The Frequency and Radio Properties of Broad Absorption Line Quasars

By Paul Hewett, C. Foltz. 2003

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A sample of 67 broad absorption line quasars (BALQSOs) from the Large Bright Quasar Survey (LBQS) is used to estimate the observed and intrinsic fraction of BAL quasars in optically selected samples at intermediate (BJ ≃ 18.5) magnitudes. The observed BALQSO fraction in the redshift range 1.5 ≤ z ≤ 3.0 is 15% ± 3%. A well-determined empirical k-correction, to allow for the differences in the spectral energy distributions of non-BALQSOs and BALQSOs shortward of ≃2100 Å in the rest frame, is applied to the sample. The result is an estimate of the intrinsic fraction of BALQSOs of 22% ± 4% for the redshift range 1.5 ≤ z ≤ 3.0. This value is twice that commonly cited for the occurrence of BALQSOs in optically selected samples, and the figure is in reasonable agreement with that from a preliminary analysis of the SDSS Early Data Release. The fraction of BALQSOs predicted to be present in an optical survey with flux limits equivalent to that of the FIRST Bright Quasar Survey (FBQS) is shown to be ≃20%. The BALQSO fractions derived from the FBQS and the LBQS suggest that optically bright BALQSOs are half as likely as non-BALQSOs to be detectable as S1.4 GHz ≳ 1 mJy radio sources.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

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Citations in the corpus

The X-ray to optical-UV luminosity ratio of X-ray selected type 1 AGN in XMM-COSMOS (2009, background): “Assuming they constitute about 10–15% of the entire quasar population (e.g. R03, Hewett & Foltz 2003), BAL QSO may be numerous among red sources in Fig.14 and/or X-ray obscured AGN.”
The incidence of obscuration in active galactic nuclei (2013, background): “Assuming they constitute about 10–15 per cent of the entire quasar population (Richards et al. 2003; Hewett & Foltz 2003), BALQSOs may be numerous among type-12 AGN.”
THE QUASAR OUTFLOW CONTRIBUTION TO AGN FEEDBACK: VLT MEASUREMENTS OF SDSS J0318-0600 (2009, background): “Statistically, C iv BALs are seen in 20% of all quasars (Hewett & Foltz 2003).”
Soft X-Ray and Ultraviolet Emission Relations in Optically Selected AGN Samples (2005, background): “…with an observed fraction of 10%–15% in optically selected samples (Foltz et al. 1990; Weymann et al. 1991; Menou et al. 2001; Tolea et al. 2002; Hewett & Foltz 2003; Reichard et al. 2003), are known to be strongly absorbed in the soft X-ray band and thus to have steep ox values (e.g., Brandt…”
A strong redshift dependence of the broad absorption line quasar fraction (2010, methodology): “The observed C iv BALQSO fraction has been variously calculated as, among other measurements, 15±3 (Hewett & Foltz 2003), 14.0±1.0 (Reichard et al. 2003b), 12.5 (Scaringi et al. 2009), and 13.3±0.6 per cent (G09).”
A Catalog of Broad Absorption Line Quasars from the Sloan Digital Sky Survey Early Data Release (2003, background): “Hewett & Foltz (2003) report a corrected BALQSO fraction of 22 ± 4% for their sample of 42 bright (BJ < 19) quasars, Tolea, Krolik & Tsvetanov (2002) estimate a fraction of ∼ 15% from their sample of 116 quasars, and Reichard et al. (2003b) estimate a corrected fraction of 15.9±1.4% for a sample of…”
The Intrinsic Fraction of Broad Absorption Line Quasars (2008, methodology): “It is also similar to recent BI-based estimates (Hewett & Foltz 2003; Dai, Shankar & Sivakoff 2008) and consistent with the BALQSO fraction measured by Maddox et al. (2008) from a K-band selected QSO sample.”
An Exploratory Chandra Survey of a Well-defined Sample of 35 Large Bright Quasar Survey Broad Absorption Line Quasars (2006, methodology): “This sample includes all of the confirmed LBQS BAL quasars identified by Weymann et al. (1991) and Green et al. (1995); several more with more moderate absorption were subsequently found by Hewett & Foltz (2003).”
Black Hole Masses and Enrichment of z ~ 6 SDSS Quasars (2007, background): “At low and intermediate redshift, BAL QSOs account for ∼15% of the whole quasar population (Reichard et al. 2003; Hewett & Foltz 2003), but Maiolino et al. (2004a) find four BAL QSOs among the eight QSOs at 4.9 < z < 6.4 that they observe, suggesting that the most distant quasars are surrounded by…”
Quasar outflows and AGN feedback in the extreme UV: HST/COS observations of HE 0238−1904 (2013, background): “(Hewett & Foltz 2003; Ganguly & Brotherton 2008; Dai et al. 2008; Knigge et al. 2008; Dunn et al. 2012; Dai et al. 2012), and 5.”
UNIFICATION OF LUMINOUS TYPE 1 QUASARS THROUGH C iv EMISSION (2010, background): “This is important in the context of the observed BAL fraction of ∼20% (e.g., Hewett & Foltz 2003).”
The Sloan Digital Sky Survey Quasar Catalog. II. First Data Release (2003, methodology): “In the 1990s the Large Bright Quasar Survey (LBQS; Hewett, Foltz, & Chaffee 1995, 2001) presented more than 1,000 quasars, and recent results from the 2dF Quasar Survey (Croom et al. 2001) have pushed quasar survey sample sizes past the 10,000 object milestone.”
A CATALOG OF BROAD ABSORPTION LINE QUASARS IN SLOAN DIGITAL SKY SURVEY DATA RELEASE 5 (2008, methodology): “Hewett & Foltz (2003) identified a sample of 67 BAL QSOs in the Large Bright Quasar Survey (LBQS; Hewett et al. 1995, and references therein).”
Continuum and Emission-Line Properties of Broad Absorption Line Quasars (2003, background): “Weymann et al. (1991) estimated a BALQSO fraction of 12% (for 1.5 d z d 3.0), while Hewett & Foltz (2003) found an observed fraction of 15% 3% (and an intrinsic fraction of 22% 4”