Investigating the Projected Phase Space of Gaussian and Non-Gaussian Clusters

Abstract

By way of the projected phase-space (PPS), we investigate the relation between galaxy properties and cluster environment in a subsample of groups from the Yang Catalog. The sample is split according to the gaussianity of the velocity distribution in the group into gaussian (G) and non-gaussian (NG). Our sample is limited to massive clusters with ${\mathrm{M}}_{200}\ge 10^{14}{\mathrm{M}}_{\odot }$ and $0.03\le \mathrm{z}\le 0.1$. NG clusters are more massive, less concentrated and have an excess of faint galaxies compared to G clusters. NG clusters show mixed distributions of galaxy properties in the PPS compared to the G case. Using the relation between infall time and locus on the PPS, we find that, on average, NG clusters accreted $\sim 10^{11}{\mathrm{M}}_{\odot }$ more stellar mass in the last $\sim 5$ Gyr than G clusters. The relation between galaxy properties and infall time is significantly different for galaxies in G and NG systems. The more mixed distribution in the PPS of NG clusters translates into shallower relations with infall time. Faint galaxies whose first crossing of the cluster virial radius happened 2-4 Gyr ago in NG clusters are older and more metal-rich than in G systems. All these results suggest that NG clusters experience a higher accretion of pre-processed galaxies, which characterizes G and NG clusters as different environments to study galaxy evolution.

arXiv commentAccepted for publication in MNRAS, 17 pages, 9 Figures

References in corpus (62)

• The NumPy array: a structure for efficient numerical computation
• The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package
• The physical properties of star forming galaxies in the low redshift universe
• Mass and environment as drivers of galaxy evolution in SDSS and zCOSMOS and the origin of the Schechter function
• MILES: A Medium resolution INT Library of Empirical Spectra
• NYU-VAGC: a galaxy catalog based on new public surveys
• Galaxy Groups in the SDSS DR4: I. The Catalogue and Basic Properties
• Morphological quenching of star formation: making early-type galaxies red
• The Fifth Data Release of the Sloan Digital Sky Survey
• The Origin of Star Formation Gradients in Rich Galaxy Clusters
• The Green Valley is a Red Herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early- and late-type galaxies
• Ram Pressure Stripping of Spiral Galaxies in Clusters
• Galaxy evolution in groups and clusters: satellite star formation histories and quenching timescales in a hierarchical Universe
• The Thirteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey MApping Nearby Galaxies at Apache Point Observatory
• Galaxy evolution in groups and clusters: star formation rates, red sequence fractions, and the persistent bimodality
• The effect of galaxy mass ratio on merger--driven starbursts
• Formation of a spiral galaxy in a major merger
• Mean proper motions, space orbits and velocity dispersion profiles of Galactic globular clusters derived from Gaia DR2 data
• Improving galaxy morphologies for SDSS with Deep Learning
• The Observational Distribution of Internal Velocity Dispersions in Nearby Galaxy Clusters
• The driving mechanism of starbursts in galaxy mergers
• Pre-Processing of Galaxies before Entering a Cluster
• Natural Downsizing in Hierarchical Galaxy Formation
• Phase-space Analysis in the Group and Cluster environment: Time since Infall and Tidal Mass Loss
• The tidal stripping of satellites
• Both starvation and outflows drive galaxy quenching
• Morphology Segregation of Galaxies in the Color-Color Gradient Space
• Ram pressure stripping of disc galaxies orbiting in clusters. I. Mass and radius of the remaining gas disc
• A Systematic Study of X-Ray Substructure of Galaxy Clusters Detected in the ROSAT All-Sky Survey
• Disentangling satellite galaxy populations using orbit tracking in simulations
• Measuring Mass Loss Rates from Galactic Satellites
• The velocity modulation of galaxy properties in and near clusters: quantifying the decrease in star formation in backsplash galaxies
• Mapping stellar content to dark matter halos. II. Halo mass is the main driver of galaxy quenching
• Discovery of a Dissociative Galaxy Cluster Merger with Large Physical Separation
• The halo merger rate in the Millennium Simulation and implications for observed galaxy merger fractions
• Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS
• AGN host galaxy mass function in COSMOS: is AGN feedback responsible for the mass-quenching of galaxies?
• Physical properties of SDSS satellite galaxies in projected phase-space
• Slow quenching of star formation in OMEGAWINGS clusters: galaxies in transition in the local universe
• Dark matter distribution function from non-extensive statistical mechanics
• The environmental dependence of gas accretion onto galaxies: quenching satellites through starvation
• A Systematic Analysis of Caustic Methods for Galaxy Cluster Masses
• Mass profiles and galaxy orbits in nearby galaxy clusters from the analysis of the projected phase-space
• X-ray Substructure Studies of Four Galaxy Clusters using XMM-Newton Data
• A homogeneous measurement of the delay between the onsets of gas stripping and star formation quenching in satellite galaxies of groups and clusters
• Quenching low-mass satellite galaxies: evidence for a threshold ICM density
• NoSOCS in SDSS. I. Sample Definition and Comparison of Mass Estimates
• Evidence of pre-processing and a dependence on dynamical state for low-mass satellite galaxies
• YZiCS: Unveiling Quenching History of Cluster Galaxies Using Phase-space Analysis
• SPIDER IX - Classifying Galaxy Groups according to their Velocity Distribution
• The Morphology-Density relationship in 1<z<2 clusters
• NoSOCS in SDSS. II. Mass Calibration of Low Redshift Galaxy Clusters with Optical and X-ray Properties
• Investigating the Relation between Galaxy Properties and the Gaussianity of the Velocity Distribution of Groups and Clusters
• Evidence for galaxies being pre-processed before accreted into clusters
• Exploring a new definition of the green valley and its implications
• Relaxation of a Collisionless System and the Transition to a New Equilibrium Velocity Distribution
• Segregation Effects According to the Evolutionary Stage of Galaxy Groups
• The time delay between star formation quenching and morphological transformation of galaxies in clusters: a phase-space view of EDisCS
• Constraints on feedback processes during the formation of early-type galaxies
• The Shape of Velocity Dispersion Profiles and the Dynamical State of Galaxy Clusters
• The Mass Density Profile and Star Formation History of Gaussian and Non-Gaussian Clusters
• "Observing" Unrelaxed Clusters in Dark Matter Simulations

Cited by in corpus (15)

• From Blue Cloud to Red Sequence: Evidence of Morphological Transition Prior to Star Formation Quenching
• The Three Hundred: Cluster Dynamical States and Relaxation Time Scale
• NGC 3314a/b and NGC 3312: Ram pressure stripping in Hydra I Cluster substructure
• The Three Hundred project: connection between star formation quenching and dynamical evolution in and around simulated galaxy clusters
• DS+: a method for the identification of cluster substructures
• Examining transitional galaxies to understand the role of clusters and their dynamical status in galaxy quenching
• Exploring Galaxy Evolution Time-Scales in Clusters: Insights from the Projected Phase Space
• The co-evolution of strong AGN and central galaxies in different environments
• CLASH-VLT: Galaxy cluster MACS J0329-0211 and its surroundings using galaxies as kinematic tracers
• New observational recipes for measuring dynamical state of galaxy clusters
• Boosting the evolutionary picture of Cl 0024+17 and MS 0451-03: A case study at intermediate-redshift
• Exploring the stellar populations of backsplash galaxies
• Estimating infall times of galaxies around clusters: how accurately can it be done with observational data?
• Late growth of early-type galaxies in low-z massive clusters
• The origin of ionized gas in retired galaxies: dynamical clues