The 2dF-SDSS LRG and QSO Survey: The z<2.1 Quasar Luminosity Function from 5645 Quasars to g=21.85

By G. T. Richards, Scott M. Croom, S. Anderson, Joss Bland-Hawthorn, B. Boyle, R. Propris, Michael Drinkwater, Xiaohui Fan, J. Gunn, Željko Ivezic´ and 18 more. 2005

178 citations recorded by the source corpus.

We have used the 2dF instrument on the AAT to obtain redshifts of a sample of z<3, 18.0<g<21.85 quasars selected from SDSS imaging. These data are part of a larger joint programme: the 2dF-SDSS LRG and QSO Survey (2SLAQ). We describe the quasar selection algorithm and present the resulting luminosity function of 5645 quasars in 105.7 deg^2. The bright end number counts and luminosity function agree well with determinations from the 2dF QSO Redshift Survey (2QZ) data to g\sim20.2. However, at the faint end the 2SLAQ number counts and luminosity function are steeper than the final 2QZ results from Croom et al. (2004), but are consistent with the preliminary 2QZ results from Boyle et al. (2000). Using the functional form adopted for the 2QZ analysis, we find a faint end slope of beta=-1.78+/-0.03 if we allow all of the parameters to vary and beta=-1.45+/-0.03 if we allow only the faint end slope and normalization to vary. Our maximum likelihood fit to the data yields 32% more quasars than the final 2QZ parameterization, but is not inconsistent with other g>21 deep surveys. The 2SLAQ data exhibit no well defined ``break'' but do clearly flatten with increasing magnitude. The shape of the quasar luminosity function derived from 2SLAQ is in good agreement with that derived from type I quasars found in hard X-ray surveys. [Abridged]

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/820e459c740e7a247e1df177f2a4a83b13d2a5bc

