Publication details for Prof Richard MasseyJullo, E., Rhodes, J., Kiessling, A., Taylor, J.E., Massey, R., Berge, J., Schimd, C., Kneib, J.-P. & Scoville, N. (2012). COSMOS stochastic bias from measurements of weak lensing and galaxy clustering. Astrophysical journal 750(1): 37.
- Publication type: Journal Article
- ISSN/ISBN: 0004-637X, 1538-4357
- DOI: 10.1088/0004-637X/750/1/37
- Keywords: Cosmology: observations, Gravitational lensing: weak, Large-scale structure of universe.
- Further publication details on publisher web site
- Durham Research Online (DRO) - may include full text
Author(s) from Durham
In the theory of structure formation, galaxies are biased tracers of the underlying matter density field. The statistical relation between galaxy and matter density field is commonly referred to as galaxy bias. In this paper, we test the linear bias model with weak-lensing and galaxy clustering measurements in the 2 deg2 COSMOS field. We estimate the bias of galaxies between redshifts z = 0.2 and z = 1 and over correlation scales between R = 0.2 h –1 Mpc and R = 15 h –1 Mpc. We focus on three galaxy samples, selected in flux (simultaneous cuts I 814W < 26.5 and Ks < 24) and in stellar mass (109 < M * < 1010 h –2 M ☉ and 1010 < M * < 1011 h –2 M ☉). At scales R > 2 h –1 Mpc, our measurements support a model of bias increasing with redshift. The Tinker et al. fitting function provides a good fit to the data. We find the best-fit mass of the galaxy halos to be log (M 200/h –1 M ☉) = 11.7+0.6 – 1.3 and log (M 200/h –1 M ☉) = 12.4+0.2 – 2.9, respectively, for the low and high stellar-mass samples. In the halo model framework, bias is scale dependent with a change of slope at the transition scale between the one and the two halo terms. We detect a scale dependence of bias with a turndown at scale R = 2.3 ± 1.5 h –1 Mpc, in agreement with previous galaxy clustering studies. We find no significant amount of stochasticity, suggesting that a linear bias model is sufficient to describe our data. We use N-body simulations to quantify both the amount of cosmic variance and systematic errors in the measurement.