Galaxy Correlation Function and Local Density from Photometric Redshifts Using the Stochastic Order Redshift Technique (SORT)

Abstract

The stochastic order redshift technique () is a simple, efficient, and robust method to improve cosmological redshift measurements. The method relies upon having a small (∼10 per cent) reference sample of high-quality redshifts. Within pencilbeam-like sub-volumes surrounding each galaxy, we use the precise d𝑁/d𝑧 distribution of the reference sample to recover new redshifts and assign them one-to-one to galaxies such that the original rank order of redshifts is preserved. Preserving the rank order is motivated by the fact that random variables drawn from Gaussian probability density functions with different means but equal standard deviations satisfy stochastic ordering. The process is repeated for sub-volumes surrounding each galaxy in the survey. This results in every galaxy with an uncertain redshift being assigned multiple 'recovered' redshifts from which a new redshift estimate can be determined. An earlier paper applied to a mock Sloan Digital Sky Survey at 𝑧 0.2 and accurately recovered the two-point correlation function on scales 4 ℎ −1 Mpc. In this paper, we test the performance of in surveys spanning the redshift range 0.75 < 𝑧 < 2.25. We used two mock surveys extracted from the Small MultiDark-Planck and Bolshoi-Planck 𝑁-body simulations with dark matter haloes that were populated by the Santa Cruz semi-analytic model. We find that is able to improve redshift estimates and recover distinctive large-scale features of the cosmic web. Further, it provides unbiased estimates of the redshift-space two-point correlation function 𝜉 (𝑠) on scales 2.5 ℎ −1 Mpc, as well as local densities in regions of average or higher density. This may allow improved understanding of how galaxy properties relate to their local environments.