2010
DOI: 10.1088/0004-6256/140/2/546
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Eddington-Limited Accretion and the Black Hole Mass Function at Redshift 6

Abstract: We present discovery observations of a quasar in the Canada-France High-z Quasar Survey (CFHQS) at redshift z = 6.44. We also use near-IR spectroscopy of nine CFHQS quasars at z ∼ 6 to determine black hole masses. These are compared with similar estimates for more luminous Sloan Digital Sky Survey (SDSS) quasars to investigate the relationship between black hole mass and quasar luminosity. We find a strong correlation between Mg ii FWHM and UV luminosity and that most quasars at this early epoch are accreting … Show more

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Cited by 363 publications
(558 citation statements)
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References 101 publications
(196 reference statements)
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“…A model involving stellar-sized seeds is below our limits (lower long-dashed curve in Fig. 1), but fixing the accretion rate at 30% of the Eddington luminosity, it is unable to explain the presence of the population of z 6 quasars (Willott et al 2010). If we increased the accretion rate to 100% Eddington, to account for z = 6 quasars, this model would overproduce the total unresolved CXRB (see Treister et al 2011, for an example of this case).…”
Section: Resultsmentioning
confidence: 56%
“…A model involving stellar-sized seeds is below our limits (lower long-dashed curve in Fig. 1), but fixing the accretion rate at 30% of the Eddington luminosity, it is unable to explain the presence of the population of z 6 quasars (Willott et al 2010). If we increased the accretion rate to 100% Eddington, to account for z = 6 quasars, this model would overproduce the total unresolved CXRB (see Treister et al 2011, for an example of this case).…”
Section: Resultsmentioning
confidence: 56%
“…More suppression is expected in the beaming directions, while we do not see any angular dependence in LAEs and LBGs distributions. Among known z>6 QSOs, our QSO is relatively faint, with M 1450Å =-25.2 and a black hole mass of 2.5×10 8 M⊙ (Willott et al 2010). The host galaxy of the QSO was not detected by ALMA (Willott et al 2013), putting tight constraints on the SFR in the QSO host.…”
Section: Physical Interpretationmentioning
confidence: 80%
“…In this paper, we report our N B906 observation of the QSO field centred on CFHQS J2329−0301 (Table 1; Willott et al 2007) at z=6.417 (Willott et al 2010). Unless otherwise stated, we adopt the following cosmology: (h, Ωm, ΩL) = (0.7, 0.3, 0.7).…”
Section: Introductionmentioning
confidence: 99%
“…At z < 0.3, we used the distribution of Netzer (2009b), which are shifted toward higher Eddington ratios with respect to the Kauffmann & Heckman (2009) distributions (see the discussion in Netzer 2009b,a). At medium to high redshift, we used the distributions of Trakhtenbrot et al (2011), Shemmer et al (2004, Netzer & Trakhtenbrot (2007), and Willott et al (2010b). This provides a SMBH mass for each chosen X-ray luminosity and Eddington ratio.…”
Section: Agn Luminosity Function and Duty Cycle Evolutionmentioning
confidence: 99%