The Physical Origins of The Morphology-Density Relation: Evidence for Gas Stripping from the SDSS

Abstract

We provide a physical interpretation and explanation of the morphology-density relation for galaxies, drawing on stellar masses, star formation rates, axis ratios and group halo masses from the Sloan Digital Sky Survey. We first re-cast the classical morphology-density relation in more quantitative terms, using low star formation rate (quiescence) as a proxy for early-type morphology and dark matter halo mass from a group catalog as a proxy for environmental density: for galaxies of a given stellar mass the quiescent fraction is found to increase with increasing dark matter halo mass. Our novel result is that - at a given stellar mass - quiescent galaxies are significantly flatter in dense environments, implying a higher fraction of disk galaxies. Supposing that the denser environments differ simply by a higher incidence of quiescent disk galaxies that are structurally similar to star-forming disk galaxies of similar mass, explains simultaneously and quantitatively these quiescence -nvironment and shape-environment relations. Our findings add considerable weight to the slow removal of gas as the main physical driver of the morphology-density relation, at the expense of other explanations.

published in ApJ: http://adsabs.harvard.edu/abs/2010ApJ...714.1779V

References in corpus (23)

• Galaxy Groups in the SDSS DR4: I. The Catalogue and Basic Properties
• Galaxy Zoo: the dependence of morphology and colour on environment
• The Importance of Satellite Quenching for the Build-Up of the Red Sequence of Present Day Galaxies
• Ram pressure stripping the hot gaseous halos of galaxies in groups and clusters
• Kinematic Structure of Merger Remnants
• The population of barred galaxies in the local universe I. Detection and characterisation of bars
• Multiple minor mergers: formation of elliptical galaxies and constraints for the growth of spiral disks
• Environmental Effects on Satellite Galaxies: The Link Between Concentration, Size and Colour Profile
• The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star-formation in cluster infall
• The DEEP2 Galaxy Redshift Survey: Evolution of the Color-Density Relation at 0.4 < z < 1.35
• A Wide-field Survey of Two Z~0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s
• Ram pressure stripping of disc galaxies orbiting in clusters. I. Mass and radius of the remaining gas disc
• A Halo Model of Galaxy Colors and Clustering in the SDSS
• Dissecting the Red Sequence--I. Star Formation Histories of Quiescent Galaxies: The Color-Magnitude vs. the Color-Sigma Relation
• The Dependence of Galaxy Morphology and Structure on Environment and Stellar Mass
• The Tully-Fisher relation for S0 galaxies
• The shapes of galaxies in the Sloan Digital Sky Survey
• Galaxy bulges and their black holes: a requirement for the quenching of star formation
• The Evolution of the Field and Cluster Morphology-Density Relation for Mass-Selected Samples of Galaxies
• Bars, ovals and lenses in early-type disk galaxies: probes of galaxy evolution
• The Rise and Fall of Galaxy Activity in Dark Matter Haloes
• Mass-Selection and the Evolution of the Morphology-Density Relation from z=0.8 to z=0
• Central and Satellite Colors in Galaxy Groups: A Comparison of the Halo Model and SDSS Group Catalogs

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• 3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since $z=3$
• Abundant molecular gas and inefficient star formation in intracluster regions: Ram pressure stripped tail of the Norma galaxy ESO137-001
• Bar quenching in gas-rich galaxies
• The distinct stellar-to-halo mass relations of satellite and central galaxies: insights from the IllustrisTNG simulations
• The Fornax3D project: Tracing the assembly history of the cluster from the kinematic and line-strength maps
• The MAGPI Survey -- science goals, design, observing strategy, early results and theoretical framework
• The fate of the gaseous disks of galaxies that fall into clusters
• Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies in the Local Universe I. - The Effect of the Group Environment on Star Formation in Spiral Galaxies
• Shape Evolution of Massive Early-Type Galaxies: Confirmation of Increased Disk Prevalence at z>1
• Investigating the Relation between Galaxy Properties and the Gaussianity of the Velocity Distribution of Groups and Clusters
• Specific Frequencies and Luminosity Profiles of Cluster Galaxies and Intracluster Light in Abell 1689
• The galaxy morphology-density relation in the EAGLE simulation
• Clustercentric distance or local density? It depends on galaxy morphology
• Connecting galaxy structure and star formation: the role of environment in formation of S0 galaxies
• The impact of cosmic variance on simulating weak lensing surveys
• The environment of AGNs and the activity degree of their surrounding galaxies
• The Arecibo Galaxy Environment Survey VII : A Dense Filament With Extremely Long HI Streams
• Galaxy populations in groups and clusters: evidence for a characteristic stellar mass scale at $M_{\ast }\sim 10^{9.5}{M}_{\odot }$
• Morphologies of galaxies within voids
• Early-type galaxies in the Antlia Cluster: global properties
• An Absence of Radio-Loud Active Galactic Nuclei in Geometrically Flat Quiescent Galaxies: Implications for Maintenance-Mode Feedback Models
• The XXL Survey XLV. Linking the ages of optically selected groups to their X-ray emission
• Quenched galaxies in clusters of galaxies and their outskirts
• Deep Extragalactic VIsible Legacy Survey (DEVILS): First Data Release Covering The D10 (COSMOS) Region
• HI in and behind the Hubble Frontier Field Clusters: A Deep MeerKAT Pilot Search out to $z\sim 0.5$
• Transforming galaxies with EASE: widespread structural changes enabled by short-lived spirals
• The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies