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Evidence of increased UV Fe II emission in quasars in candidate overdense regions

Harris, Kathryn A. and Williger, G. M. and Haberzettl, L. and Mitchell, S. and Farrah, D. and Graham, M. J. and Davé, R. and Younger, M. P. and Söchting, I. K. (2013) Evidence of increased UV Fe II emission in quasars in candidate overdense regions. Monthly Notices of the Royal Astronomical Society, 435 (4). pp. 3125-3132. ISSN 0035-8711. doi:10.1093/mnras/stt1508.

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We present evidence for a skewed distribution of UV Fe ii emission in quasars within candidate overdense regions spanning spatial scales of ∼50 Mpc at 1.11 < z < 1.67, compared to quasars in field environments at comparable redshifts. The overdense regions have an excess of high-equivalent-width sources (W2400 > 42 Å) and a dearth of low-equivalent-width sources. There are various possible explanations for this effect, including dust, Lyα fluorescence, microturbulence and iron abundance. We find that the most plausible of these is enhanced iron abundance in the overdense regions, consistent with an enhanced star formation rate in the overdense regions compared to the field.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Farrah, D.0000-0003-1748-2010
Graham, M. J.0000-0002-3168-0139
Additional Information:© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 August 8. Received 2013 August 8; in original form 2012 August 31. First published online: September 6, 2013. KAH would like to acknowledge and thank the STFC, the University of Central Lancashire and the Obs. de la Côte d’Azur for their funding and hospitality. KAH would also like thank Roger Clowes and Luis Campusano for their communications. This research uses data from the Hectospec instrument on the MMT. The authors acknowledge support from the NASA GALEX programme GI5-059, grant NNX09AQ13G. This research has used the SDSS DR7QSO catalogue (Schneider et al. 2010). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)UNSPECIFIED
University of Central LancashireUNSPECIFIED
Observatoire de la Côte d’AzurUNSPECIFIED
Subject Keywords:galaxies: abundances, galaxies: active, quasars: emission lines, large-scale structure of Universe.
Issue or Number:4
Record Number:CaltechAUTHORS:20131209-083758520
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Official Citation:Kathryn A. Harris, G. M. Williger, L. Haberzettl, S. Mitchell, D. Farrah, M. J. Graham, R. Davé, M. P. Younger, and I. K. Söchting Evidence of increased UV Fe ii emission in quasars in candidate overdense regions MNRAS (November 11, 2013) Vol. 435 3125-3132 doi:10.1093/mnras/stt1508
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42891
Deposited By: Ruth Sustaita
Deposited On:09 Dec 2013 17:43
Last Modified:10 Nov 2021 16:30

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