期刊
ASTRONOMICAL JOURNAL
卷 142, 期 4, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-6256/142/4/130
关键词
accretion, accretion disks; line: profiles; quasars: emission lines; quasars: general; ultraviolet: galaxies; X-rays: galaxies
资金
- National Aeronautics and Space Administration [G08-9103X, NAS8-03060, 07-ADP07-0035]
- Alfred P. Sloan Research Fellowship
- National Science and Engineering Research Council of Canada
- Ontario Early Research Award
- NSF [AST-0707703]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- Cambridge University
- Case Western Reserve University
- University of Chicago
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max-PlanckInstitute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
- Science and Technology Facilities Council [ST/H004912/1, ST/H00243X/1] Funding Source: researchfish
- STFC [ST/H004912/1] Funding Source: UKRI
In the rest-frame ultraviolet (UV), two of the parameters that best characterize the range of emission-line properties in quasar broad emission-line regions are the equivalent width and the blueshift of the C IV lambda 1549 line relative to the quasar rest frame. We explore the connection between these emission-line properties and the UV through X-ray spectral energy distribution (SED) for radio-quiet (RQ) quasars. Our sample consists of a heterogeneous compilation of 406 quasars from the Sloan Digital Sky Survey (at z > 1.54) and Palomar-Green survey (at z < 0.4) that have well-measured C IV emission-line and X-ray properties (including 164 objects with measured G). We find that RQ quasars with both strong C IV emission and small C IV blueshifts can be classified as hard-spectrum sources that are (relatively) strong in the X-ray as compared to the UV. On the other hand, RQ quasars with both weak C IV emission and large C IV blueshifts are instead soft-spectrum sources that are (relatively) weak in the X-ray as compared to the UV. This work helps to further bridge optical/softX-ray eigenvector 1 relationships to the UV and hard X-ray. Based on these findings, we argue that future work should consider systematic errors in bolometric corrections (and thus accretion rates) that are derived from a single mean SED. Detailed analysis of the C IV emission line may allow for SED-dependent corrections to these quantities.
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