The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k Catalogue

We present a power spectrum analysis of the 10K catalogue from the 2dF QSO Redshift Survey. Although the Survey currently has a patchy angular selection func- tion, we use the Virgo Consortium's Hubble Volume simulation to demonstrate that we are able to make a useful first measurement of the power spectrum over more than a decade in scale. We compare the redshift-space power spectra of QSOs to those measured for galaxies and Abell clusters at low redshift and find that they show similar shapes in their overlap range, 50-150h 1 Mpc, with PQSO(k) / k 1.4 . The amplitude of the QSO power spectrum at z � 1.4 is almost comparable to that of galaxies at the present day if m=0.3 and �=0.7 (thecosmology), and a factor of � 3 lower if m=1 (the EdS cosmology) is assumed. The amplitude of the QSO power spectrum is a factor of � 10 lower than that measured for Abell clusters at the present day. At larger scales, the QSO power spectra continue to rise robustly to � 400 h 1 Mpc, implying more power at large scales than in the APM galaxy power spectrum measured by Baugh & Efstathiou. We split the QSO sample into two redshift bins and find little evolution in the amplitude of the power spectrum, consistent with the result for the QSO correlation function. In models with m �0.1 this represents evidence for a QSO-mass bias that evolves as a function of time. The QSO power spectrum may show a spike feature at � 90h 1 Mpc assuming thecosmology or � 65h 1 Mpc assuming an EdS cosmology. Although the spike appears to reproduce in both the North and South strips and in two independent redshift ranges, its statistical significance is still marginal and more data is needed to test further its reality. We compare the QSO power spectra to CDM models to obtain a constraint on the shape parameter, . For two choices of cosmology ( m=1, �=0 and m=0.3, �=0.7), we find the best fit model has � 0.1 ± 0.1. In addition, we have shown that a power spectrum analysis of the Hubble VolumeCDM mock QSO catalogues with = 0 .17 as input, produces a result which is statistically consistent with the data. The analysis of the mock catalogues also indicates that the above results for are unlikely to be dominated by systematic effects due to the current catalogue window. We conclude that the form of the QSO power spectrum shows large-scale power significantly in excess of the standard CDM prediction, similar to that seen in local galaxy surveys at intermediate scales.

[1]  G. Luppino,et al.  Mass and Light in the Universe , 2001, astro-ph/0203172.

[2]  Oxford,et al.  The 2dF QSO Redshift Survey — II. Structure and evolution at high redshift , 2000, astro-ph/0012375.

[3]  James J. Bock,et al.  Constraints on Cosmological Parameters from MAXIMA-1 , 2000 .

[4]  Scott M. Croom,et al.  The 2dF QSO Redshift Survey — I. The optical luminosity function of quasi-stellar objects , 2000 .

[5]  Scott M. Croom,et al.  The 2dF QSO Redshift Survey - I. The Optical QSO Luminosity Function , 2000 .

[6]  A. Melchiorri,et al.  A flat Universe from high-resolution maps of the cosmic microwave background radiation , 2000, Nature.

[7]  P. Hall,et al.  The CNOC2 Field Galaxy Redshift Survey. I. The Survey and the Catalog for the Patch CNOC 0223+00 , 2000, astro-ph/0004026.

[8]  D. Eisenstein,et al.  Correlations in the Spatial Power Spectrum Inferred from Angular Clustering , 1999, astro-ph/9912149.

[9]  S. Maddox,et al.  The environments of intermediate-redshift QSOs: 0·3 < z < 0·7 , 1999, astro-ph/9911400.

[10]  S. Maddox,et al.  THE POWER SPECTRUM OF THE POINT SOURCE CATALOGUE REDSHIFT SURVEY , 1999, astro-ph/9901189.

[11]  J. Peacock,et al.  Baryonic signatures in Large-Scale Structure , 1998, astro-ph/9812214.

[12]  C. Baugh,et al.  The Durham/UKST Galaxy Redshift Survey — VI. Power spectrum analysis of clustering , 1998, astro-ph/9812137.

[13]  M. White,et al.  The growth of correlations in the matter power spectrum , 1998, astro-ph/9812129.

[14]  S. Croom,et al.  Radio-quiet QSO environments — I. The correlation of QSOs and bJ < 23 galaxies , 1998, astro-ph/9810170.

[15]  C. Lawrence,et al.  Evolution of Large-Scale Structure , 1998 .

[16]  D. Schlegel,et al.  Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds , 1998 .

