The 2dF QSO Redshift Survey – XII. The spectroscopic catalogue and luminosity function

By Scott M. Croom, R. Smith, B. Boyle, T. Shanks, L. Miller, P. Outram, N. A. A. Observatory, Liverpool Jmu, Durham, Oxford and 1 more. 2004

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We present the final catalogue of the 2dF QSO Redshift Survey (2QZ), based on Anglo-Australian Telescope 2dF spectroscopic observations of 44 576 colour-selected (ub J r) objects with 18.25 < b J < 20.85 selected from automated plate measurement scans of UK Schmidt Telescope (UKST) photographic plates. The 2QZ comprises 23 338 quasi-stellar objects (QSOs), 12 292 galactic stars (including 2071 white dwarfs) and 4558 compact narrow emission-line galaxies. We obtained a reliable spectroscopic identification for 86 per cent of objects observed with 2dF. We also report on the 6dF QSO Redshift Survey (6QZ), based on UKST 6dF observations of 1564 brighter (16 < b J < 18.25) sources selected from the same photographic input catalogue. In total, we identified 322 QSOs spectroscopically in the 6QZ. The completed 2QZ is, by more than a factor of 50, the largest homogeneous QSO catalogue ever constructed at these faint limits (b J < 20.85) and high QSO surface densities (35 QSOs deg -2 ). As such, it represents an important resource in the study of the Universe at moderate-to-high redshifts. As an example of the results possible with the 2QZ, we also present our most recent analysis of the optical QSO luminosity function and its cosmological evolution with redshift. For a flat, Ω m = 0.3 and Ω A = 0.7, universe, we find that a double power law with luminosity evolution that is exponential in look-back time, τ, of the form L* bJ (z) α e 6.15τ , equivalent to an e-folding time of 2 Gyr, provides an acceptable fit to the redshift dependence of the QSO LF over the range 0.4 < z < 2.1 and M bJ < -22.5. Evolution described by a quadratic in redshift is also an acceptable fit, with L* bJ (z) α 10 1.39 z-0.29z 2 .

