Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey

Nicholas P. Ross, Yue Shen, Michael A. Strauss, Daniel E. Vanden Berk, Andrew J. Connolly, Gordon T. Richards, Donald P. Schneider, David H. Weinberg, Patrick B. Hall, Neta A. Bahcall, Robert J. Brunner

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Abstract

We present measurements of the quasar two-point correlation function, ξQ, over the redshift range 0.3 ≤ z ≤ 2.2 based upon data from the Sloan Digital Sky Survey (SDSS). Using a homogeneous sample of 30,239 quasars with spectroscopic redshifts from the Data Release 5 Quasar Catalog, our study represents the largest sample used for this type of investigation to date. With this redshift range and an areal coverage of 4000 deg2, we sample over 25 h -3 Gpc3 (comoving) of the universe in volume, assuming the current Lambda Cold Dark Matter (ΛCDM) cosmology. Over this redshift range, we find that the redshift-space correlation function, ξ(s), is adequately fit by a single power law, with s 0 = 5.95 0.45 h -1 Mpc and γs = 1.16+0.11 -0.16 when fit over 1.0 h -1 Mpc ≤ s ≤ 25.0 h -1 Mpc. We find no evidence for deviation from ξ(s) = 0 at scales of s>100 h -1 Mpc, but do observe redshift-space distortions in the two-dimensional ξ(rp , π) measurement. Using the projected correlation function, wp (rp ), we calculate the real-space correlation length, r 0 = 5.45+0.35 -0.45 h -1 Mpc and γ = 1.90+0.04 -0.03, over scales of 1.0 h -1 Mpc ≤ rp ≤ 130.0 h -1 Mpc. Dividing the sample into redshift slices, we find very little, if any, evidence for the evolution of quasar clustering, with the redshift-space correlation length staying roughly constant at s 0 6-7 h -1 Mpc at z ≲ 2.2 (and only increasing at redshifts greater than this). We do, however, see tentative evidence for evolution in the real-space correlation length, r 0, at z>1.7. Our results are consistent with those from the 2dF QSO Redshift Survey and previous SDSS quasar measurements using photometric redshifts. Comparing our clustering measurements to those reported for X-ray selected active galactic nucleus at z 0.5-1, we find reasonable agreement in some cases but significantly lower correlation lengths in others. Assuming a standard ΛCDM cosmology, we find that the linear bias evolves from b 1.4 at z = 0.5 to b 3 at z = 2.2, with b(z = 1.27) = 2.06 0.03 for the full sample. We compare our data to analytical models and infer that quasars inhabit dark matter halos of constant mass M halo 2 × 1012 h -1 M from redshifts z 2.5 (the peak of quasar activity) to z 0; therefore, the ratio of the halo mass for a typical quasar to the mean halo mass at the same epoch drops with decreasing redshift. The measured evolution of the clustering amplitude is in reasonable agreement with recent theoretical models, although measurements to fainter limits will be needed to distinguish different scenarios for quasar feeding and black hole growth.

Original languageEnglish (US)
Pages (from-to)1634-1655
Number of pages22
JournalAstrophysical Journal
Volume697
Issue number2
DOIs
StatePublished - Jan 1 2009

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quasars
halos
cosmology
dark matter
dimensional measurement
power law
active galactic nuclei
catalogs
universe
time measurement
deviation

