TY - JOUR
T1 - An FeLoBAL binary quasar
AU - Gregg, Michael D.
AU - Becker, Robert H.
AU - White, Richard L.
AU - Richards, Gordon T.
AU - Chaffee, Fred H.
AU - Fan, Xiaohui
N1 - Funding Information:
We thank Mark Lacy for helpful discussions. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Part of the work reported here was done at the Institute of Geophysics and Planetary Physics, under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under contract W-7405-Eng-48. Funding for the creation and distribution of the SDSS10 archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.
Funding Information:
9 The Image Reduction and Analysis Facilities package is distributed by the NOAO, which is operated by AURA, Inc., under contract to the National Science Foundation.
Funding Information:
1Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the financial support of the W. M. Keck Foundation. 2Department of Physics, University of California at Davis, 1 Shields Avenue, Davis, CA 95616-8677; [email protected], [email protected]. 3Institute for Geophysics and Planetary Physics, L-413, Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94550. 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; [email protected]. 5Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802; [email protected]. 6W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743; [email protected]. 7Institute for Advanced Study, Einstein Drive, Princeton, NJ 80540; [email protected]. 8See http://cfa-www.harvard.edu/castles (C. S. Kochanek, E. E. Falco, C. Impey, J. Lehar, B. McLeod, & H.-W. Rix).
PY - 2002/7/10
Y1 - 2002/7/10
N2 - In an ongoing infrared imaging survey of quasars at the Keck Observatory, we have discovered that the z = 1.285 quasar SDSS J233646.2-010732.6 comprises two point sources with a separation of 1″.67. Resolved spectra show that one component is a standard quasar with a blue continuum and broad emission lines; the other is a broad absorption line (BAL) quasar, specifically, a BAL QSO with prominent absorption from Mg II and metastable Fe II, making it a member of the "FeLoBAL" class. The number of known FeLoBALs has recently grown dramatically from a single example to more than a dozen, including a gravitationally lensed example and the binary member presented here, suggesting that this formerly rare object may be fairly common. Additionally, the presence of this BAL quasar in a relatively small separation binary adds to the growing evidence that the BAL phenomenon is not due to viewing a normal quasar at a specific orientation but rather that it is an evolutionary phase in the life of many, if not all, quasars and is particularly associated with conditions found in interacting systems.
AB - In an ongoing infrared imaging survey of quasars at the Keck Observatory, we have discovered that the z = 1.285 quasar SDSS J233646.2-010732.6 comprises two point sources with a separation of 1″.67. Resolved spectra show that one component is a standard quasar with a blue continuum and broad emission lines; the other is a broad absorption line (BAL) quasar, specifically, a BAL QSO with prominent absorption from Mg II and metastable Fe II, making it a member of the "FeLoBAL" class. The number of known FeLoBALs has recently grown dramatically from a single example to more than a dozen, including a gravitationally lensed example and the binary member presented here, suggesting that this formerly rare object may be fairly common. Additionally, the presence of this BAL quasar in a relatively small separation binary adds to the growing evidence that the BAL phenomenon is not due to viewing a normal quasar at a specific orientation but rather that it is an evolutionary phase in the life of many, if not all, quasars and is particularly associated with conditions found in interacting systems.
KW - Galaxies: interactions
KW - Quasars: absorption lines
KW - Quasars: general
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U2 - 10.1086/342088
DO - 10.1086/342088
M3 - Article
AN - SCOPUS:0041526293
SN - 0004-637X
VL - 573
SP - L85-L89
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 II
ER -