TITLE:
SDSS galaxy bias from halo mass-bias relation and its cosmological implications
AUTHOR(S):
Uros Seljak, Alexey Makarov, Rachel Mandelbaum, Christopher M. Hirata, Nikhil Padmanabhan, and Patrick McDonald (Princeton); Michael R.
Blanton (NYU); Max Tegmark (U. Pennsylvania and MIT); Neta A. Bahcall (Princeton); and Jonathan Brinkmann (Apache Point Obs.)
DATE:
2004 Jun 25 (Phys. Rev. D, submitted);
2004 Jun 25 (arXiv, v1, posted);
2005 Jan 05 (production proof);
2005 Feb 09 (arXiv, v2, posted);
2005 Feb 16 (Phys. Rev. D, published).
AVAILABILITY: arXiv
astro-ph/0406594 (free); APS (requires subscription).
PUBLICATION INFORMATION: Phys. Rev. D, 71, 043511 (2005), 18 pages.
ABSTRACT:
We combine the measurements of luminosity dependence of bias with the luminosity dependent weak lensing analysis of dark matter around
galaxies to derive the galaxy bias and constrain nonlinear mass and cosmological parameters. We take advantage of theoretical and
simulation predictions that predict that while halo bias is rapidly increasing with mass for high masses, it is nearly constant in low
mass halos. We use a new weak lensing analysis around the same SDSS galaxies to determine their halo mass probability distribution.
These halo mass probability distributions are used to predict the bias for each luminosity subsample and we find an excellent agreement
with observed values. The required nonlinear mass suggests slightly lower matter density than usually assumed, Wm=0.25+/- 0.03 for
the simplest models. We combine the bias constraints with those from the WMAP and the SDSS power spectrum analysis to derive new
constraints on bias and s8. For the most general parameter space we find s8=0.88+/- 0.06 and
b*=0.99+/- 0.07. In the context
of spatially flat models we improve the limit on the neutrino mass for the case of 3 degenerate families from mn<0.6eV without bias to
mn<0.18eV with bias (95% c.l.), which is weakened to mn<0.24eV if running is allowed. The
corresponding limit for 3 massless + 1 massive neutrino is 1.37eV.
ADS BIBLIOGRAPHIC CODE: 2005PhRvD..71d3511S
COMMENTS:
SDSS Publication #345. This paper makes use of SDSS weak lensing data, the analysis of which is described (in part) in Publication #352 and Publication #472.