The 2dF QSO Redshift Survey — V. The 10k catalogue

By Scott M. Croom, R. Smith, B. Boyle, T. Shanks, N. Loaring, L. Miller, I. Observatory, Liverpool John Moore's University, D. University, O. University. 2001

171 citations recorded by the source corpus.

We present a catalogue comprising over 10 000 QSOs covering an effective area of 289.6 deg2, based on spectroscopic observations with the 2-degree Field (2dF) instrument at the Anglo-Australian Telescope. This catalogue forms the first release of the 2dF QSO Redshift Survey. QSO candidates with 18.25<bJ<20.85 were obtained from a single homogeneous colour-selected catalogue based on APM measurements of UK Schmidt photographic material. The final catalogue will contain approximately 25 000 QSOs and will be released to the public at the end of 2002, one year after the observational phase is concluded.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f71f46e2b7bba361e2483b1ac2d660e4a85623f6

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Citations in the corpus

The 2dF Galaxy Redshift Survey: spectra and redshifts (2001, methodology): “The adaptive tiling algorithm also needed to cope with the requirement that the galaxy redshift survey be merged with the concurrent survey of QSO candidates (the 2dF QSO Redshift Survey: Boyle et al. 2000; Croom et al. 2001).”
The 2dF QSO Redshift Survey – XII. The spectroscopic catalogue and luminosity function (2004, methodology): “This has no significant effect on the clustering analysis of QSOs (e.g. see Croom et al. 2001a).”
The Sloan Digital Sky Survey Quasar Catalog. I. Early Data Release (2001, background): “567 quasar survey (Croom et al. 2001), which is extremely effective at identifying quasars with redshifts below 3.0 that have bJmagnitudes between 18.25 and 20.85.”
Target Selection and Validation of DESI Quasars (2022, background): “Being among the most luminous extragalactic sources, they have become a mainstay of cosmological surveys such as the 2dF Quasar Redshift Survey (Croom et al. 2001) and the Sloan Digital Sky Survey (SDSS; York et al. 2000), where they are the source of choice to study large-scale structures at high r”
The cosmological evolution of quasar black hole masses (2003, methodology): “…defined in terms of absolute B−band magnitudes, so we initially convert the bolometric luminosity estimates for our SDSS quasars into absolute B−band magnitudes, using a transformation defined by > 300 quasars common to both the SDSS and the 2dF 10K quasar catalog (Croom et al. 2001; see Appendix).”
The Sloan Digital Sky Survey Quasar Catalog. II. First Data Release (2003, background): “One of the most intensively studied quasar data sets, the Bright Quasar Survey of Schmidt & Green (1983), contains approximately 100 quasars.”
Radio Loudness of Active Galactic Nuclei: Observational Facts and Theoretical Implications (2006, background): “…1995; Condon et al. 1998), and optical massive surveys, e.g., SDSS (Sloan Digital Sky Survey) and 2dF (Two Degree Field Survey) (York et al. 2000; Croom et al. 2001), confirm very broad distribution of radio loudness among quasars but are not very conclusive about bimodality nature of this…”
The 2dF-SDSS LRG and QSO Survey: the QSO luminosity function at 0.4 < z < 2.6 (2009, background): “The 2dF QSO Redshift Survey (2QZ; Croom et al. 2001, 2004) covered an area of 720 deg2, and reached ∼1 mag fainter than the break in the QSO LF at z < 2.”
Roma-BZCAT: A multifrequency catalogue of Blazars (2008, background): “The former type is characterised by featureless optical spectra, while those of FSRQs display the prominent emission lines that are typical of QSOs.”
Spectroscopic Target Selection in the Sloan Digital Sky Survey: The Quasar Sample (2002, background): “In so doing, the SDSS Quasar Survey will also be approximately four times the size of the concurrent 2dF QSO Redshift Survey (Croom et al. 2001).”
Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, methodology): “In GOODS-S we rely on a large spectroscopic database,4 including more than 3000 sources (Cristiani et al. 2000; Croom et al. 2001; Bunker et al. 2003; Dickinson et al. 2004; Stanway et al. 2004a,b; Strolger et al. 2004; Szokoly et al. 2004; van der Wel et al. 2004; Doherty et al. 2005; Le Fèvre et…”
The Anglo-Australian Observatory 2dF facility (2002, background): “…but linked large redshift surveys where c© 2001 RAS, MNRAS 000, 1–21 the initial main projects with 2dF: one for 250,000 galaxies brighter than bJ=19.45 with a median redshift of 0.1 (Colless et al. 2001) and one for 30,000 colour-selected quasars covering redshifts up to 4 (Croom et al. 2001).”
The 2dF QSO Redshift Survey - XIV. Structure and evolution from the two-point correlation function (2004, methodology): “In order to create realistic mock QSO catalogues, the mass particles are then biased to give a similar clustering amplitude to that observed in the 2QZ (based on the results of Croom et al. 2001a).”
Soft X-Ray and Ultraviolet Emission Relations in Optically Selected AGN Samples (2005, unknown): “The advent of large-area, highly complete optical surveys like the Two-Degree Field (2DF) survey (Croom et al. 2001) and the Sloan Digital Sky Survey (SDSS; York et al. 2000), coupled with the increased sky coverage of medium-depth X-ray imaging (pointed observation with ROSAT, XMM-Newton, and…”
The evolution of faint AGN between z ' 1 and z ' 5 from the COMBO-17 survey (2003, background): “In the S11 field, the COMBO-17 sample overlaps at its bright end with the ‘2QZ’ quasar survey (Croom et al. 2001), and in the CDFS we found that a number of spectroscopically identified X-ray sources coincide with faint COMBO-17 AGN (Hasinger 2002, priv.comm.; Szokoly et al, in prep.).”
The FIRST-2MASS Red Quasar Survey (2007, methodology): “The UVX-selected sample is described in Paper I. Briefly, it was constructed by combining the Large Bright Quasar Survey (LBQS) described in Hewett et al. (1995) and the Two Degree Field QSO Redshift Survey (2QZ) described in Croom et al. (2001).”
The Cosmological Constant and Dark Energy (2002, background): “The peak is now well established, centered at z ∼ 2.5 (Croom et al., 2001; Fan et al., 2001).”