[17]  D. Weinberg,et al.  Mock 2dF and SDSS galaxy redshift surveys , 1998, astro-ph/9801250.

[18]  S. Cristiani,et al.  Quasar Clustering: Evidence for an Increase with Redshift and Implications for the Nature of Active Galactic Nuclei , 1997, astro-ph/9711048.

[19]  D. Schlegel,et al.  Maps of Dust IR Emission for Use in Estimation of Reddening and CMBR Foregrounds , 1997, astro-ph/9710327.

[20]  G. Efstathiou,et al.  The power spectrum of rich clusters of galaxies on large spatial scales , 1997, astro-ph/9708259.

[21]  A. Heavens,et al.  Eulerian bias and the galaxy density field , 1997, astro-ph/9708031.

[22]  R. Croft,et al.  Recovery of the Power Spectrum of Mass Fluctuations from Observations of the Lyα Forest , 1997, astro-ph/9708018.

[23]  S. Croom,et al.  QSO clustering - III. Clustering in the Large Bright Quasar Survey and evolution of the QSO correlation function , 1996 .

[24]  S. Shectman,et al.  The Power Spectrum of Galaxy Clustering in the Las Campanas Redshift Survey , 1996, astro-ph/9606055.

[25]  U. Seljak,et al.  A Line of sight integration approach to cosmic microwave background anisotropies , 1996, astro-ph/9603033.

[26]  G. Efstathiou,et al.  Power spectrum analysis of the Stromlo—APM redshift survey , 1996, astro-ph/9603016.

[27]  S. Cole,et al.  Using the evolution of clusters to constrain Omega , 1996, astro-ph/9601088.

[28]  C. Steidel,et al.  Lyman Limit Imaging of High Redshift Galaxies. III. New Observations of 4 QSO Fields , 1995, astro-ph/9509089.

[29]  O. Fèvre,et al.  The Canada-France Redshift Survey. V. Global Properties of the Sample , 1995, astro-ph/9507014.

[30]  S. Maddox,et al.  The environments of $z\leqslant0.3$ QSOs , 1995, astro-ph/9506093.

[31]  A. Evrard,et al.  Galaxy Tracers and Velocity Bias , 1995, astro-ph/9505080.

[32]  Frederic H. Chaffee,et al.  The Large Bright Quasar Survey.VI.Quasar Catalog and Survey Parameters , 1995 .

[33]  T. Shanks,et al.  QSO clustering – I. Optical surveys in the redshift range 0.3 < z < 2.2 , 1994 .

[34]  N. Sugiyama.  Cosmic background anistropies in CDM cosmology , 1994, astro-ph/9412025.

[35]  C. Baugh,et al.  A comparison of the evolution of density fields in perturbation theory and numerical simulations – I. Non-linear evolution of the power spectrum , 1994 .

[36]  Carlton M. Baugh,et al.  The three-dimensional power spectrum measured from the APM Galaxy Survey – I. Use of the angular correlation function , 1993 .

[37]  D. Weinberg,et al.  Fourier analysis of redshift-space distortions and the determination of Ω , 1993, astro-ph/9308003.

[38]  P. Coles.  Galaxy formation with a local bias , 1993 .

[39]  J. Peacock,et al.  Power spectrum analysis of three-dimensional redshift surveys , 1993, astro-ph/9304022.

[40]  R. Green,et al.  Quasars and active galactic nuclei in rich environments. II - The evolution of radio-loud quasars , 1991 .

[41]  S. Maddox,et al.  The cosmological constant and cold dark matter , 1990, Nature.

[42]  N. Kaiser.  Clustering in real space and in redshift space , 1987 .

[43]  A. Szalay,et al.  The statistics of peaks of Gaussian random fields , 1986 .

[44]  P. Osmer.  The three-dimensional distribution of quasars in the CTIO surveys , 1981 .

[45]  D. Eisenstein,et al.  Correlations in the Spatial Power Spectra Inferred from Angular Clustering: Methods and Application to the Automated Plate Measuring Survey , 2001 .

[46]  Warrick J. Couch,et al.  Looking Deep in the Southern Sky , 1999 .

[47]  A. Banday,et al.  Evolution of large scale structure : from recombination to Garching : proceedings of the MPA-ESO Cosmology Conference : Garching, Germany, 2-7 August 1998 , 1999 .

[48]  Cambridge,et al.  ∼ 4 and the Evolution of the Uv Luminosity Density at High Redshift , 2022 .