The prevalence of narrow optical Fe II emission lines in type 1 active galactic nuclei

Xiao Bo Dong; Luis C. Ho; Jian Guo Wang; Ting Gui Wang; Huiyuan Wang; Xiaohui Fan; Hongyan Zhou

doi:10.1088/2041-8205/721/2/L143

The prevalence of narrow optical Fe II emission lines in type 1 active galactic nuclei

Xiao Bo Dong, Luis C. Ho, Jian Guo Wang, Ting Gui Wang, Huiyuan Wang, Xiaohui Fan, Hongyan Zhou

Astronomy

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14 Scopus citations

Abstract

From detailed spectral analysis of a large sample of low-redshift active galactic nuclei (AGNs) selected from the Sloan Digital Sky Survey, we demonstrate - statistically for the first time - that narrow optical Fe _II emission lines, both permitted and forbidden, are prevalent in type 1 AGNs. Remarkably, these optical lines are completely absent in type 2 AGNs, across a wide luminosity range, from Seyfert 2 galaxies to type 2 quasars. We suggest that the narrow Fe II-emitting gas is confined to a disk-like geometry in the innermost regions of the narrow-line region on physical scales smaller than the obscuring torus.

Original language	English (US)
Pages (from-to)	L143-L147
Journal	Astrophysical Journal Letters
Volume	721
Issue number	2 PART 2
DOIs	https://doi.org/10.1088/2041-8205/721/2/L143
State	Published - Oct 1 2010

Keywords

Accretion, accretion disks
Galaxies: active
Line: formation
Line: identification
Quasars: emission lines
Radiation mechanisms: general

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/2041-8205/721/2/L143

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abstract = "From detailed spectral analysis of a large sample of low-redshift active galactic nuclei (AGNs) selected from the Sloan Digital Sky Survey, we demonstrate - statistically for the first time - that narrow optical Fe II emission lines, both permitted and forbidden, are prevalent in type 1 AGNs. Remarkably, these optical lines are completely absent in type 2 AGNs, across a wide luminosity range, from Seyfert 2 galaxies to type 2 quasars. We suggest that the narrow Fe II-emitting gas is confined to a disk-like geometry in the innermost regions of the narrow-line region on physical scales smaller than the obscuring torus.",

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T1 - The prevalence of narrow optical Fe II emission lines in type 1 active galactic nuclei

AU - Dong, Xiao Bo

AU - Ho, Luis C.

AU - Wang, Jian Guo

AU - Wang, Ting Gui

AU - Wang, Huiyuan

AU - Fan, Xiaohui

AU - Zhou, Hongyan

PY - 2010/10/1

Y1 - 2010/10/1

N2 - From detailed spectral analysis of a large sample of low-redshift active galactic nuclei (AGNs) selected from the Sloan Digital Sky Survey, we demonstrate - statistically for the first time - that narrow optical Fe II emission lines, both permitted and forbidden, are prevalent in type 1 AGNs. Remarkably, these optical lines are completely absent in type 2 AGNs, across a wide luminosity range, from Seyfert 2 galaxies to type 2 quasars. We suggest that the narrow Fe II-emitting gas is confined to a disk-like geometry in the innermost regions of the narrow-line region on physical scales smaller than the obscuring torus.

AB - From detailed spectral analysis of a large sample of low-redshift active galactic nuclei (AGNs) selected from the Sloan Digital Sky Survey, we demonstrate - statistically for the first time - that narrow optical Fe II emission lines, both permitted and forbidden, are prevalent in type 1 AGNs. Remarkably, these optical lines are completely absent in type 2 AGNs, across a wide luminosity range, from Seyfert 2 galaxies to type 2 quasars. We suggest that the narrow Fe II-emitting gas is confined to a disk-like geometry in the innermost regions of the narrow-line region on physical scales smaller than the obscuring torus.

KW - Accretion, accretion disks

KW - Galaxies: active

KW - Line: formation

KW - Line: identification

KW - Quasars: emission lines

KW - Radiation mechanisms: general

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JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 2 PART 2

ER -

The prevalence of narrow optical Fe II emission lines in type 1 active galactic nuclei

Abstract

Keywords

ASJC Scopus subject areas

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