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ross, N. P., Shen, Y., Strauss, M. A., Vanden Berk, D. E., Connolly, A. J., Richards, G. T., ... Brunner, R. J. (2009). Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey. Astrophysical Journal, 697(2), 1634-1655. https://doi.org/10.1088/0004-637X/697/2/1634
Ross, Nicholas P. ; Shen, Yue ; Strauss, Michael A. ; Vanden Berk, Daniel E. ; Connolly, Andrew J. ; Richards, Gordon T. ; Schneider, Donald P. ; Weinberg, David H. ; Hall, Patrick B. ; Bahcall, Neta A. ; Brunner, Robert J. / Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey. In: Astrophysical Journal. 2009 ; Vol. 697, No. 2. pp. 1634-1655.
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abstract = "We present measurements of the quasar two-point correlation function, ξQ, over the redshift range 0.3 ≤ z ≤ 2.2 based upon data from the Sloan Digital Sky Survey (SDSS). Using a homogeneous sample of 30,239 quasars with spectroscopic redshifts from the Data Release 5 Quasar Catalog, our study represents the largest sample used for this type of investigation to date. With this redshift range and an areal coverage of 4000 deg2, we sample over 25 h -3 Gpc3 (comoving) of the universe in volume, assuming the current Lambda Cold Dark Matter (ΛCDM) cosmology. Over this redshift range, we find that the redshift-space correlation function, ξ(s), is adequately fit by a single power law, with s 0 = 5.95 0.45 h -1 Mpc and γs = 1.16+0.11 -0.16 when fit over 1.0 h -1 Mpc ≤ s ≤ 25.0 h -1 Mpc. We find no evidence for deviation from ξ(s) = 0 at scales of s>100 h -1 Mpc, but do observe redshift-space distortions in the two-dimensional ξ(rp , π) measurement. Using the projected correlation function, wp (rp ), we calculate the real-space correlation length, r 0 = 5.45+0.35 -0.45 h -1 Mpc and γ = 1.90+0.04 -0.03, over scales of 1.0 h -1 Mpc ≤ rp ≤ 130.0 h -1 Mpc. Dividing the sample into redshift slices, we find very little, if any, evidence for the evolution of quasar clustering, with the redshift-space correlation length staying roughly constant at s 0 6-7 h -1 Mpc at z ≲ 2.2 (and only increasing at redshifts greater than this). We do, however, see tentative evidence for evolution in the real-space correlation length, r 0, at z>1.7. Our results are consistent with those from the 2dF QSO Redshift Survey and previous SDSS quasar measurements using photometric redshifts. Comparing our clustering measurements to those reported for X-ray selected active galactic nucleus at z 0.5-1, we find reasonable agreement in some cases but significantly lower correlation lengths in others. Assuming a standard ΛCDM cosmology, we find that the linear bias evolves from b 1.4 at z = 0.5 to b 3 at z = 2.2, with b(z = 1.27) = 2.06 0.03 for the full sample. We compare our data to analytical models and infer that quasars inhabit dark matter halos of constant mass M halo 2 × 1012 h -1 M ⊙ from redshifts z 2.5 (the peak of quasar activity) to z 0; therefore, the ratio of the halo mass for a typical quasar to the mean halo mass at the same epoch drops with decreasing redshift. The measured evolution of the clustering amplitude is in reasonable agreement with recent theoretical models, although measurements to fainter limits will be needed to distinguish different scenarios for quasar feeding and black hole growth.",
author = "Ross, {Nicholas P.} and Yue Shen and Strauss, {Michael A.} and {Vanden Berk}, {Daniel E.} and Connolly, {Andrew J.} and Richards, {Gordon T.} and Schneider, {Donald P.} and Weinberg, {David H.} and Hall, {Patrick B.} and Bahcall, {Neta A.} and Brunner, {Robert J.}",
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Ross, NP, Shen, Y, Strauss, MA, Vanden Berk, DE, Connolly, AJ, Richards, GT, Schneider, DP, Weinberg, DH, Hall, PB, Bahcall, NA & Brunner, RJ 2009, 'Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey', Astrophysical Journal, vol. 697, no. 2, pp. 1634-1655. https://doi.org/10.1088/0004-637X/697/2/1634

Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey. / Ross, Nicholas P.; Shen, Yue; Strauss, Michael A.; Vanden Berk, Daniel E.; Connolly, Andrew J.; Richards, Gordon T.; Schneider, Donald P.; Weinberg, David H.; Hall, Patrick B.; Bahcall, Neta A.; Brunner, Robert J.

In: Astrophysical Journal, Vol. 697, No. 2, 01.01.2009, p. 1634-1655.

Research output: Contribution to journalReview article

TY - JOUR

T1 - Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey

AU - Ross, Nicholas P.

AU - Shen, Yue

AU - Strauss, Michael A.

AU - Vanden Berk, Daniel E.

AU - Connolly, Andrew J.

AU - Richards, Gordon T.

AU - Schneider, Donald P.

AU - Weinberg, David H.

AU - Hall, Patrick B.

AU - Bahcall, Neta A.

AU - Brunner, Robert J.

