The Star Formation Histories of Galaxies in Distant Clusters

Poggianti, Bianca M.; Smail, Ian; Dressler, Alan; Couch, Warrick J.; Barger, A. J.; Butcher, H. R.; Ellis, Richard S.; Oemler, Augustus

doi:10.1086/307322

Cited by 712 publications

(1,122 citation statements)

References 76 publications

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“…There are two hypotheses for the formation of S0's, one is "Nature" where it is believed that early types were formed as such, and the other is "Nurture" according to which S0's are transformed spirals. Some of the recent observations indicate that the clusters at intermediate redshifts (z ∼ 0.1 − 0.3) tend to have a higher fraction of S0's at the expense of spirals (e.g., Poggianti et al 1999, Fasano et al 2000. These observations support the "Nurture" scenario.…”

Section: Motivationmentioning

confidence: 59%

GMRTHI observations of the Eridanus group of galaxies

Omar

Dwarakanath

2005

J Astrophys Astron

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Abstract.The GMRT H i 21cm-line observations of galaxies in the Eridanus group are presented. The Eridanus group, at a distance of ∼ 23 Mpc, is a loose group of ∼ 200 galaxies. The group extends more than 10 Mpc in projection. The velocity dispersion of the galaxies in the group is ∼ 240 km s −1 . The galaxies are clustered into different sub-groups. The overall population mix of the group is 30% (E+S0) and 70% (Sp+Irr). The observations of 57 Eridanus galaxies were carried out with the GMRT for ∼ 200 hour. H i emission was detected from 31 galaxies. The channel rms of ∼ 1 mJy beam −1 was achieved for most of the image-cubes made with 4 hour of data. The corresponding H i column density sensitivity (3σ) is ∼ 1 × 10 20 cm −2 for a velocity-width of ∼ 13.4 km s −1 . The 3σ detection limit of H i mass is ∼ 1.2 × 10 7 M ⊙ for a line-width of 50 km s −1 . Total H i images, H i velocity fields, global H i line profiles, H i mass surface densities, H i disk parameters and H i rotation curves are presented. The velocity fields are analysed separately for the approaching and the receding sides of the galaxies. This data will be used to study the H i and the radio continuum properties, the Tully-Fisher relations, the dark matter halos, and the kinematical and H i lopsidedness in galaxies.

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Section: Motivationmentioning

confidence: 59%

GMRTHI observations of the Eridanus group of galaxies

Omar

Dwarakanath

2005

J Astrophys Astron

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“…However, there has been long-standing tension between the relatively short transition time-scales derived from the abundance of post-starburst (PSB) and similar galaxies (e.g. Poggianti et al 1999;Balogh et al 1999) that appear to be caught in the act of transforming, and the nonzero fraction of star-forming galaxies in clusters and groups which imply a much longer time between accretion and the end of star formation (e.g. McGee et al 2011).…”

Section: T R a N S F O R M At I O N T I M E -S C A L E Smentioning

confidence: 99%

Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

Balogh

McGee

Mok

et al. 2016

Mon. Not. R. Astron. Soc.

136

230

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“…In the general environment, it is widely known that the star formation rate (SFR) depends on local density, with galaxies living in dense regions having their star for-mation rates strongly reduced with respect to field galaxies (Balogh et al 1997;Poggianti et al 1999;Elbaz et al 2007). Evidence has also emerged showing that this SFRdensity relation is largely due to an increasing fraction of passive galaxies in dense environment, whereas the starforming population does not show any significant trend with the environment (Peng et al 2010;Wijesinghe et al 2012).…”

Section: Introductionmentioning

confidence: 99%

The star formation activity in cosmic voids

Ricciardelli¹,

Cava²,

Varela³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using a sample of cosmic voids identified in the Sloan Digital Sky Survey Data Release 7, we study the star formation activity of void galaxies. The properties of galaxies living in voids are compared with those of galaxies living in the void shells and with a control sample, representing the general galaxy population. Void galaxies appear to form stars more efficiently than shell galaxies and the control sample. This result can not be interpreted as a consequence of the bias towards low masses in underdense regions, as void galaxy subsamples with the same mass distribution as the control sample also show statistically different specific star formation rates. This highlights the fact that galaxy evolution in voids is slower with respect to the evolution of the general population. Nevertheless, when only the star forming galaxies are considered, we find that the star formation rate is insensitive to the environment, as the main sequence is remarkably constant in the three samples under consideration. This fact implies that environmental effects manifest themselves as fast quenching mechanisms, while leaving the non-quenched galaxies almost unaffected, as their star formation activity is largely regulated by the mass of their halo. We also analyse galaxy properties as a function of void-centric distance and find that the enhancement in the star formation activity with respect to the control sample is observable up to a radial distance 1.5 · R void . This result can be used as a suitable definition of void shells. Finally, we find that larger voids show an enhanced star formation activity in the shells with respect to their smaller counterparts, that could be related to the different dynamical evolution experienced by voids of different sizes.

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The Star Formation Histories of Galaxies in Distant Clusters

Cited by 712 publications

References 76 publications

GMRTHI observations of the Eridanus group of galaxies

GMRTHI observations of the Eridanus group of galaxies

Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

The star formation activity in cosmic voids

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