A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4

By P. Behroozi, C. Conroy, Risa Wechsler. 2010

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We conduct a comprehensive analysis of the relationship between central galaxies and their host dark matter halos, as characterized by the stellar mass–halo mass (SM–HM) relation, with rigorous consideration of uncertainties. Our analysis focuses on results from the abundance matching technique, which assumes that every dark matter halo or subhalo above a specific mass threshold hosts one galaxy. We provide a robust estimate of the SM–HM relation for 0 < z < 1 and discuss the quantitative effects of uncertainties in observed galaxy stellar mass functions (including stellar mass estimates and counting uncertainties), halo mass functions (including cosmology and uncertainties from substructure), and the abundance matching technique used to link galaxies to halos (including scatter in this connection). Our analysis results in a robust estimate of the SM–HM relation and its evolution from z = 0 to z = 4. The shape and the evolution are well constrained for z < 1. The largest uncertainties at these redshifts are due to stellar mass estimates (0.25 dex uncertainty in normalization); however, failure to account for scatter in stellar masses at fixed halo mass can lead to errors of similar magnitude in the SM–HM relation for central galaxies in massive halos. We also investigate the SM–HM relation to z = 4, although the shape of the relation at higher redshifts remains fairly unconstrained when uncertainties are taken into account. We find that the integrated star formation at a given halo mass peaks at 10%–20% of available baryons for all redshifts from 0 to 4. This peak occurs at a halo mass of 7 × 1011 M☉ at z = 0 and this mass increases by a factor of 5 to z = 4. At lower and higher masses, star formation is substantially less efficient, with stellar mass scaling as M* ∼ M2.3h at low masses and M* ∼ M0.29h at high masses. The typical stellar mass for halos with mass less than 1012 M☉ has increased by 0.3–0.45 dex for halos since z ∼ 1. These results will provide a powerful tool to inform galaxy evolution models.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/3aaa6ae2536ac2557a5aa835c385eb232ff25347

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Citations in the corpus

Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, background): “At all redshift, this cut is just below the mass corresponding to the maximal efficiency of star formation inside halos (defined here as the ratio between stellar mass and halo mass, Moster et al. 2010, 2013; Behroozi et al. 2010; Béthermin et al. 2012b; Wang et al. 2013).”
THE COUPLING BETWEEN THE CORE/CUSP AND MISSING SATELLITE PROBLEMS (2012, background): “(8) is also consistent with the abundance of luminous structures found in external galaxies (e.g. Behroozi et al. 2010).”
EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, result): “The conversion efficiency of our model at the low-mass end is lower than the results that have been obtained with subhalo abundance matching (Moster et al. 2010; Behroozi et al. 2010; Guo et al. 2010; Moster et al. 2013; Behroozi et al. 2010).”
TOWARD A COMPLETE ACCOUNTING OF ENERGY AND MOMENTUM FROM STELLAR FEEDBACK IN GALAXY FORMATION SIMULATIONS (2012, background): “…& Wechsler 2009; Guo et al. 2010), satellite kinematics (Klypin & Prada 2009; More et al. 2010), and weak lensing (Mandelbaum et al. 2006), see Behroozi et al. (2010) for 1 Kavli Institute for Cosmological Physics and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637 USA 2…”
The formation of disc galaxies in a ΛCDM universe (2010, background): “Behroozi et al. (2010) performed a comprehensive analysis of abundance matching, accounting for systematic errors in e.g. the stellar mass estimates, the halo mass function, cosmology etc.”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, background): “There may also be non-zero galaxy-to-galaxy variations in f⋆ at a fixed mass and type; the value of this scatter is less well established, but recent analyses suggest that it may be ∼ 0.15 dex (Behroozi et al. 2010; More et al. 2011).”
Hunting for the Dark Matter Wake Induced by the Large Magellanic Cloud (2019, methodology): “Using abundance matching, a statistical technique used to assign a DM halo mass to a galaxy of a given stellar mass, the total mass of the LMC, prior to accretion by the MW, should be ∼ 1.6× 1011 M (Moster et al. 2010; Behroozi et al. 2010; Guo et al. 2010).”
Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, background): “…in reproducing the observed luminosity dependence of galaxy clustering (Kravtsov et al. 2004; Tasitsiomi et al. 2004; Conroy et al. 2006; Reddick et al. 2013) and other statistics (Vale & Ostriker 2004, 2006; Behroozi et al. 2010, 2013a; Guo et al. 2010; Moster et al. 2013; Hearin et al. 2013).”
A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, methodology): “One such conversion between M⋆ and Mhalo is given by Behroozi et al. (2010) and Leauthaud et al. (2012), derived from a combination of methods for measuring Mhalo and M⋆ over a wide range of luminosity regimes (see Eq.”
Evolution of density profiles in high-z galaxies: compaction and quenching inside-out (2015, background): “−Mvir) relation of the simulations with results from abundance matching (Conroy & Wechsler 2009; Moster et al. 2010, 2013; Behroozi et al. 2010, 2013a) and observed kinematics (Burkert et al. 2015).”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “The halo masses of many of the galaxies in the high stellar mass tertile of the LRIS sample are likely above 1012 M⊙ based on either their clustering properties (Coil et al. 2008) or halo abundance matching (Behroozi, Conroy, and Wechsler 2010).”
SHORT-LIVED STAR-FORMING GIANT CLUMPS IN COSMOLOGICAL SIMULATIONS OF z ≈ 2 DISKS (2010, background): “…and dark matter halos suggests that atz ≈ 2, much like atz = 0, typically not more than≈ 10% of the baryons associated with halos of any mass have turned into stars (Moster et al. 2010; Behroozi et al. 2010; Wake et al. 2011), causing some tension with the high efficiency of ’cold-mode’ accretion.”