PY - 2009/1/1

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N2 - We present measurements of the quasar two-point correlation function, ξQ, over the redshift range 0.3 ≤ z ≤ 2.2 based upon data from the Sloan Digital Sky Survey (SDSS). Using a homogeneous sample of 30,239 quasars with spectroscopic redshifts from the Data Release 5 Quasar Catalog, our study represents the largest sample used for this type of investigation to date. With this redshift range and an areal coverage of 4000 deg2, we sample over 25 h -3 Gpc3 (comoving) of the universe in volume, assuming the current Lambda Cold Dark Matter (ΛCDM) cosmology. Over this redshift range, we find that the redshift-space correlation function, ξ(s), is adequately fit by a single power law, with s 0 = 5.95 0.45 h -1 Mpc and γs = 1.16+0.11 -0.16 when fit over 1.0 h -1 Mpc ≤ s ≤ 25.0 h -1 Mpc. We find no evidence for deviation from ξ(s) = 0 at scales of s>100 h -1 Mpc, but do observe redshift-space distortions in the two-dimensional ξ(rp , π) measurement. Using the projected correlation function, wp (rp ), we calculate the real-space correlation length, r 0 = 5.45+0.35 -0.45 h -1 Mpc and γ = 1.90+0.04 -0.03, over scales of 1.0 h -1 Mpc ≤ rp ≤ 130.0 h -1 Mpc. Dividing the sample into redshift slices, we find very little, if any, evidence for the evolution of quasar clustering, with the redshift-space correlation length staying roughly constant at s 0 6-7 h -1 Mpc at z ≲ 2.2 (and only increasing at redshifts greater than this). We do, however, see tentative evidence for evolution in the real-space correlation length, r 0, at z>1.7. Our results are consistent with those from the 2dF QSO Redshift Survey and previous SDSS quasar measurements using photometric redshifts. Comparing our clustering measurements to those reported for X-ray selected active galactic nucleus at z 0.5-1, we find reasonable agreement in some cases but significantly lower correlation lengths in others. Assuming a standard ΛCDM cosmology, we find that the linear bias evolves from b 1.4 at z = 0.5 to b 3 at z = 2.2, with b(z = 1.27) = 2.06 0.03 for the full sample. We compare our data to analytical models and infer that quasars inhabit dark matter halos of constant mass M halo 2 × 1012 h -1 M ⊙ from redshifts z 2.5 (the peak of quasar activity) to z 0; therefore, the ratio of the halo mass for a typical quasar to the mean halo mass at the same epoch drops with decreasing redshift. The measured evolution of the clustering amplitude is in reasonable agreement with recent theoretical models, although measurements to fainter limits will be needed to distinguish different scenarios for quasar feeding and black hole growth.

AB - We present measurements of the quasar two-point correlation function, ξQ, over the redshift range 0.3 ≤ z ≤ 2.2 based upon data from the Sloan Digital Sky Survey (SDSS). Using a homogeneous sample of 30,239 quasars with spectroscopic redshifts from the Data Release 5 Quasar Catalog, our study represents the largest sample used for this type of investigation to date. With this redshift range and an areal coverage of 4000 deg2, we sample over 25 h -3 Gpc3 (comoving) of the universe in volume, assuming the current Lambda Cold Dark Matter (ΛCDM) cosmology. Over this redshift range, we find that the redshift-space correlation function, ξ(s), is adequately fit by a single power law, with s 0 = 5.95 0.45 h -1 Mpc and γs = 1.16+0.11 -0.16 when fit over 1.0 h -1 Mpc ≤ s ≤ 25.0 h -1 Mpc. We find no evidence for deviation from ξ(s) = 0 at scales of s>100 h -1 Mpc, but do observe redshift-space distortions in the two-dimensional ξ(rp , π) measurement. Using the projected correlation function, wp (rp ), we calculate the real-space correlation length, r 0 = 5.45+0.35 -0.45 h -1 Mpc and γ = 1.90+0.04 -0.03, over scales of 1.0 h -1 Mpc ≤ rp ≤ 130.0 h -1 Mpc. Dividing the sample into redshift slices, we find very little, if any, evidence for the evolution of quasar clustering, with the redshift-space correlation length staying roughly constant at s 0 6-7 h -1 Mpc at z ≲ 2.2 (and only increasing at redshifts greater than this). We do, however, see tentative evidence for evolution in the real-space correlation length, r 0, at z>1.7. Our results are consistent with those from the 2dF QSO Redshift Survey and previous SDSS quasar measurements using photometric redshifts. Comparing our clustering measurements to those reported for X-ray selected active galactic nucleus at z 0.5-1, we find reasonable agreement in some cases but significantly lower correlation lengths in others. Assuming a standard ΛCDM cosmology, we find that the linear bias evolves from b 1.4 at z = 0.5 to b 3 at z = 2.2, with b(z = 1.27) = 2.06 0.03 for the full sample. We compare our data to analytical models and infer that quasars inhabit dark matter halos of constant mass M halo 2 × 1012 h -1 M ⊙ from redshifts z 2.5 (the peak of quasar activity) to z 0; therefore, the ratio of the halo mass for a typical quasar to the mean halo mass at the same epoch drops with decreasing redshift. The measured evolution of the clustering amplitude is in reasonable agreement with recent theoretical models, although measurements to fainter limits will be needed to distinguish different scenarios for quasar feeding and black hole growth.

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Ross NP, Shen Y, Strauss MA, Vanden Berk DE, Connolly AJ, Richards GT et al. Clustering of low-redshift (z ≤ 2.2) quasars from the sloan digital sky survey. Astrophysical Journal. 2009 Jan 1;697(2):1634-1655. https://doi.org/10.1088/0004-637X/697/2/1634