Emergence of the Galaxy Morphology-Star Formation Activity-Clustercentric Radius Relations in Galaxy Clusters

Abstract

We investigate when and how the relations of galaxy morphology and star forming activity with clustercentric radius become evident in galaxy clusters. We identify 162 galaxy clusters with total mass $M_{\mathrm{tot}}^{\mathrm{cl}}>5\times 10^{13}{\mathrm{M}}_{\odot }$ at $z=0.625$ in the Horizon Run 5 (HR5) cosmological hydrodynamical simulation and study how the properties of the galaxies with stellar mass $M_{\ast }>5\times 10^9{\mathrm{M}}_{\odot }$ near the cluster main progenitors have evolved in the past. Galaxies are classified into disk, spheroid, and irregular morphological types according to the asymmetry and Sersic index of their stellar mass distribution. We also classify galaxies into active and passive ones depending on their specific star-formation rate. We find that the morphology-clustercentric radius relation (MRR) emerges at $z\simeq 1.8$ as the fraction of spheroidal types exceeds 50% in the central region ($d\lesssim 0.1R_{200}$). Galaxies outside the central region remain disk-dominated. Numerous encounters between galaxies in the central region seem to be responsible for the morphology transformation from disks to spheroids. We also find that the star formation activity-clustercentric radius relation emerges at an epoch different from that of MRR. At $z\simeq 0.8$, passive galaxies start to dominate the intermediate radius region ($0.1\lesssim d/R_{200}\lesssim 0.3$) and this "quenching region" grows inward and outward thereafter. The region dominated by early-type galaxies (spheroids and passive disks) first appears at the central region at $z\simeq 1.8$, expands rapidly to larger radii as the population of passive disks grows in the intermediate radii, and clusters are dominated by early types after $z\simeq 0.8$.

arXiv comment19 pages, 9 figures, ApJ accepted

References in corpus (68)

