On the Infall of Matter Into Clusters of Galaxies and Some Effects on Their Evolution

Gunn, James E.; Gott, J. Richard

doi:10.1086/151605

Cited by 3,817 publications

(4,186 citation statements)

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“…This suggests that in dense environments ther is the existence of the transformation from late to early type. Many physical mechanisms, such as galaxy harassment (Moore et al 1996), rampressure stripping (Gunn & Gott 1972) and galaxy-galaxy merging (Toomre & Toomre 1972) can explain such process. But we also note that other galaxy properties do not present significant dependence on local environment.…”

Section: Correlations Between Galaxy Properties and Local Galaxy Densitymentioning

confidence: 99%

“…Many authors have investigated correlations between environment and galaxy properties, such as ones between environment and morphology (e.g., Postman & Geller 1984;Dressler et al 1997;Hashimoto & Oemler 1999;Fasano et al 2000;Tran et al 2001;Goto et al 2003;Helsdon & Ponman 2003;Treu et al 2003), ones between environment and star formation rate (e.g., Hashimoto et al 1998;Lewis et al 2002;G´omez et al 2003;Balogh et al 2004a;Tanaka et al 2004;Kelm, Focardi & Sorrentino 2005), and ones between environment and colour (e.g., Tanaka et al 2004;Balogh et al 2004b;Hogg et al 2004). In order to explain these correlations, various physical mechanisms have been proposed, including rampressure stripping (Gunn & Gott 1972;Kent 1981;Fujita & Nagashima 1999;Quilis, Moore & Bower 2000); galaxy harassment (Moore et al 1996(Moore et al , 1999; cluster tidal forces (Byrd &Valtonen 1990;Valluri 1993;Gnedin 2003); and interaction/merging of galaxies (Icke 1985;Lavery & Henry 1988;Mamon 1992;Bekki 1998).…”

Section: Introductionmentioning

confidence: 99%

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Local Environmental Dependence of Galaxy Properties in a Volume-Limited Sample of Main Galaxies

Deng

Zhang

et al. 2007

Chin. J. Astron. Astrophys.

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Using a volume-limited sample of Main Galaxies from the SDSS Data Release 5, we investigate the dependence of galaxy properties on local environment. For each galaxy, the local three-dimensional density is calculated. We find that galaxy morphologies strongly depend on local environment: galaxies in dense environments have predominantly early type morphologies, but other galaxy properties do not present significant dependence on local environment. Clearly, this puts a important constraint on proposed physical mechanisms.

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Section: Correlations Between Galaxy Properties and Local Galaxy Densitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Local Environmental Dependence of Galaxy Properties in a Volume-Limited Sample of Main Galaxies

Deng

Zhang

et al. 2007

Chin. J. Astron. Astrophys.

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“…Recent IFU observations demonstrate that many nearby spiral galaxies show negative gradients in stellar ages and metallicities, supporting this inside-out picture (González Delgado et al 2014;Sánchez-Blázquez et al 2014;Li et al 2015;Belfiore et al 2017;Goddard et al 2017). On the other hand, if "nurture" dominates galaxy evolution, external processes such as ram-pressure stripping (Gunn & Gott 1972), high speed galaxy encounters (Moore et al 1996), galaxy mergers (Mihos & Hernquist 1994), and "strangulation" (Larson et al 1980;Balogh et al 2000;Peng et al 2015) are responsible for quenching. In this picture, star formation quenching is likely to occur globally or in the outer regions of galaxies first due to the lack of continuous supply for the cold gas reservoir.…”

Section: Introductionmentioning

confidence: 99%

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

Lin

Belfiore

Pan

et al. 2017

ApJ

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We study the role of cold gas in quenching star formation in the green valley by analyzing ALMA 12 CO (1-0) observations of three galaxies with resolved optical spectroscopy from the MaNGA survey. We present resolution-matched maps of the star formation rate and molecular gas mass. These data are used to calculate the star formation efficiency (SFE) and gas fraction ( f gas ) for these galaxies separately in the central "bulge" regions and outer disks. We find that, for the two galaxies whose global specific star formation rate (sSFR) deviates most from the star formation main sequence, the gas fraction in the bulges is significantly lower than that in their disks, supporting an "inside-out" model of galaxy quenching. For the two galaxies where SFE can be reliably determined in the central regions, the bulges and disks share similar SFEs. This suggests that a decline in f gas is the main driver of lowered sSFR in bulges compared to disks in green valley galaxies. Within the disks, there exist common correlations between the sSFR and SFE and between sSFR and f gas on kiloparsec scales-the local SFE or f gas in the disks declines with local sSFR. Our results support a picture in which the sSFR in bulges is primarily controlled by f gas , whereas both SFE and f gas play a role in lowering the sSFR in disks. A larger sample is required to confirm if the trend established in this work is representative of the green valley as a whole.

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“…Balogh, Navarro & Morris 2000), stripping via e.g. ram pressure (Gunn & Gott 1972) or tidal effects (King 1962), and mergers (that transform spirals into ellipticals; e.g. Toomre & Toomre 1972), are a number of "quenching" effects that are triggered by changes in a galaxy's environment (e.g.…”

Section: Introductionmentioning

confidence: 99%

The abundance and environment of dark matter haloes

Metuki

Libeskind

Hoffman

2016

Mon. Not. R. Astron. Soc.

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An open question in cosmology and the theory of structure formation is to what extent does environment affect the properties of galaxies and haloes. The present paper aims at shedding light on this problem. The paper focuses on the analysis of a dark matter only simulation and it addresses the issue of how the environment affects the abundance of haloes, which are are assigned four attributes: their virial mass, an ambient density calculated with an aperture that scales with R vir (∆ M ), a fixedaperture (∆ R ) ambient density, and a cosmic web classification (i.e. voids, sheets, filaments, and knots, as defined by the V-web algorithm). ∆ M is the mean density around a halo evaluated within a sphere of a radius of 5R vir , where R vir is the virial radius. ∆ R is the density field Gaussian smoothed with R = 4 h −1 Mpc, evaluated at the center of the halo. The main result of the paper is that the difference between haloes in different web elements stems from the difference in their mass functions, and does not depend on their adaptive-aperture ambient density. A dependence on the fixed-aperture ambient density is induced by the cross correlation between the mass of a halo and its fixed-aperture ambient density.

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On the Infall of Matter Into Clusters of Galaxies and Some Effects on Their Evolution

Cited by 3,817 publications

References 1 publication

Local Environmental Dependence of Galaxy Properties in a Volume-Limited Sample of Main Galaxies

Local Environmental Dependence of Galaxy Properties in a Volume-Limited Sample of Main Galaxies

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

The abundance and environment of dark matter haloes

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