Candidate Type II Quasars from the Sloan Digital Sky Survey. I. Selection and Optical Properties of a Sample at 0.3 < Z < 0.83

By N. Zakamska, M. Strauss, Julian Krolik, M. Collinge, P. Hall, L. Hao, T. Heckman, Željko Ivezic´, Gordon Richards, David Schlegel and 5 more. 2003

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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 3 × 108–1010 L⊙, comparable to those of luminous (-27 < MB < -23) quasars; this, along with other evidence, suggests that the objects in the luminous subsample are type II quasars.

Subfields: Astronomy and Astrophysics

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Nuclear Activity in Nearby Galaxies (2008, background): “With an ionization potential of 97 eV, [Ne V] unambiguously arises from nonstellar excitation, but the practical difficulty is that these lines are quite weak (strength ∼10% of [O III] λ5007) and often can only be detected with confidence in stacked spectra (e.g., Zakamska et al. 2003).”
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The Mass Function of Active Black Holes in the Local Universe (2007, methodology): “…of the narrow-line region components, as uming that the velocity dispersion of the narrow lines is equal to that of the bulge (e.g., Nelson & Whittle 1996; Greene & Ho 2005a),while the narrow-line flux is fixed using the empirical relation of Zakamska et al. (2003), which relatesL[OIII] to L5100.”
A Comprehensive Study of 2000 Narrow Line Seyfert 1 Galaxies from the Sloan Digital Sky Survey. I. The Sample (2006, background): “The best linear fit to the data points yields logfkLk(5100)g¼ (7:11 0:56)þ (0:885 0:0133) log fL½O iii g: ð9Þ This relation is useful for estimating the intrinsic luminosity of narrow emission-line AGNs based on [O iii] luminosity (e.g., Zakamska et al. 2003).”
The Sloan Digital Sky Survey Quasar Survey: Quasar Luminosity Function from Data Release 3 (2006, background): “…for any remaining bad fields (§ 2.3) and counting lowerluminosity AGN [i.e., Seyfert (1943) galaxies], narrow-lined AGN (e.g., Heckman 1980; Zakamska et al. 2003), and BL Lac objects (e.g., Collinge et al. 2005) would further increase the selection efficiency of AGN in general (cf., the…”
A CATALOG OF QUASAR PROPERTIES FROM SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 (2010, methodology): “This correlation is usually used to estimate the bolometric luminosity using the [OIII] λ5007 luminosity as a surrogate for type 2 quasars (e.g, Kauffmann et al. 2003; Zakamska et al. 2003; Heckman et al. 2004; Reyes et al. 2008).”
What drives the growth of black holes (2011, background): “…2010), X-ray spectroscopy of known quasars (e.g., Page et al., 2004; Comastri et al., 2011), detection of luminous, narrow emission lines (e.g., Zakamska et al., 2003; Alexander et al., 2008b; Reyes et al., 2008; Vignali et al., 2010; Gilli et al., 2010; Juneau et al., 2011), or through…”
The Relationship of Hard X-Ray and Optical Line Emission in Low-Redshift Active Galactic Nuclei (2005, background): “These data not only allow AGNs to be efficiently recognized (e.g.,Kauffmann et al. 2003;Hao et al. 2005a; Zakamska et al. 2003); the same data can be used to quantifymany of the key properties of the AGNs and their host galaxies (e.g., Kauffmann et al. 2003).”
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PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE–BULGE RELATIONS AT LOW MASS (2010, background): “One is the strong and ubiquitous [OIII ] line that has been used both to find AGNs and to determine their intrinsic luminosities (e.g., Kauffmann et al. 2003; Zakamska et al. 2003) although concerns about reddening remain (e.g., Mulchaey et al. 1994; Meléndez et al. 2008).”
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Discovery of extreme [O III] λ5007 Å outflows in high-redshift red quasars (2015, background): “For this reason, Zakamska et al. (2003), Reyes et al. (2008) and Alexandroff et al. (2013) expanded the search for type 2 quasars to FWHM(Hβ) ≤ 2000 km s−1.”
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