• Astropy: A Community Python Package for Astronomy
• Planck 2015 results. XIII. Cosmological parameters
• The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package
• Efficient Computation of CMB anisotropies in closed FRW models
• Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
• Mass and environment as drivers of galaxy evolution in SDSS and zCOSMOS and the origin of the Schechter function
• Evolution since z = 0.5 of the Morphology-Density relation for Clusters of Galaxies
• Morphological Transformation from Galaxy Harassment
• The Galactic disk mass function: reconciliation of the HST and nearby determinations
• Multi-scale initial conditions for cosmological simulations
• Galaxy Stellar Mass Assembly between 0.2<z<2 from the S-COSMOS survey
• The Asymmetry of Galaxies: Physical Morphology for Nearby and High Redshift Galaxies
• The Importance of Satellite Quenching for the Build-Up of the Red Sequence of Present Day Galaxies
• The Morphology - Density Relation in z ~ 1 Clusters
• A wide field Hubble Space Telescope study of the cluster CL0024+16 at z=0.4. I: morphological distributions to 5 Mpc radius
• Transients from Initial Conditions: A Perturbative Analysis
• Environmental Dependence of Properties of Galaxies in the Sloan Digital Sky Survey
• The History of the Baryon Budget: Cosmic Logistics in a Hierarchical Universe
• Evolution Since z=1 of the Morphology-density Relation of Galaxies
• The Era of Star Formation in Galaxy Clusters
• The role of mergers and halo spin in shaping galaxy morphology
• Morphology Segregation of Galaxies in the Color-Color Gradient Space
• A simple multigrid scheme for solving the Poisson equation with arbitrary domain boundaries
• Photometric scaling relations of lenticular and spiral galaxies
• A snapshot on galaxy evolution occurring in the Great Wall: the role of Nurture at z=0
• The role of mergers in driving morphological transformation over cosmic time
• The Environment of Passive Spiral Galaxies in the SDSS
• Galaxy And Mass Assembly (GAMA): Stellar mass functions by Hubble type
• Interactions of Galaxies in the Galaxy Cluster Environment
• Combined Effects of Galaxy Interactions and Large-Scale Environment on Galaxy Properties
• Star Formation and AGN Activity in Galaxy Clusters from $z=1-2$: a Multi-wavelength Analysis Featuring $Herschel$/PACS
• Star-Forming Brightest Cluster Galaxies at 0.25 < z < 1.25: A Transitioning Fuel Supply
• The SAMI Galaxy Survey: mass as the driver of the kinematic morphology - density relation in clusters
• The Horizon Run N-body Simulation: Baryon Acoustic Oscillations and Topology of Large Scale Structure of the Universe
• The Morphology of Passively Evolving Galaxies at z ~ 2 from HST/WFC3 Deep Imaging in the Hubble Ultradeep Field
• The Horizon Run 5 Cosmological Hydrodynamic Simulation: Probing Galaxy Formation from Kilo- to Giga-parsec Scales
• Transformation of Morphology and Luminosity Classes of the SDSS Galaxies
• Horizon Run 4 Simulation: Coupled Evolution of Galaxies and Large-scale Structures of the Universe
• What shapes a galaxy? - Unraveling the role of mass, environment and star formation in forming galactic structure
• Morphological Fractions of Galaxies in WINGS Clusters: revisiting the Morphology-Density Paradigm
• Secular diffusion in discrete self-gravitating tepid discs II: accounting for swing amplification via the matrix method
• The star formation rate and stellar content contributions of morphological components in the EAGLE simulations
• A New Halo Finding Method for N-Body Simulations
• RAMSES-CH: A New Chemodynamical Code for Cosmological Simulations
• Near-infrared bulge-disc correlations of lenticular galaxies
• New Horizon: On the origin of the stellar disk and spheroid of field galaxies at $z=0.7$
• Rapid Quenching of Galaxies at Cosmic Noon
• The specific star formation rate function at different mass scales and quenching: A comparison between cosmological models and SDSS
• Red but not dead : Unveiling the Star-forming Far-infrared Spectral Energy Distribution of SpARCS Brightest Cluster Galaxies at 0 < z < 1.8
• Effects of the initial conditions on cosmological $N$-body simulations
• Sussing Merger Trees : The Impact of Halo Merger Trees on Galaxy Properties in a Semi-Analytic Model
• The Most Bound Halo Particle-Galaxy Correspondence Model: Comparison between Models with Different Merger Timescales
• Evidence for Morphology and Luminosity Transformation of Galaxies at High Redshifts
• Formation and Morphology of the First Galaxies in the Cosmic Morning
• Effects of large-scale environment on the assembly history of central galaxies
• Ongoing growth of the brightest cluster galaxies via major dry mergers in the last ~6 Gyr
• Evolution of star formation rate-density relation over cosmic time in a simulated universe: the observed reversal reproduced
• Dynamical flows through Dark Matter Haloes: Inner perturbative dynamics, secular evolution, and applications
• The role of environment in the morphological transformation of galaxies in 9 intermediate redshift clusters
• The population of early-type galaxies: how it evolves with time and how it differs from passive and late-type galaxies
• Resonant thickening of self-gravitating discs: imposed or self-induced orbital diffusion in the tightly wound limit
• Minor Mergers are not enough: The importance of Major Mergers during Brightest Cluster Galaxy assembly
• Star-Gas Misalignment in Galaxies: II. Origins Found from the Horizon-AGN Simulation
• The submillimetre view of massive clusters at z~0.8-1.6
• Evolution of Late-type Galaxies in a Cluster Environment: Effects of High-speed Multiple Encounters with Early-type Galaxies
• Low-Surface-Brightness Galaxies are missing in the observed Stellar Mass Function
• Quasars as a tracer of large-scale structures in the distant universe
• Connecting galaxy structure and star formation: the role of environment in formation of S0 galaxies