorescence from a cold medium is detected at the 99 percent confidence level in the spectrum of the brightest image A. During the last two observations of our monitoring program we detected a five-fold increase of the equivalent width of a narrow Fe Ka line in the spectrum of image B but not in the brighter image A whereas image C is too faint to resolve the line. The continuum emission component of image B did not follow the sudden enhancement of the iron line in the last two observations. We propose that the sudden increase in the iron line strength from ~ 190eV to 900eV only in image B can be explained with a caustic crossing due to microlensing that selectively enhances a strip of the line emission region of the accretion disk. The non-enhancement of the continuum emission in the spectrum of image B suggests that the continuum emission region is concentrated closer to the center of the accretion disk than the iron line emission region and the magnification caustic has not reached close enough to the former region to amplify it. A model of a caustic crossing event predicts discontinuities in the light-curve of the magnification and provides an upper limit of ~ 5 x 10^(-4) pc on the outer radius of the Fe Ka emission region. The non-detection of any relativistic or Doppler shifts of the iron line in the spectrum of image B implies that the magnification caustic for the last two observations was located at a radius greater than ~ 100 gravitational radii.

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