XMM-Newton Observations of High-Redshift Quasars

DSpace/Manakin Repository

XMM-Newton Observations of High-Redshift Quasars

Citable link to this page

 

 
Title: XMM-Newton Observations of High-Redshift Quasars
Author: Grupe, D.; Mathur, S.; Wilkes, Belinda Jane; Osmer, P.

Note: Order does not necessarily reflect citation order of authors.

Citation: Grupe, D., S. Mathur, B. Wilkes, and P. Osmer. 2006. “XMM-Newton Observations of High-Redshift Quasars.” The Astronomical Journal 131 (1) (January): 55–69. doi:10.1086/498260.
Full Text & Related Files:
Abstract: We report on our XMM-Newton observations of the high-redshift quasars BR 2237-0607 (z = 4.558) and BR 0351-1034 (z = 4.351). We also report on XMM-Newton observations of 19 other z > 4 objects available in the public archive of which 14 were detected. We find that the optical to X-ray spectral index αox is correlated with the luminosity density at 2500 Å but does not show a correlation with redshift, which is consistent with earlier results. Radio-loud quasars are brighter and have flatter X-ray slopes compared to radio-quiet quasars. There is some evidence for the jet-dominated sources to be intrinsically absorbed. The mean intrinsic 2–10 keV power-law slope of the 10 high-redshift radio-quiet quasars in our sample for which a spectral analysis can be performed is αX = 1.21 ± 0.52 (ranging between 0.32 and 1.96), which is more like the αX = 1.19 ± 0.10 found from the ASCA observations of low-redshift narrow-line Seyfert 1 galaxies (NLS1s) but different from the αX = 0.78 ± 0.11 found for low-redshift broad-line Seyfert galaxies. The steep X-ray spectral index suggests high Eddington ratios L/LEdd. These observations give credence to the hypothesis of Mathur that NLS1s are low-luminosity cousins of high-redshift quasars. Comparison with other results from the literature indicates that perhaps the most luminous quasars, from low to high redshift, have similarly steep X-ray spectra suggestive of high Eddington luminosities.
Published Version: doi:10.1086/498260
Other Sources: https://arxiv.org/abs/astro-ph/0501521
Terms of Use: This article is made available under the terms and conditions applicable to Other Posted Material, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#LAA
Citable link to this page: http://nrs.harvard.edu/urn-3:HUL.InstRepos:30212134
Downloads of this work:

Show full Dublin Core record

This item appears in the following Collection(s)

 
 

Search DASH


Advanced Search
 
 

Submitters