Galaxy bias can be split into two components: a formation-bias based on the locations of galaxy creation, and an evolution-bias that details their subsequent evolution. In this letter we consider evolution-bias in the peaks model. In this model, galaxy formation takes place at local maxima in the density field, and we analyse the subsequent peculiar motion of these galaxies in a linear model of...

Abstract We construct accurate emulators for the projected and redshift space galaxy correlation functions excess surface density as measured by galaxy–galaxy lensing, based on halo occupation distribution modeling. Using complete Mira-Titan suite of 111 N -body simulations, our vary over eight cosmological parameters include effects neutrino mass dynamical dark energy. demonstrate that are suf...

The redshift-space correlation function ξs for projected galaxy separations <∼ 1h Mpc can be expressed as the convolution of the real-space correlation function with the galaxy pairwise velocity distribution function (PVDF). An exponential PVDF yields the best fit to the ξs measured from galaxy samples of different redshift surveys. We show that this exponential PVDF is not merely a fitting fun...

Modern cosmological analyses of galaxy-galaxy lensing face a theoretical systematic effect arising from the non-locality observed signal. Because predicted tangential shear signal at given separation depends on physical modeling all scales internal to that separation, uncertainties in non-linear small are propagated outwards larger scales. Even absence other limiting factors, this alone can nec...

We present the Shapley Optical Survey, a photometric study covering a ∼ 2 deg2 region of the Shapley Supercluster core at z∼0.05 in two bands (B and R). The galaxy sample is complete to B = 22.5 (>M+6, Ngal = 16 588), and R = 22.0 (>M+7, Ngal = 28 008). The galaxy luminosity function cannot be described by a single Schechter function due to dips apparent at B ∼ 17.5 (MB ∼ 19.3) and R ∼ 17.0 (MR...

We investigate galaxy bias in the framework of the “Halo Occupation Distribution” (HOD), which defines the bias of a population of galaxies by the conditional probability P (N |M) that a dark matter halo of virial mass M contains N galaxies, together with prescriptions that specify the relative spatial and velocity distributions of galaxies and dark matter within halos. By populating the halos ...