Environmental Effects on Late‐Type Galaxies in Nearby Clusters

By A. Boselli, G. Gavazzi. 2006

625 citations recorded by the source corpus.

The transformations that take place in late‐type galaxies in the environment of rich clusters of galaxies at z = 0 are reviewed. From the handful of late‐type galaxies that inhabit local clusters, whether they were formed in situ and survived as such, avoiding transformation or even destruction, or if they are newcomers that have recently fallen in from outside, we can learn an important lesson on the latest stages of galaxy evolution. We start by reviewing the observational scenario, covering the broadest possible stretch of the electromagnetic spectrum, from the gas tracers (radio and optical) to the star formation tracers (UV and optical), the old star tracers (near‐IR), and the dust (far‐IR). Strong emphasis is given to the three nearby, well‐studied clusters Virgo, A1367, and Coma, which are representative of different evolutionary stages, from unrelaxed and spiral‐rich (Virgo) to relaxed and spiral‐poor (Coma). We continue by providing a review of models of galaxy interactions that are relevant to clusters of galaxies. Prototypes of various mechanisms and processes are discussed, and their typical timescales are given in an a. Observations indicate the presence of healthy late‐type galaxies falling into nearby clusters individually or as part of massive groups. More rare are infalling galaxies belonging to compact groups, where significant preprocessing might take place. Once they have entered the cluster, they lose their gas and quench their star formation activity, becoming anemic. Observations and theory agree in indicating that the interaction with the intergalactic medium is responsible for the gas depletion. However, this process cannot be the origin of the cluster lenticular galaxy population. Physical and statistical properties of S0 galaxies in nearby clusters and at higher redshift indicate that they originate from spiral galaxies that have been transformed by gravitational interactions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f4917d84b687f457e8ae0a20c328f69d1d89f744

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Citations in the corpus

Virgo Cluster Early-Type Dwarf Galaxies with the Sloan Digital Sky Survey. II. Early-Type Dwarfs with Central Star Formation (2006, background): “Even violent relaxation, which might only apply for the case of merging groups or subclusters, would take at least a few crossing times tcr, with tcr ≈ 1.7 Gyr for the Virgo cluster (Boselli & Gavazzi 2006).”
Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample (2009, background): “The physical processes operating on galaxies and transformingtheir colours and/or morphologies are manifold and can be internally or externally driven and gravitationally or hydrodynamically induced (see for reviews Boselli & Gavazzi 2006; Treu et al. 2003).”
Galaxy Zoo: Passive Red Spirals . (2009, background): “In normal spirals, the gas that feeds ongoing star formation comes from infall of matter from a reservoir in the outer halo (Boselli & Gavazzi 2006).”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “Moreover, at sufficiently high gas densities, their own gas, including their corona and fountain effect, will be stripped entirely (Boselli & Gavazzi 2006).”
RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, background): “Interactions with the the intra-cluster medium and the cluster potential well may likely affect their SFHs by removing gas from the disks and quenching their SF activity, thus progressively turning them into anemic spirals (see e.g. Boselli & Gavazzi 2006 and references therein).”
A Wide-Field Survey of Two z ~ 0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s (2007, background): “Both of these flavors of interaction have been implicated before in the decline of star formation and the possible conversion of spirals into S0s (see Boselli & Gavazzi 2006, and references therein), yet a detailed evaluation of their importance remains elusive.”
Galaxy Zoo: the dependence of morphology and colour on environment (2008, background): “Direct stripping of gas from the disks of galaxies may also be important within groups (Boselli & Gavazzi 2006).”
GASP. I. Gas Stripping Phenomena in Galaxies with MUSE (2017, background): “7d d,gas ,stars (Boselli & Gavazzi 2006).”
The ACS Virgo Cluster Survey. XIII. SBF Distance Catalog and the Three-dimensional Structure of the Virgo Cluster (2007, background): “…structure, with galaxies of different morphological type showing different spatial and kinematic distributions (e.g., de Vaucouleurs 1961; Sandage & Tammann 1976; Huchra 1985; Binggeli et al. 1987, 1993; Yasuda et al. 1997; Gavazzi et al. 1999; Solanes et al. 2002; Boselli & Gavazzi 2006).”
The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, background): “Possible processes (see Boselli & Gavazzi 2006, for a review) that can transform spiral galaxies into fast-rotators in the field, or reduce spiral formation via cold accretion (Dekel et al. 2009) in the first place, include quenching produced by galaxy harassment (Moore et al. 1996, 1999), or…”
The effect of the environment on the Hi scaling relations (2011, background): “…(Giovanelli & Haynes 1985; Cayatte et al. 1990; Solanes et al. 2001; Boselli & Gavazzi 2009), providing strong constraints on the possible environmental mechanisms responsible for the quenching of the star formation in clusters of galaxies (see Boselli & Gavazzi 2006 and references therein).”
Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, background): “These galaxies have their gas content stripped by the environment (Boselli & Gavazzi 2006).”
The role of cold gas and environment on the stellar mass-metallicity relation of nearby galaxies (2012, background): “…though galaxies are thought to form heirarchically (e.g. Springel et al. 2005; Baugh 2006) and evidence shows that galaxies do not evolve as truely closed systems (e.g. Boselli & Gavazzi 2006), it is still important to test that these results are indeed consistent with the simple closed box model.”
A fundamental relation between the metallicity, gas content, and stellar mass of local galaxies (2013, background): “Both Skillman et al. (1996) and Peeples, Pogge & Stanek (2008) noted that local metal-rich galaxies tended to be gas poor, and Boselli & Gavazzi (2006) made the same observation for cluster galaxies.”
A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe (2007, background): “Boselli & Gavazzi (2006) review the important role of environmental effects on galaxy evolution.”
Virgo Cluster Early-Type Dwarf Galaxies with the Sloan Digital Sky Survey. III. Subpopulations: Distributions, Shapes, Origins (2007, background): “Even violent relaxation, which could apply for the case of infalling or merging groups, would take at least a few crossing times tcr, with tcr ≈ 1.7 Gyr for the Virgo cluster (Boselli & Gavazzi 2006).”
A DOZEN NEW GALAXIES CAUGHT IN THE ACT: GAS STRIPPING AND EXTENDED EMISSION LINE REGIONS IN THE COMA CLUSTER (2010, background): “It is well known that galaxies residing in the central region of clusters are generally deficient in gas(e.g., Giovanelli & Haynes 1985; Gavazzi 1987; Solanes et al. 2001; Boselli & Gavazzi 2006; BravoAlfaro et al. 2009).”
Ultraviolet tails and trails in cluster galaxies: a sample of candidate gaseous stripping events in Coma (2010, methodology): “The term GSE, as we use it here, doesnotdistinguish between various possible physical mechanisms: tidal interaction withneighbours or with the cluster potential, ram-pressure stripping, viscous stripping etc (see Boselli & Gavazzi 2006 for detailed discussion of these processes).”
Physical properties and environments of nearby galaxies (2009, background): “…in the field, and to have a correspondingly smaller Hi radius as well, and are thus more likely to be anemic (e.g., Giovanelli & Haynes 1983; Haynes, Giovanelli & Chincarini 1984; Warmels 1988; Cayatte et al. 1994; Vogt et al. 2004; Boselli & Gavazzi 2006; Levy et al. 2007; Chung et al. 2008).”