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Discovery of the Most Distant Double-Peaked Emitter at z = 1.369

Luo, B. and Brandt, W. N. and Silverman, J. D. and Strateva, I. V. and Bauer, F. E. and Capak, P. and Kartaltepe, J. and Lehmer, B. D. and Mainieri, V. and Salvato, M. and Szokoly, G. and Schneider, D. P. and Vignali, C. (2009) Discovery of the Most Distant Double-Peaked Emitter at z = 1.369. Astrophysical Journal, 695 (2). pp. 1227-1232. ISSN 0004-637X. doi:10.1088/0004-637X/695/2/1227.

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We report the discovery of the most distant double-peaked emitter, CXOECDFS J033115.0-275518, at z = 1.369. A Keck/DEIMOS spectrum shows a clearly double-peaked broad Mg II λ2799 emission line, with FWHM ≈ 11,000 km s^(–1) for the line complex. The line profile can be well fitted by an elliptical relativistic Keplerian disk model. This is one of a handful of double-peaked emitters known to be a luminous quasar, with excellent multiwavelength coverage and a high-quality X-ray spectrum. CXOECDFS J033115.0-275518 is a radio-loud quasar with two radio lobes (FR II morphology) and a radio loudness of f_(5 GHz)/f_(4400 Å) ≈ 429. The X-ray spectrum can be modeled by a power law with photon index 1.72 and no intrinsic absorption; the rest-frame 0.5-8.0 keV luminosity is 5.0 × 10^(44) erg s^(–1). The spectral energy distribution (SED) of CXOECDFS J033115.0-275518 has a shape typical for radio-loud quasars and double-peaked emitters at lower redshift. The local viscous energy released from the line-emitting region of the accretion disk is probably insufficient to power the observed line flux, and external illumination of the disk appears to be required. The presence of a big blue bump in the SED along with the unexceptional X-ray spectrum suggest that the illumination cannot arise from a radiatively inefficient accretion flow.

Item Type:Article
Related URLs:
URLURL TypeDescription
Luo, B.0000-0002-9036-0063
Brandt, W. N.0000-0002-0167-2453
Silverman, J. D.0000-0002-0000-6977
Bauer, F. E.0000-0002-8686-8737
Capak, P.0000-0003-3578-6843
Kartaltepe, J.0000-0001-9187-3605
Lehmer, B. D.0000-0003-2192-3296
Salvato, M.0000-0001-7116-9303
Vignali, C.0000-0002-8853-9611
Additional Information:© 2009 The American Astronomical Society. Received 2008 October 20; accepted 2009 January 19; published 2009 April 7. We acknowledge financial support from NASA LTSA grant NAG5-13035 (B.L., W.N.B.), CXC grant SP8-9003A/B (B.L., W.N.B., F.E.B.), the Polanyi Program of NKTH (G.S.), and the Italian Space Agency (contracts ASI–INAF I/023/05/0 and ASI I/088/06/0) and PRIN–MIUR grant 2006-02-5203 (C.V.). We thank M. Brusa, M. Eracleous, B. P. Miller, J. Wu, and Y. Xue for helpful discussions. We also thank the referee for carefully reviewing the manuscript and providing helpful comments.
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Polanyi Program of NKTHUNSPECIFIED
Agenzia Spaziale Italiana (ASI)ASI-INAF I/023/05/0
Agenzia Spaziale Italiana (ASI)ASI I/088/06/0
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)2006-02-5203
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Subject Keywords:accretion, accretion disks; galaxies: active; galaxies: nuclei; line: profiles; quasars: emission lines
Issue or Number:2
Record Number:CaltechAUTHORS:20090831-154312839
Persistent URL:
Official Citation:Discovery of the Most Distant Double-Peaked Emitter at z = 1.369 B. Luo, W. N. Brandt, J. D. Silverman, I. V. Strateva, F. E. Bauer, P. Capak, J. Kartaltepe, B. D. Lehmer, V. Mainieri, M. Salvato, G. Szokoly, D. P. Schneider, and C. Vignali 2009 ApJ 695 1227-1232 doi: 10.1088/0004-637X/695/2/1227.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:15506
Deposited By: Tony Diaz
Deposited On:11 Sep 2009 20:49
Last Modified:08 Nov 2021 23:19

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