A spectroscopic study of three rich galaxy clusters at z = 0.31

Couch, Warrick J.; Sharples, R. M.

doi:10.1093/mnras/229.3.423

Cited by 422 publications

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“…This raises a further question: What fraction of the kϩa/aϩk galaxies observed in distant clusters were previously starburst galaxies with e(a) spectra? Although a comparison of the fraction of e(a) galaxies with that of kϩa/aϩk types gives a rough estimate of the fraction of kϩa/aϩk galaxies that have evolved from e(a) galaxies (Couch & Sharples 1987;Barger et al 1996;Poggianti et al 1999), the dusty nature of starburst galaxies makes this estimation considerably inaccurate. For example, based on the detection of some kϩa galaxies by 1.4 GHz Very Large Array radio observations, Smail et al (1999) suggested that even kϩa galaxies classified by EW([O ii]) and EW(Hd) can be dusty starburst galaxies.…”

Section: ‫2ע6‬mentioning

confidence: 99%

“…z 1 0.2 Dressler & Gunn (1983) proposed that this peculiar spectroscopic property was due to the presence of a substantial population of A-type stars, having been formed as part of a recent starburst that was abruptly truncated. Since Couch & Sharples (1987) suggested a possible evolutionary link between these EϩA galaxies and the general population of blue galaxies found in distant clusters (Butcher & Oemler 1978), several attempts have been made to determine what physical processes are closely associated with the abrupt truncation of star formation that is inferred from their spectral characteristics (e.g., Abraham et al 1996;Barger et al 1996;Balogh et al 1997;Couch et al 1998;Poggianti et al 1999). Although the formation of EϩA galaxies has been often discussed in terms of physical processes specific to the cluster environment, Zabludoff et al (1996) found that a large fraction of nearby EϩA galaxies lie in the field rather than in clusters and therefore suggested that cluster environmental effects such as interaction with the cluster gravitational potential or intracluster medium are not responsible for EϩA formation.…”

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confidence: 99%

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Formation and Evolution of E+A Galaxies in Dusty Starburst Galaxies

Bekki¹,

Shioya²,

Couch³

2001

The Astrophysical Journal

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The formation and evolution of the "EϩA" (also named "kϩa" and "aϩk" types by A. Dressler et al.) galaxies found in significant numbers in the cores of intermediate-redshift clusters has been extensively discussed by many authors. In this Letter, we model the spectral, dynamical, and morphological evolution of a prime candidate for producing this spectral signature: a dusty starburst associated with a major galaxy merger. We show that as this system evolves dynamically, its spectral type changes from an "e(a)" type (exhibiting strong Hd absorption and modest [O ii] emission-the identifying features of local dusty starburst galaxies) to a kϩa type and then finally to a passive "k" type. This result shows that galaxies with an e(a) spectral type can be precursors to the kϩa systems and that dynamical evolution greatly controls the spectral evolution in these merger cases. Our simulations also show that a merger with very high infrared luminosity ( ) is more likely to showan e(a) spectrum, which implies that spectral types can be correlated with infrared fluxes in dusty starburst galaxies. With these results, we discuss the origin of the evolution of kϩa/aϩk galaxies in distant clusters and the role merging is likely to have.

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Section: ‫2ע6‬mentioning

confidence: 99%

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confidence: 99%

Formation and Evolution of E+A Galaxies in Dusty Starburst Galaxies

Bekki¹,

Shioya²,

Couch³

2001

The Astrophysical Journal

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“…This galaxy population was first discovered, and has been primarily studied since, inside clusters (Dressler & Gunn 1983;Couch & Sharples 1987;Tran et al 2003;Poggianti et al 1999Poggianti et al , 2009, even if post-starburst galaxies have also been found in the field. Numerous studies have been undertaken to study the properties of field post-starburst galaxies at low redshift (Liu & Kennicutt 1995;Zabludoff et al 1996;Chang et al 2001;Norton et al 2001;Goto & SDSS collaboration 2003;Quintero et al 2004;Yang et al 2004), and at z > 0.3 (Hammer et al 1997;Dressler et al 1999;Poggianti et al 1999;Balogh et al 1999;Tran et al 2004;Yang et al 2008;Poggianti et al 2009).…”

