Variable Energy Injection by a Near-Relativistic Outflow in APM 08279+5255.

Details Variable Energy Injection by a Near-Relativistic Outflow in APM 08279+5255. Variable Energy Injection by a Near-Relativistic Outflow in APM 08279+5255.

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.190s&link_type=abstract

Chandra's First Decade of Discovery, Proceedings of the conference held 22-25 September, 2009 in Boston, MA. Edited by Scott Wo

Physics

Accretion And Outflows

Scientific paper

We present results from multi-epoch spectral analysis of XMM-Newton and Chandra observations of the broad absorption line (BAL) quasar APM 08279+5255. Our analysis shows significant X-ray BALs in all epochs with rest- frame energies lying in the range of ˜ 6.7--17 keV. The X-ray BALs and 0.2--10 keV continuum show significant variability on timescales as short as 3.3 days (proper time) confirming the intrinsic nature of the absorbing outflow and implying a source size-scale of ˜10 rg, where, rg is the gravitational radius. The fitted width of the X-ray absorption troughs imply a large gradient in the outflow velocity of the X-ray absorbers with projected outflow velocities of up to 0.76c. The detected projected maximum outflow velocity of v ˜ 0.76c constrains the angle between the wind velocity and our line of sight to <22 deg. Such a small angle is consistent with the unification scheme of BAL and non-BAL quasars that posits that BAL quasars are viewed almost along the outflow direction. We found a possible trend between the X-ray photon index and the maximum outflow velocity of the ionized X-ray absorber in the sense that flatter X- ray spectra appear to result in lower outflow velocities. We provide a plausible explanation for this effect. Our results on APM 08279+5255 imply that quasar winds are massive and energetic enough to influence significantly the formation of the host galaxy, provide significant metal enrichment to the ISM and IGM, and are a viable mechanism for feedback at redshifts near the peak in the number density of galaxy mergers.

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