The Environmental Dependence of the Evolving S0 Fraction

Just, Dennis W.; Zaritsky, Dennis; Sand, David J.; Desai, Vandana; Rudnick, G.

doi:10.1088/0004-637x/711/1/192

Cited by 63 publications

(78 citation statements)

References 50 publications

(86 reference statements)

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“…They find that the combined tidal interaction can have a significant impact on the morphology of galaxies, inducing series of bursts of star formation that increase the stellar mass in the central bulges. These results suggest that groups are suitable environments where S0 galaxies can be formed, in line with implications from observational evidence Just et al 2010). …”

Section: Introductionsupporting

confidence: 80%

Simulating the evolution of disc galaxies in a group environment – II. The influence of close encounters between galaxies

Villalobos¹,

Lucia²,

Murante³

2014

Monthly Notices of the Royal Astronomical Society

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We study the evolution of disc galaxies in group environments under the effect of both the global tidal field and close-encounters between galaxies, using controlled Nbody simulations of isolated mergers. We find that close-range encounters between galaxies are less frequent and less damaging to disc galaxies than originally expected, since they mostly occur when group members have lost a significant fraction of their initial mass to tidal stripping. We also find that group members mostly affect disc galaxies indirectly by modifying their common global tidal field. Different initial orbital parameters of group members introduce a significant "scatter" in the evolution of general properties of disc galaxies around a "median" evolution that is similar to when only the effect of the global tidal field is included. Close-encounters introduce a high variability in the properties of disc galaxies, even slowing their evolution in some cases, and could wash out correlations between galaxy properties and the group total mass. The combined effect of the global tidal field and close-encounters appears to be inefficient at forming/enhancing central stellar bulges. This implies that bulges of S0 galaxies should be mostly composed by young stars, which is consistent with recent observations.

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Section: Introductionsupporting

confidence: 80%

Simulating the evolution of disc galaxies in a group environment – II. The influence of close encounters between galaxies

Villalobos¹,

Lucia²,

Murante³

2014

Monthly Notices of the Royal Astronomical Society

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“…It has also been studied the properties of galaxies in the infalling region at intermediate/high redshifts. Just et al (2015) found evidences of preprocessing of galaxies in the infall region of clusters in the redshift range 0.4 < z < 0.8. These authors found that at z ∼ 0.6, the fraction of red galaxies in the infall region is larger than in the field (see also Moran et al 2007 andPatel et al 2011) In this paper, we study the population of galaxies in the infalling region of massive groups taken from Zandivarez & Martínez (2011).…”

Section: Introductionmentioning

confidence: 94%

Galaxies infalling into groups: filaments versus isotropic infall

Martínez

Muriel

Coenda

2015

Mon. Not. R. Astron. Soc.

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We perform a comparative analysis of the properties of galaxies infalling into groups classifying them accordingly to whether they are: falling along filamentary structures; or they are falling isotropically. For this purpose, we identify filamentary structures connecting massive groups of galaxies in the SDSS. We perform a comparative analysis of some properties of galaxies in filaments, in the isotropic infall region, in the field, and in groups. We study the luminosity functions (LF) and the dependence of the specific star formation rate (SSFR) on stellar mass, galaxy type, and projected distance to the groups that define the filaments. We find that the LF of galaxies in filaments and in the isotropic infalling region are basically indistinguishable between them, with the possible exception of late-type galaxies. On the other hard, regardless of galaxy type, their LFs are clearly different from that of field or group galaxies. Both of them have characteristic absolute magnitudes and faint end slopes in between the field and group values. More significant differences between galaxies in filaments and in the isotropic infall region are observed when we analyse the SSFR. We find that galaxies in filaments have a systematically higher fraction of galaxies with low SSFR as a function of both, stellar mass and distance to the groups, indicating a stronger quenching of the star formation in the filaments compared to both, the isotropic infalling region, and the field. Our results suggest that some physical mechanisms that determine the differences observed between field galaxies and galaxies in systems, affect galaxies even when they are not yet within the systems.

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“…Poggianti et al 2008;Fumagalli & Gavazzi 2008) or the emergence of lenticular galaxies (S0) and corresponding decline in spirals (e.g. Desai et al 2007;Just et al 2010). Although spiral disc fading is not a sufficient explanation for the rise of S0s (Christlein & Zabludoff 2004), spirals are strongly affected both in numbers and properties by dense environments.…”

Section: Introductionmentioning

confidence: 99%

Disc colours in field and cluster spiral galaxies at 0.5 ≲z≲ 0.8

Cantale

Jablonka

Courbin

et al. 2016

A&A

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We present a detailed study of the colours of late-type galaxy discs for ten of the EDisCS galaxy clusters with 0.5 z 0.8. Our cluster sample contains 172 spiral galaxies, and our control sample is composed of 96 field disc galaxies. We deconvolved their ground-based V and I images obtained with FORS2 at the VLT with initial spatial resolutions between 0.4 and 0.8 arcsec to achieve a final resolution of 0.1 arcsec with 0.05 arcsec pixels, which is close to the resolution of the ACS at the HST. After removing the central region of each galaxy to avoid pollution by the bulges, we measured the V − I colours of the discs. We find that 50% of cluster spiral galaxies have disc V − I colours redder by more than 1σ of the mean colours of their field counterparts. This is well above the 16% expected for a normal distribution centred on the field disc properties. The prominence of galaxies with red discs depends neither on the mass of their parent cluster nor on the distance of the galaxies to the cluster cores. Passive spiral galaxies constitute 20% of our sample. These systems are not abnormally dusty. They are are made of old stars and are located on the cluster red sequences. Another 24% of our sample is composed of galaxies that are still active and star forming, but less so than galaxies with similar morphologies in the field. These galaxies are naturally located in the blue sequence of their parent cluster colour-magnitude diagrams. The reddest of the discs in clusters must have stopped forming stars more than ∼5 Gyr ago. Some of them are found among infalling galaxies, suggesting preprocessing. Our results confirm that galaxies are able to continue forming stars for some significant period of time after being accreted into clusters, and suggest that star formation can decline on seemingly long (1 to 5 Gyr) timescales.

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The Environmental Dependence of the Evolving S0 Fraction

Cited by 63 publications

References 50 publications

Simulating the evolution of disc galaxies in a group environment – II. The influence of close encounters between galaxies

Simulating the evolution of disc galaxies in a group environment – II. The influence of close encounters between galaxies

Galaxies infalling into groups: filaments versus isotropic infall

Disc colours in field and cluster spiral galaxies at 0.5 ≲z≲ 0.8

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