Testing Galaxy Quenching Theories with Scatter in the Stellar to Halo Mass Relation

Abstract

We use the scatter in the stellar-to-halo mass relation to constrain galaxy evolution models. If the efficiency of converting accreted baryons into stars varies with time, halos of the same present-day mass but different formation histories will have different z=0 galaxy stellar mass. This is one of the sources of scatter in stellar mass at fixed halo mass, ${\sigma }_{\log M\ast }$. For massive halos that undergo rapid quenching of star formation at z~2, different mechanisms that trigger this quenching yield different values of ${\sigma }_{\log M\ast }$. We use this framework to test various models in which quenching begins after a galaxy crosses a threshold in one of the following physical quantities: redshift, halo mass, stellar mass, and stellar-to-halo mass ratio. Our model is highly idealized, with other sources of scatter likely to arise as more physics is included. Thus, our test is whether a model can produce scatter lower than observational bounds, leaving room for other sources. Recent measurements find ${\sigma }_{\log M\ast }=0.16$ dex for 10^11 Msol galaxies. Under the assumption that the threshold is constant with time, such a low value of ${\sigma }_{\log M\ast }$ rules out all of these models with the exception of quenching by a stellar mass treshold. Most physical quantities, such as metallicity, will increase scatter if they are uncorrelated with halo formation history. Thus, to decrease the scatter of a given model, galaxy properties would correlate tightly with formation history, creating testable predictions for their clustering. Understanding why ${\sigma }_{\log M\ast }$ is so small may be key to understanding the physics of galaxy formation.

arXiv comment10 pages, 6 figures, submitted to MNRAS

References in corpus (33)

• The broken hierarchy of galaxy formation
• Stellar Masses and Star Formation Histories for 10^5 Galaxies from the Sloan Digital Sky Survey
• How Do Galaxies Get Their Gas?
• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• The Average Star Formation Histories of Galaxies in Dark Matter Halos from z=0-8
• The Baryon Oscillation Spectroscopic Survey of SDSS-III
• Galaxy Bimodality due to Cold Flows and Shock Heating
• The epochs of early-type galaxy formation as a function of environment
• Galactic star formation and accretion histories from matching galaxies to dark matter haloes
• Concentrations of Dark Halos from their Assembly Histories
• The ages and metallicities of galaxies in the local universe
• Galaxies in a simulated $\Lambda$CDM Universe I: cold mode and hot cores
• Properties of Galaxy Groups in the SDSS: I.-- The Dependence of Colour, Star Formation, and Morphology on Halo Mass
• The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation
• New constraints on the evolution of the stellar-to-dark matter connection: a combined analysis of galaxy-galaxy lensing, clustering, and stellar mass functions from z=0.2 to z=1
• Connecting Galaxies, Halos, and Star Formation Rates Across Cosmic Time
• Modelling the Galaxy Bimodality: Shutdown Above a Critical Halo Mass
• A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies: II. Formation of Red Ellipticals
• LSD: Lyman-break galaxies Stellar populations and Dynamics. I: Mass, metallicity and gas at z~3.1
• The Connection between Galaxies and Dark Matter Structures in the Local Universe
• Assembly bias in the clustering of dark matter haloes
• Satellite Kinematics III: Halo Masses of Central Galaxies in SDSS
• On the Lack of Evolution in Galaxy Star Formation Efficiency
• A 2.5% measurement of the growth rate from small-scale redshift space clustering of SDSS-III CMASS galaxies
• Detection of the Splashback Radius and Halo Assembly bias of Massive Galaxy Clusters
• The 2dF-SDSS LRG and QSO survey: Evolution of the Luminosity Function of Luminous Red Galaxies to z=0.6
• Galaxy evolution near groups and clusters: ejected satellites and the spatial extent of environmental quenching
• Mapping stellar content to dark matter halos. II. Halo mass is the main driver of galaxy quenching
• Evidence of Halo Assembly Bias in Massive Clusters
• The Clustering of Massive Halos
• Luminosity Function Constraints on the Evolution of Massive Red Galaxies Since z~0.9
• Connecting massive galaxies to dark matter halos in BOSS - I. Is galaxy color a stochastic process in high-mass halos?
• Hierarchical Galaxy Growth and Scatter in the Stellar Mass - Halo Mass Relation

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• Halo Histories vs. Galaxy Properties at z=0, I: The Quenching of Star Formation
• Physical Correlations of the Scatter between Galaxy Mass, Stellar Content, and Halo Mass
• Probing Galaxy Assembly Bias in BOSS Galaxies Using Void Probabilities
• Galaxy assembly bias of central galaxies in the Illustris simulation
• The Observed Evolution of the Stellar Mass - Halo Mass Relation for Brightest Central Galaxies
• Surrogate modelling the Baryonic Universe I: The colour of star formation
• The Outer Stellar Mass of Massive Galaxies: A Simple Tracer of Halo Mass with Scatter Comparable to Richness and Reduced Projection Effects
• Surrogate modelling the Baryonic Universe II: on forward modelling the colours of individual and populations of galaxies
• Halo Histories vs. Galaxy Properties at z=0, III: The Properties of Star-Forming Galaxies
• The evolution of compact massive quiescent and starforming galaxies derived from the $R_e-R_h$ and $M_{\mathrm{star}}-M_h$ relations
• The Impact of Environment on Late Time Evolution of the Stellar Mass - Halo Mass Relation
• Constraining the scatter in the galaxy-halo connection at Milky Way masses
• Small scale clustering of BOSS galaxies: dependence on luminosity, color, age, stellar mass, specific star formation rate and other properties
• Why do semi-analytic models predict higher scatter in the stellar mass-halo mass relation than cosmological hydrodynamic simulations?
• Isolated dark matter deprived galaxies in hydrodynamical simulations: real objects or artefacts?
• The origin of galaxy colour bimodality in the scatter of the Stellar-to-Halo Mass Relation
• On the baryon budget in the X-ray-emitting circumgalactic medium of Milky Way-mass galaxies