The 2dF QSO Redshift Survey - I. The Optical QSO Luminosity Function

By B. Boyle, T. Shanks, Scott M. Croom, R. Smith, L. Miller, N. Loaring, Catherine Heymans. 2000

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In Astronomy and Astrophysics

Citations in the corpus

Reionization of Hydrogen and Helium by Early Stars and Quasars (2002, methodology): “At redshifts below z ¼ 2:5 we use the luminosity function of Boyle et al. (2000).”
The anti‐hierarchical growth of supermassive black holes (2004, background): “R AY AC T I V E G A L AC T I C N U C L E I L U M I N O S I T Y F U N C T I O N Large optical surveys carried out in recent years (Boyle et al. 2000; Fan et al. 2001; Wolf et al. 2003) probe the evolution of the QSO luminosity function up to high redshift, and all agree in establishing a strong rise…”
The Changing Active Galactic Nucleus Population (2003, background): “Pure luminosity evolution is consistent with the most recent optical determinations (Boyle et al. 2000).”
ON THE COSMIC EVOLUTION OF THE SCALING RELATIONS BETWEEN BLACK HOLES AND THEIR HOST GALAXIES: BROAD-LINE ACTIVE GALACTIC NUCLEI IN THE zCOSMOS SURVEY (2009, result): “This is consistent with the estimate for ∆LogMBH of Lauer et al. (2007) based on the local AGN luminosity function of Boyle et al. (2000), and slightly smaller than the measured offset.”
Active Galactic Nuclei in the Sloan Digital Sky Survey. II. Emission-Line Luminosity Function (2005, background): “Many attempts have been made to derive the luminosity function of quasars (Schmidt & Green 1983; Marshall et al. 1983; Boyle et al. 1988, 1990, 2000; Hewett et al. 1993; Schmidt et al. 1995; Hawkins & Véron 1995; Koehler et al. 1997; Goldschmidt & Miller 1998; La Franca & Cristiani 1997; Fan et…”
The X-Ray-to-Optical Properties of Optically Selected Active Galaxies over Wide Luminosity and Redshift Ranges (2006, background): “5 INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy. functions derived from optical (e.g., Boyle et al. 2000; Wolf et al. 2003; Richards et al. 2005) and X-ray (e.g., Miyaji et al. 2000; Steffen et al. 2003; Ueda et al. 2003; Barger et al. 2005; Hasinger et al. 2005; La…”
The 2dF-SDSS LRG and QSO Survey: the QSO luminosity function at 0.4 < z < 2.6 (2009, background): “…AGN is to characterize and understand their strong evolution (e.g. Schmidt 1972; Braccesi et al. 1980; Schmidt & Green 1983; Boyle, Shanks & Peterson 1988, hereafter BSP88; Hewett, Foltz & Chaffee 1993; Boyle et al. 2000; Croom et al. 2004, hereafter C04; Richards et al. 2006, hereafter R06).”
THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, background): “The QLF is generally found to have the form of a broken power law (Boyle et al. 1988; Pei 1995; Boyle et al. 2000), with a steep slope towards high luminosities and a flatter slope extending to low luminosities.”
Reionization and the Cosmic Dawn with the Square Kilometre Array (2012, background): “…the IGM (Zaroubi et al. 2007; Baek et al. 2010), it has been argued that the space density of quasars at high redshifts is too small to provide a significant contribution to the ionizing flux (Loeb 2009; Schmidt et al. 1995; Boyle et al. 2000; Cristiani et al. 2004; González-Serrano et al. 2005).”
An Observational Determination of the Bolometric Quasar Luminosity Function (2006, background): “Some measured QLFs do not appear in this compilation (e.g., Boyle et al. 2000), as updated versions from the same or expanded samples exist (e.g., Croom et al. 2004).”
Quasars, their host galaxies and their central black holes (2001, methodology): “7GHz > 1 × 10 25 WHz−1sr−1 has risen to ≃ 1 × 10−6 Mpc−3 (Dunlop & Peacock 1990) while that of optically-selected quasars brighter than MV = −23 is ≃ 5 × 10−6 Mpc−3 (Warren, Hewett & Osmer 1995, Boyle et al. 2000).”
The cosmological evolution of quasar black hole masses (2003, methodology): “…of the quasar activation rates in Section 5, it was necessary to provide a calibration between the quasar bolometric luminosities estimated via the spectra modelling, and the absolute B−band magnitudes used in the Boyle et al. (2000) determination of the 2dF+LBQS quasar luminosity function.”
The 2dF QSO Redshift Survey – XII. The spectroscopic catalogue and luminosity function (2004, methodology): “Although such models with an exponential evolution in τ have previously been shown not to fit the QSO distribution (Boyle et al. 2000; La Franca & Cristiani 1997) for an EdS Universe, exponential evolution models have not been fitted to Universes with non-zero ΩΛ.”
Galaxy Zoo: 'Hanny's Voorwerp', a quasar light echo? (2009, background): “It has long been clear that the AGN population evolves over time (see e.g. Boyle et al. 2000; Wolf et al. 2003; Richards et al. 2006), but it is harder to constrain the time-scales on which individual objects undergo change.”
Cosmic X-ray surveys of distant active galaxies (2015, background): “Most analyses up to the year ≈ 2000 found that the form of the evolution at z <∼ 2.5 could be fit acceptably with pure luminosity evolution models, although there were reports of more complex evolution at bright magnitudes (e.g., Hartwick and Schade 1990; Boyle et al 2000).”
Self-regulated Growth of Supermassive Black Holes in Galaxies as the Origin of the Optical and X-Ray Luminosity Functions of Quasars (2003, methodology): “Boyle et al. (2000) found that the luminosity function at z .”
The Rest-Frame Optical Properties of SCUBA Galaxies (2004, background): “The combined population will then be about 10 times more numerous than optically selected QSOs with MB > 25 at this epoch (Boyle et al. 2000).”
The SDSS Damped Lyα Survey: Data Release 3 (2005, background): “This difference in magnitudes is significant and it nearly brackets the ‘break magnitude’ of the quasar luminosity function at z = 2 (Boyle et al. 2000).”
DISCOVERY OF THREE z > 6.5 QUASARS IN THE VISTA KILO-DEGREE INFRARED GALAXY (VIKING) SURVEY (2013, background): “The Quasar Luminosity Function at z 6.5 The quasar luminosity function, Φ(M, z), is often parameterized by a double power-law (e.g., Boyle et al. 2000; Fan et al. 2001): Φ(M, z) = 10 k(z−6)Φ(M∗, z = 6) 100.4(α+1)(M−M∗) + 100.4(β+1)(M−M∗) , (1) where α is the faint end slope, β the bright end slope,…”