2018/07/30 by Andrew Benson, Andrew J. Benson · 1 citation
Mathematics · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics #Correlation function (quantum field theory) #Covariance #Covariance function #Covariance matrix #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Halo #Interacting galaxy #Lenticular galaxy #Mathematics #Physics #Scientific Research and Discoveries #Statistics #astro-ph.GA
paper · pdf · doi:10.1093/mnras/sty2676
published in Monthly Notices of the Royal Astronomical Society 482(1), 1062-1079 (Oxford University Press) · Submitted to MNRAS. Associated data files will be made available when (and if) the paper is accepted for publication
arxiv created 2018/07/30 · openalex publication_date 2018/10/04 · arxiv updated 2018/10/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We compute covariance matrices for many observed estimates of the stellar mass function of galaxies from |z| = 0 to |z| ≈ 4, and for one estimate of the projected correlation function of galaxies split by stellar mass at |z| ≲ 0.5, using a combination of analytic methods and N-body simulations coupled to a halo occupation distribution approach. All covariance matrices include contributions due to large-scale structure, the preference for galaxies to be found in groups and clusters, and for shot noise. These covariance matrices are made available for use in constraining models of galaxy formation and the galaxy–halo connection.