Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0511513)
· On-line Data
· References in the article
· Citations to the Article (9) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (7)
· NED Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Extended X-Ray Emission from QSOs
Authors:
Stockton, Alan; Fu, Hai; Henry, J. Patrick; Canalizo, Gabriela
Affiliation:
AA(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822), AB(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822), AC(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822), AD(Department of Physics and Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 95521)
Publication:
The Astrophysical Journal, Volume 638, Issue 2, pp. 635-641. (ApJ Homepage)
Publication Date:
02/2006
Origin:
UCP
ApJ Keywords:
quasars: individual (3C 249.1), quasars: individual (4C 25.40), Galaxies: Quasars: Individual: Alphanumeric: 4C 37.43, quasars: individual (Mrk 1014), X-Rays: Galaxies
DOI:
10.1086/499036
Bibliographic Code:
2006ApJ...638..635S

Abstract

We report Chandra ACIS observations of the fields of four QSOs showing strong extended optical emission-line regions. Two of these show no evidence for significant extended X-ray emission. The remaining two fields, those of 3C 249.1 and 4C 37.43, show discrete (but resolved) X-ray sources at distances ranging from ~10 to ~40 kpc from the nucleus. In addition, 4C 37.43 also may show a region of diffuse X-ray emission extending out to ~65 kpc and centered on the QSO. It has been suggested that extended emission-line regions such as these may originate in the cooling of a hot intragroup medium. We do not detect a general extended medium in any of our fields, and the upper limits we can place on its presence indicate cooling times of at least a few 109 yr. The discrete X-ray emission sources we detect cannot be explained as the X-ray jets frequently seen associated with radio-loud quasars, nor can they be due to electron scattering of nuclear emission. The most plausible explanation is that they result from high-speed shocks from galactic superwinds resulting either from a starburst in the QSO host galaxy or from the activation of the QSO itself. Evidence from the densities and velocities found in studies of the extended optical emission around QSOs also supports this interpretation.

Based in part on data obtained with the Chandra X-Ray Observatory, which is operated for the National Aeronautics and Space Administration by the Smithsonian Astrophysical Observatory. Also based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints