EDP Sciences
Free access
Volume 498, Number 2, May I 2009
Page(s) 347 - 355
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361/200811360
Published online 18 February 2009
A&A 498, 347-355 (2009)
DOI: 10.1051/0004-6361/200811360

Using the large scale quasar clustering to constrain flat quintessential universes

A. Zandivarez and H. J. Martínez

Instituto de Astronomía Teórica y Experimental (IATE), CONICET-Observatorio Astronómico, Universidad Nacional de Córdoba. Laprida 854, Córdoba X5000BGR, Argentina
    e-mail: [arielz;julian]@mail.oac.uncor.edu

Received 17 November 2008 / Accepted 21 January 2009

Aims. We search for the most suitable set of cosmological parameters that describes the observable universe. The search includes the possibility of quintessential flat universes, i.e., the analysis is restricted to the determination of the dimensionless matter density and the quintessential parameters, $\Omega_{\rm M}$ and $w_{\rm Q}$, respectively.
Methods. Our study is focused on comparing the position of features at large scales in the density fluctuation field at different redshifts by analysing the evolution of the quasar two-point correlation function. We trace the density field fluctuations at large scales using a large and homogeneous sample of quasars (~38 000 objects with 0.3 $\lesssim$ z $\le$ 2.4 and a median z = 1.45) drawn from the Sloan Digital Sky Survey Data Release Six. The analysis relies on the assumption that, in the linear regime, the length scale of a particular feature should remain fixed at different times of the universe for the proper cosmological model. Our study does not assume any particular comoving length scale at which a feature should be found, but intends to perform a comparison for a wide range of scales instead. This is done by quantifying the amount of overlap among the quasar correlation functions at different times using a cross-correlation technique.
Results. The most likely cosmological model is $\Omega_{\rm M}$ = 0.21$\pm$0.02 and $w_{\rm Q}$ = -0.93$\pm$0.04, in agreement with previous studies. These constraints are the result of a good overall agreement of the correlation function at different redshifts over scales ~100–300 h-1 Mpc.
Conclusions. Under the assumption of a flat cosmological model, our results indicate that we are living in a low density universe with a quintessential parameter greater than the one corresponding to a cosmological constant. This work also demonstrates that a large homogeneous quasar sample can be used to tighten the constraints upon cosmological parameters.

Key words: cosmological parameters -- cosmology: observations -- large-scale structure of Universe -- quasars: general

© ESO 2009