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Near-Infrared Spectroscopy of High-Redshift Active Galactic Nuclei. I. A Metallicity-Accretion Rate Relationship (2004, methodology): “…5100 8 band using our new IR observations and data from the literature and compared them with the monochromatic luminosities at the rest-frame 1450 8 band obtained from the literature and from the archives of the SDSS and the Two-Degree Field (2dF) quasar redshift survey (2QZ; Croom et al. 2004).”
The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei (2004, methodology): “Yu & Tremaine used the optical QSO luminosity function of Boyle et al. (2000), which found a faintend slope of 1.58, whereas a more recent determination by Croom et al. (2004) finds a shallower slope of 1.09.”
The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, background): “…Hopkins & Beacom 2006) is also reflected in the evolution of the number density of bright Quasi-stellar Objects (QSOs) and the cosmic SMBH accretion rate density sincez ∼ 3 (Boyle & Terlevich 1998; Ueda et al. 2003; Croom et al. 2004; Silverman et al. 2008; Aird et al. 2010; Assef et al. 2011).”
A Measurement of the Quadrupole Power Spectrum in the Clustering of the 2dF QSO Survey (2005, methodology): “Details of the QSO selection of the catalog is also described in the reference Croom et al. 2004, in which the photometric and spectroscopic incompleteness is discussed, as well as the angular selection function.”
The Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: The Fourth and Fifth Data Releases (2018, background): “Especially, the milestone of discovering more than 105 new quasars has been reached thanks to the advent of two large surveys in last two decades, namely, the Two-Degree Field Quasar Redshift Survey (2dF, Croom et al. 2004) and the Sloan Digital Sky Survey (SDSS, Schneider et al. 2010).”
Active Galactic Nuclei in the Sloan Digital Sky Survey. II. Emission-Line Luminosity Function (2005, methodology): “It also agrees well with the low-redshift bin of the 2dF QSO luminosity function by Croom et al. (2004).”
Multiwavelength Study of Massive Galaxies at z ~ 2. II. Widespread Compton-thick Active Galactic Nuclei and the Concurrent Growth of Black Holes and Bulges (2007, background): “The peak of QSO activity has been established to take place at z≈ 2 (e.g., Schmidt 1968; Croom et al. 2004; Hasinger et al. 2005).”
Binary Quasars in the Sloan Digital Sky Survey: Evidence for Excess Clustering on Small Scales (2005, methodology): “Most recently, Croom et al. (2001, 2005) and Porciani et al. (2004, hereafter PMN04) measured the clustering of quasars in the redshift range z ¼ 0:3 2:2 from the 15,000 quasars in the 2dF QSO Redshift Survey (2QZ; Croom et al. 2004a).”
Supermassive black hole demography: the match between the local and accreted mass functions (2004, background): “8, the Croom et al. (2004) power-law model provides a sufficiently accurate description also of the data at z 4.”
HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, unknown): “For example, at z ≈ 2 there are ≈ 2.7 × 10−5 sub-mm galaxies per Mpc3 with M⋆ & 2 × 10 11M⊙, while the density of QSOs brighter than the corresponding luminosity of LB ≈ 1.6×10 12L⊙ (kbol ≈ 10) is ≈ 8 × 10 −7Mpc−3 (Croom et al. 2004).”
Biases in Virial Black Hole Masses: An SDSS Perspective (2007, methodology): “…< 0.35 from the SDSS. Fine et al. (2006) used composite spectra to measure the redshift evolution of the mean BH mass for the 2QZ quasar sample (Croom et al. 2004) fromz ∼ 0.5 to z ∼ 2.5, and Kollmeier et al. (2006) presented virial BH masses for a sample of 407 AGN with z∼ 0.3− 4 selected…”
EFFICIENT PHOTOMETRIC SELECTION OF QUASARS FROM THE SLOAN DIGITAL SKY SURVEY. II. ∼1, 000, 000 QUASARS FROM DATA RELEASE 6 (2004, methodology): “Since (1) the efficiency of our algorithm is so high, (2) the selection yields a redshift distribution similar to that of the 2QZ survey (Croom et al. 2004), and (3) g and BJ are roughly equivalent, we can quite easily compare the number counts distribution of our quasar candidates with that of the…”
The 2dF-SDSS LRG and QSO (2SLAQ) luminous red galaxy survey (2006, methodology): “The other was used for a lower resolution survey of faint QSOs (Richards et al. 2005; Croom et al., in preparation) which extends the earlier 2dF QSO Redshift survey (2QZ: Croom et al. 2004).”
The Cosmic Energy Inventory (2004, methodology): “As a convenient approximation to this behavior we adopt the Croom et al. (2004) luminosity evolution at z < 2.1, constant comoving luminosity density from z = 2.1 to z = 3, and negligibly small luminosity at larger redshifts.”
Luminosity-dependent evolution of soft X-ray selected AGN : New Chandra and XMM-Newton surveys (2005, methodology): “The z < 2 number density curve for optically selected QSOs (MbJ < −26.0) is from the combination of the 2dF and 6dF QSO redshift surveys by Croom et al. (2004).”
Black Hole Growth to z = 2 - I: Improved Virial Methods for Measuring M_BH and L/L_Edd (2012, methodology): “2 AGN (e.g., Croom et al. 2004; Fine et al. 2006; Shen et al. 2008; Rafiee & Hall 2011).”
CLUSTERING OF LOW-REDSHIFT (z ⩽ 2.2) QUASARS FROM THE SLOAN DIGITAL SKY SURVEY (2008, background): “…1000 deg2) surveys with efficient selection techniques, these limitations have been overcome, and the number of known quasars has increased by more than an order of magnitude in the last decade, thanks mainly to the 2dF QSO Redshift Survey (2QZ; Boyle et al. 2000; Croom et al. 2004) and the SDSS.”
The Half Million Quasars (HMQ) Catalogue (2015, methodology): “HMQ has sourced much data directly from large source catalogues like SDSS, 2QZ (Croom et al. 2004), etc., so the actual uptake from VCV consists of a residue from smaller papers which amount to 19127 type 1 objects, 1083 BL Lac objects, and 1594 type 2 objects for a total of 21794 legacy objects.”
The Sloan Digital Sky Survey Quasar Survey: Quasar Luminosity Function from Data Release 3 (2006, methodology): “Our value of A1 corresponds to a bright end slope in the Croom et al. (2004) parameterization of β = −2.95 (A1 = 0.78).”