Section: Introductionmentioning

confidence: 99%

K+a galaxies in the zCOSMOS survey

Vergani

Zamorani

Lilly³

et al. 2009

A&A

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Aims. The identities of the main processes triggering and quenching star-formation in galaxies remain unclear. A key stage in evolution, however, appears to be represented by post-starburst galaxies. To investigate the prevalence of these galaxies and their impact on galaxy evolution in general, we initiated a multiwavelength study of galaxies with k + a spectral features in the well-studied COSMOS field. Methods. We examine a mass-selected sample of k + a galaxies in the COSMOS field at z = 0.48−1.2 using the spectroscopic zCOSMOS sample. To classify galaxies in their k + a phase, we use a spectroscopic criterion, based on the amplitude of the Hδ absorption line and the absence of the [OII] emission line. We develop our analysis for a well-defined sample by imposing stringent confidence levels on the spectroscopic redshifts and spectral measurements. We compare our results for two mass-selected samples of star-forming and quiescent galaxies selected using a purely spectral classification scheme from the 10 000 zCOSMOS catalogue (i.e. , based on measurements of 4000 Å break and EW[OII]). Results. In our mass-limited sample, k+a galaxies occupy the brightest tail of the luminosity distribution. They are as massive as quiescent galaxies and populate the green valley in the colour versus luminosity (or stellar mass) distribution. A small percentage (<8%) of these galaxies have radio and/or X-ray counterparts (implying an upper limit to the SFR of ∼8 M yr −1 ). Over the entire redshift range explored, the class of post-starburst galaxies is morphologically a heterogeneous population with a similar incidence of bulge-dominated and disky galaxies. This distribution does not vary with the strength of the Hδ absorption line but instead with stellar mass in a way reminiscent of the well-known mass-morphology relation. The results about the incidence of asymmetries and the concentration of the light distribution derived from HST/ACS images imply that this galaxy population possibly represents an intermediate stage of galaxy evolution. Although k + a galaxies are also found in underdense regions, they appear to reside typically in a similarly rich environment as quiescent galaxies on a physical scale of ∼2-8 Mpc, and in groups they show a morphological early-to-late type ratio similar to the quiescent galaxy class. With the current data set, we do not find evidence of statistical significant evolution in either the number/mass density of k + a galaxies at intermediate redshift with respect to the local values, or the spectral properties, although more solid results on this and other aspects will be obtained following the completion of the survey. Conclusions. Several mechanisms related and unrelated to the environment are at work in quenching star-formation activity in galaxies on short timescales (<1 Gyr). Those galaxies, which are affected by a sudden quenching of their star-formation activity, may increase the stellar mass of the red-sequence by up to a non-negligible level of ∼10%.

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“…High starburst mass fractions: Extreme E+A galaxies may have starburst mass fractions M burst /M * > ∼ 0.2 (Couch & Sharples 1987;Barger et al 1996;Liu & Green 1996). Such high burst masses indicate the galaxies must have been extremely gas-rich; Milky Way-type spirals simply lack sufficient gas to fuel such a starburst.…”

Section: The Progenitors Of E+a'smentioning

confidence: 99%

Gasdynamics and Starbursts in Interacting Galaxies

Mihos

1999

Galaxy Interactions at Low and High Redshift

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Abstract.The onset of gaseous inflows and central activity in interacting galaxies is driven largely by induced bars in the host galaxies. The stability of galaxies against growing bar modes is a direct function of their structural properties -galaxies with central bulges or low disk surface densities are more stable against central starbursts than are bulgeless or disk-dominated systems. Low surface brightness galaxies prove less prone to bar formation and central starbursts than do normal high surface brightness galaxies. This stability of LSB disks also resolves many of the dynamical pitfalls encountered when attempting to link poststarburst "E+A" galaxies to interactions involving normal high surface brightness galaxy progenitors.

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A spectroscopic study of three rich galaxy clusters at z = 0.31

Cited by 422 publications

References 0 publications

Formation and Evolution of E+A Galaxies in Dusty Starburst Galaxies

Formation and Evolution of E+A Galaxies in Dusty Starburst Galaxies

K+a galaxies in the zCOSMOS survey

Gasdynamics and Starbursts in Interacting Galaxies

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