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2005MNRAS.356..415C - Mon. Not. R. Astron. Soc., 356, 415-438 (2005/January-2)
The 2dF QSO Redshift Survey - XIV. Structure and evolution from the two-point correlation function.
CROOM S.M., BOYLE B.J., SHANKS T., SMITH R.J., MILLER L., OUTRAM P.J., LOARING N.S., HOYLE F. and DA ANGELA J.
Abstract (from CDS):
We subdivide the 2QZ into 10 redshift intervals with effective redshifts from z= 0.53 to 2.48. We find a significant increase in clustering amplitude at high redshift in the WMAP/2dF cosmology. The QSO clustering amplitude increases with redshift such that the integrated correlation function,, within 20h–1 Mpc is and. We derive the QSO bias and find it to be a strong function of redshift with bQ(z= 0.53) = 1.13±0.18 and bQ(z= 2.48) = 4.24±0.53. We use these bias values to derive the mean dark matter halo (DMH) mass occupied by the QSOs. At all redshifts 2QZ QSOs inhabit approximately the same mass DMHs with MDH= (3.0±1.6)x1012h–1 M☉, which is close to the characteristic mass in the Press-Schechter mass function, M*, at z= 0. These results imply that L*QQSOs at z∼ 0 should be largely unbiased. If the relation between black hole (BH) mass and MDHor host velocity dispersion does not evolve, then we find that the accretion efficiency (L/LEdd) for L*QQSOs is approximately constant with redshift. Thus the fading of the QSO population from z∼ 2 to ∼0 appears to be due to less massive BHs being active at low redshift. We apply different methods to estimate, tQ, the active lifetime of QSOs and constrain tQto be in the range 4x106-6 x108 yr at z∼ 2.
We test for any luminosity dependence of QSO clustering by measuring ξ(s) as a function of apparent magnitude (equivalent to luminosity relative to L*Q). However, we find no significant evidence of luminosity-dependent clustering from this data set.
Abstract Copyright: 2004 RAS
Journal keyword(s): galaxies: clusters: general - quasars: general - cosmology: observations - large-scale structure of Universe
Simbad objects: 2
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