Candidate type II quasars from the Sloan Digital Sky Survey.: I.: Selection and optical properties of a sample at 0.3 < Z < 0.83

被引：306

作者：

Zakamska, NL

Strauss, MA

Krolik, JH

Collinge, MJ

Hall, PB

Hao, L

Heckman, TM

Ivezic, Z

Richards, GT

Schlegel, DJ

Schneider, DP

Strateva, I

Vanden Berk, DE

Anderson, SF

Brinkmann, J

机构：

[1] Princeton Univ Observ, Princeton, NJ 08544 USA

[2] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[3] Penn State Univ, Dept Astron & Astrophys, Davy Lab 525, University Pk, PA 16802 USA

[4] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA

[5] Univ Washington, Dept Astron, Seattle, WA 98195 USA

[6] Apache Point Observ, Sunspot, NM 88349 USA

来源：

ASTRONOMICAL JOURNAL | 2003年 / 126卷 / 05期

关键词：

galaxies : active; quasars : emission lines; quasars : general; surveys;

D O I：

10.1086/378610

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Type II quasars are the long-sought luminous analogs of type 2 (narrow emission line) Seyfert galaxies, suggested by unification models of active galactic nuclei (AGNs) and postulated to account for an appreciable fraction of the cosmic hard X-ray background. We present a sample of 291 type II AGNs at redshifts 0.3<Z<0.83 from the spectroscopic data of the Sloan Digital Sky Survey. These objects have narrow (FWHM<2000 km s(-1)), high equivalent width emission lines with high-ionization line ratios. We describe the selection procedure and discuss the optical properties of the sample. About 50% of the objects have [O III] λ5008 line luminosities in the range 3x10(8)-10(10) L-⊙, comparable to those of luminous (-27<M-B<-23) quasars; this, along with other evidence, suggests that the objects in the luminous subsample are type II quasars.

引用

页码：2125 / 2144

页数：20

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Candidate type II quasars from the Sloan Digital Sky Survey.: I.: Selection and optical properties of a sample at 0.3 &lt; Z &lt; 0.83

Candidate type II quasars from the Sloan Digital Sky Survey.: I.: Selection and optical properties of a sample at 0.3 < Z < 0.83