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

Kathryn A. Harris; G. M. Williger; L. Haberzettl; S. Mitchell; D. Farrah; M. J. Graham; R. Davé; M. P. Younger; I. K. Söchting

doi:10.1093/mnras/stt1508

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

Kathryn A. Harris, G. M. Williger, L. Haberzettl, S. Mitchell, D. Farrah, M. J. Graham, R. Davé, M. P. Younger, I. K. Söchting

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Abstract

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.

Original language	English
Pages (from-to)	3125-3132
Journal	Monthly Notices of the Royal Astronomical Society
Volume	435
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stt1508
Publication status	Published - 6 Sep 2013

Keywords

galaxies: abundances
galaxies: active
quasars: emission lines
large-scale structure of Universe

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10.1093/mnras/stt1508

http://adsabs.harvard.edu/abs/2013MNRAS.435.3125H

Cite this

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title = "Evidence of increased UV Fe II emission in quasars in candidate overdense regions",

abstract = "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 {\AA}) 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.",

keywords = "galaxies: abundances, galaxies: active, quasars: emission lines, large-scale structure of Universe",

author = "Harris, {Kathryn A.} and Williger, {G. M.} and L. Haberzettl and S. Mitchell and D. Farrah and Graham, {M. J.} and R. Dav{\'e} and Younger, {M. P.} and S{\"o}chting, {I. K.}",

year = "2013",

month = sep,

day = "6",

doi = "10.1093/mnras/stt1508",

language = "English",

volume = "435",

pages = "3125--3132",

journal = "Monthly Notices of the Royal Astronomical Society ",

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publisher = "Oxford University Press",

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TY - JOUR

T1 - Evidence of increased UV Fe II emission in quasars in candidate overdense regions

AU - Harris, Kathryn A.

AU - Williger, G. M.

AU - Haberzettl, L.

AU - Mitchell, S.

AU - Farrah, D.

AU - Graham, M. J.

AU - Davé, R.

AU - Younger, M. P.

AU - Söchting, I. K.

PY - 2013/9/6

Y1 - 2013/9/6

N2 - 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.

AB - 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.

KW - galaxies: abundances

KW - galaxies: active

KW - quasars: emission lines

KW - large-scale structure of Universe

U2 - 10.1093/mnras/stt1508

DO - 10.1093/mnras/stt1508

M3 - Article

VL - 435

SP - 3125

EP - 3132

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -

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

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Keywords

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