Discovery of probable relativistic Fe emission and absorption in the cloverleaf quasar H 1413+117

G. Chartas, M. Eracleous, X. Dai, E. Agol, S. Gallagher

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Abstract

We present results from Chandra and XMM-Newton observations of the low-ionization broad absorption line (LoBAL) quasar H 1413+117. Our spatial and spectral analysis of a recent deep Chandra observation confirms a microlensing event in a previous Chandra observation performed about five years earlier. We present constraints on the structure of the accretion flow in H 1413+117 based on the timescale of this microlensing event. Our analysis of the combined spectrum of all the images indicates the presence of two emission peaks at rest-frame energies of 5.35 and 6.32 keV, detected at the ≳98% and ≳99% confidence levels, respectively. The double-peaked Fe emission line is fit well with an accretion-disk line model; however, the best-fitting model parameters are neither well constrained nor unique. Additional observations are required to constrain the model parameters better and to confirm the relativistic interpretation of the double-peaked Fe Kα line. Another possible interpretation of the Fe emission is fluorescent Fe emission from the back side of the wind. The spectra of images C and D show significant high-energy broad absorption features that extend up to rest-frame energies of 9 and 15 keV, respectively. We propose that a likely cause of these differences is significant variability of the outflow on timescales that are shorter than the time delays between the images. The Chandra observation of H 1413+117 has made possible for the first time the detection of the inner regions of the accretion disk and/or wind and the high ionization component of the outflowing wind of a LoBAL quasar.

Original languageEnglish (US)
Pages (from-to)678-692
Number of pages15
JournalAstrophysical Journal
Volume661
Issue number2 I
DOIs
StatePublished - Jun 1 2007

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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