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “…fit to the more recent luminosity functions in the hard X-ray, soft X-ray, and optical from Ueda et al. (2003); Hasinger, Miyaji, & Schmidt (2005); Richards et al. (2005), respectively, and find the best-fit parameters (log(L0∗/L⊙), k1, k2, log(ṅ∗/ Mpc −3Myr−1), σ∗) = (11.3, 4.0, 0.65, −6.37,…”
The bolometric quasar luminosity function at z = 0–7 (2020, background): “…et al. 1995; Schmidt et al. 1995a; Fan et al. 2001a,b, 2003, 2004; Wolf et al. 2003; Cristiani et al. 2004; Croom et al. 2004; Hunt et al. 2004; Richards et al. 2005, 2006b; Siana et al. 2006), we include only those whose quasar samples are not completely covered by the more recent work…”
What drives the growth of black holes (2011, background): “The same behaviour is also found for optically selected and radio selected AGNs (e.g., Richards et al., 2005; Bongiorno et al., 2007; Hopkins et al., 2007; Rigby et al., 2008, 2011; Croom et al., 2009; Smolčić et al., 2009).7 Obscured AGNs are found to trace the same evolution as unobscured AGNs…”
First Measurement of the Clustering Evolution of Photometrically Classified Quasars (2005, background): “At these redshifts, a ‘‘characteristic luminosity’’ for quasars (e.g., Croom et al. 2004; Richards et al. 2005) can be estimated as M g ¼ ½ 23:81, 24.74, 25.23, 25.53, 25.75].”
The 2dF-SDSS LRG and QSO Survey: the QSO luminosity function at 0.4 < z < 2.6 (2009, methodology): “…area to allow accurate measurement of QSO clustering, as well as to reduce the random errors in the measurement of the LF, spectral properties, etc. Richards et al. (2005) presented the QSO LF from an early 2SLAQ data set using 5600 QSOs; this result shows an excess over the 2QZ survey at g 21,…”
Binary Quasars in the Sloan Digital Sky Survey: Evidence for Excess Clustering on Small Scales (2005, background): “…the double–power law B-band luminosity function (Boyle et al. 2000) MB; zð Þ ¼ 100:4( lþ1) MB M B (z)½ þ 100:4( hþ1) MB M B (z)½ ; ð5Þ where l ¼ 1:58, h ¼ 3:41, and ¼ 360(h/0:50)3 Gpc 3 mag 1, which is in good agreement with the recent measurement of Richards et al. (2005) to fainter magnitudes.”
Galaxy Zoo Green Peas: discovery of a class of compact extremely star-forming galaxies (2009, background): “Looking at QSO number counts, we would expect to see∼3 per sq. degree in our magnitude range (Richards et al. 2005), leaving two Peas per square degree brighter than 20.5 magnitudes.”
The physics of the intergalactic medium (2007, methodology): “Estimates of the QSO luminosity function at z < 2.1 are provided by Croom et al. (2004) based on the 2dF redshift survey, and by Richards et al. (2005), combining data sets from the 2dF and SDSS. Richards et al. (2006) use the SDSS to measure the bright end of the QSO luminosity function and its…”
SELF-CONSISTENT MODELS OF THE AGN AND BLACK HOLE POPULATIONS: DUTY CYCLES, ACCRETION RATES, AND THE MEAN RADIATIVE EFFICIENCY (2007, background): “1 (e.g., U03; La Franca et al. 2005).”
The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes (2006, background): “The Richards et al. (2005) fit reports number densities per magnitude at an AB absolute magnitude at rest frame k ¼ 15008.”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, methodology): “…B band, so we show the predicted luminosity density in K band (left) and B band (right), as a function of redshift from z ¼ 0 to 6, based on the combined Miyaji et al. (2001), Ueda et al. (2003), Croom et al. (2004), Richards et al. (2005), Hasinger et al. (2005), and La Franca et al. (2005) QLFs.”
Strong-lensing optical depths in a ΛCDM universe – II. The influence of the stellar mass in galaxies (2007, unknown): “For the calculation of the magnification bias, we use the quasar luminosity function obtained by Richards et al. (2005) from the 2dF-SDSS LRG and Quasar Survey and Croom et al. (2004): Φ(Lg; z) = Φ∗(z) L∗g(z) "„ Lg L∗g(z) «−α + „ Lg L∗g(z) «−β#−1 .”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, methodology): “We also show for comparison the extrapolation of the SDSS-2dF quasar luminosity function from Richards et al. (2005) toz= 0 (see also Boyle et al. 2000), with the 1σ range indicated as the green shaded range at high luminosities.”
Soft X-Ray and Ultraviolet Emission Relations in Optically Selected AGN Samples (2005, background): “…flux limit in a given area that are targeted) is 95% for point sources with i < 19:1, which drops to 60% for the high-redshift selection at i ¼ 20:2 (Richards et al. 2005; Vanden Berk et al. 2005).7 SDSS DR2 contains over 35,000 AGN spectra in 2630 deg2, covering the observed 3800–91008 region…”
The 2dF-SDSS LRG and QSO survey: QSO clustering and the L-z degeneracy (2006, methodology): “Indeed, Richards et al. (2005) found by direct comparison of g and bJ magnitudes for a large sample of 2QZ QSOs that g − bJ = −0.045 ± 0.01.”
Chandra and Spitzer Unveil Heavily Obscured Quasars in the Chandra/SWIRE Survey (2006, background): “…affected by obscuration are relatively easy to detect and identify across the entire wavelength spectrum, they have been well sampled up to high redshifts and their properties, space density, luminosity function, and redshift distributions are well measured (Ueda et al. 2003; Richards et al. 2005).”
The Sloan Digital Sky Survey Quasar Survey: Quasar Luminosity Function from Data Release 3 (2006, methodology): “Richards et al. (2005) empirically find that g − bJ ∼ −0.045, thus theoretically we expect MbJ −Mi(z = 2) to be ∼ 0.71.”
Gravitationally lensed quasars and supernovae in future wide-field optical imaging surveys (2010, methodology): “We fix the faint-end slope of β = −1.45 and the bright-end slope of α = −3.31 which was obtained in the combined analysis of the SDSS and 2dF (Richards et al. 2005).”