The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k Catalogue
(ABRIDGED) We present a power spectrum analysis of the 10K catalogue from the 2dF QSO Redshift Survey. 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,...
| Main Authors: | , , , , , , |
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| Format: | Journal article |
| Published: |
2001
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| _version_ | 1797103825846272000 |
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| author | Hoyle, F Outram, P Shanks, T Croom, S Loaring, B Miller, L Smith, R |
| author_facet | Hoyle, F Outram, P Shanks, T Croom, S Loaring, B Miller, L Smith, R |
| author_sort | Hoyle, F |
| collection | OXFORD |
| description | (ABRIDGED) We present a power spectrum analysis of the 10K catalogue from the 2dF QSO Redshift Survey. 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 P_QSO(k)\propto 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 Omega_m=0.3 and Omega_Lambda=0.7 (the Lambda cosmology), and a factor of ~3 lower if Omega_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 and Efstathiou. We split the QSO sample into two redshift bins and find little evolution in the amplitude of the power spectrum. The QSO power spectrum may show a spike feature at ~90h^{-1}Mpc assuming the Lambda cosmology or ~65 h^{-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, Gamma. For two choices of cosmology (Omega_m=1, Omega_Lambda=0 and Omega_m=0.3, Omega_Lambda=0.7), we find the best fit model has Gamma~0.1 +-0.1. |
| first_indexed | 2024-03-07T06:25:29Z |
| format | Journal article |
| id | oxford-uuid:f424a63c-c1bb-42e2-baee-3d50644133f7 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T06:25:29Z |
| publishDate | 2001 |
| record_format | dspace |
| spelling | oxford-uuid:f424a63c-c1bb-42e2-baee-3d50644133f72022-03-27T12:17:28ZThe 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k CatalogueJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:f424a63c-c1bb-42e2-baee-3d50644133f7Symplectic Elements at Oxford2001Hoyle, FOutram, PShanks, TCroom, SLoaring, BMiller, LSmith, R(ABRIDGED) We present a power spectrum analysis of the 10K catalogue from the 2dF QSO Redshift Survey. 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 P_QSO(k)\propto 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 Omega_m=0.3 and Omega_Lambda=0.7 (the Lambda cosmology), and a factor of ~3 lower if Omega_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 and Efstathiou. We split the QSO sample into two redshift bins and find little evolution in the amplitude of the power spectrum. The QSO power spectrum may show a spike feature at ~90h^{-1}Mpc assuming the Lambda cosmology or ~65 h^{-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, Gamma. For two choices of cosmology (Omega_m=1, Omega_Lambda=0 and Omega_m=0.3, Omega_Lambda=0.7), we find the best fit model has Gamma~0.1 +-0.1. |
| spellingShingle | Hoyle, F Outram, P Shanks, T Croom, S Loaring, B Miller, L Smith, R The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k Catalogue |
| title | The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k
Catalogue |
| title_full | The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k
Catalogue |
| title_fullStr | The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k
Catalogue |
| title_full_unstemmed | The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k
Catalogue |
| title_short | The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k
Catalogue |
| title_sort | 2df qso redshift survey iv the qso power spectrum from the 10k catalogue |
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