At the Vigintennial of the Butcher–Oemler Effect

Pimbblet, Kevin A.

doi:10.1071/as03043

Cited by 17 publications

(19 citation statements)

References 83 publications

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“…In their Seyfert subsample a slight excess of galaxies with a spiral geometry is evident. In 1980 Dressler discovered a morphology-density (T −Σ) relation for galaxies: the fraction of elliptical like (E + S0) galaxies increases strongly with increasing local galaxy density, whereas the numbers of spiral galaxies decrease (see e.g., Table 1 in Pimbblet 2003). In good agreement with further studies of this relationship he also derives values for different environments: from galaxies in the field over poor and rich groups to clusters.…”

Section: Morphologysupporting

confidence: 61%

H I in nearby low-luminosity QSO host galaxies

König¹,

Eckart

García-Marín³

et al. 2009

A&A

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We searched for 21 cm H i emission in a sample of 27 previously CO detected nearby galaxies hosting low-luminosity quasi -stellar objects (QSOs). In this paper we investigate the relationship between the H i and infrared properties of these host galaxies, compare the atomic and molecular gas content and look for connections to the optical and FIR properties. The single dish observations have been made with the Effelsberg 100-m telescope with a beam size of 9.5 . The sample objects have been drawn from a wide-angle survey for optically bright QSOs (HES), which have declinations δ > −30 • and redshifts up to z = 0.06. 12 host galaxies from the sample have been detected in the H i 21 cm emission line. Eight of them have a spiral geometry, whereas the other four are bulge dominated and probably of elliptical type (E/S0). Three of the objects seem to be in a phase of merging/interaction. The neutral atomic gas masses range from 1.1×10 9 M up to 3.8×10 10 M . The median H i gas mass in the whole sample is of the order of 11.4×10 9 M , which is a factor of two higher than the H i content of our galaxy. We find no strong correlation between H i mass and IR luminosity.The objects agree well within the expectations from the Tully-Fisher relation. In the color-color diagram we find all sources in the estimated locations. With the non-detected sources we clearly sample an upper envelope of this mass distribution.

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Section: Morphologysupporting

confidence: 61%

H I in nearby low-luminosity QSO host galaxies

König¹,

Eckart

García-Marín³

et al. 2009

A&A

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“…In higher-redshift clusters, the fraction of blue galaxies is higher (the so-called " Butcher-Oemler" effect, Butcher & Oemler 1978, 1984Pimbblet 2003), and so are the fractions of cluster galaxies with spectra characterized by young stellar populations (Dressler & Gunn 1983;Dressler et al 1999;Poggianti et al 1999) and the fraction of galaxies with late-type A&A 537, A58 (2012) morphology (Dressler et al 1997;Fasano et al 2000;Postman et al 2005;Smith et al 2005). Higher-z clusters are also observed to contain a higher fraction of infrared (IR) emitting galaxies (the so called "IR Butcher-Oemler effect", Saintonge et al 2008;Haines et al 2009;Temporin et al 2009), where most of the IR emission is powered by SF.…”

Section: In the Localmentioning

confidence: 99%

The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Popesso¹,

Biviano²,

Rodighiero³

et al. 2012

A&A

102

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Aims. Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (Σ(SFR)/M) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift z ≈ 1.6. Methods. We use deep far-infrared PACS data at 100 and 160 µm to accurately estimate the total star formation rate of the Luminous Infrared Galaxy population of 9 clusters with mass ∼ 10 15 M ⊙ , and 9 groups/poor clusters with mass ∼ 5 × 10 13 M ⊙ . Estimates of the field Σ(SFR)/M are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe.Results. The field Σ(SFR)/M increases with redshift up to z ∼ 1 and it is constant thereafter. The evolution of the Σ(SFR)/M-z relation in galaxy systems is much faster than in the field. Up to redshift z ∼ 0.2, the field has a higher Σ(SFR)/M than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar Σ(SFR)/M, while massive clusters have significantly lower Σ(SFR)/M than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z ∼ 1.6, where the group Σ(SFR)/M lies above the field Σ(SFR)/M -z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching.

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“…However, analyzing the inner 500 kpc of both A2125 and A2218 (39 and 78 galaxies, listed in Table 1 as core values) yields similar fractions. These values are due to the well-known ButcherOemler effect in these two intermediate-redshift clusters (Butcher & Oemler 1978;Dressler & Gunn 1982), which causes the increased fraction of star-forming and starburst objects compared to nearby clusters (see Pimbblet [2003] for a review). We note that the increased number of blue galaxies is clear in both these clusters despite their different cluster morphologies, richnesses, and dynamical states.…”

Section: Spectrophotometric Classificationmentioning

confidence: 99%

Cluster Populations in Abell 2125 and 2218

Rakos¹,

Schombert²

2005

Astron J

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We combine new narrowband photometry with archival Wide Field Planetary Camera 2 (WFPC2) data for A2218 (z ¼ 0:18) and A2125 (z ¼ 0:25), two clusters with intermediate redshifts but very different cluster properties, in order to examine the evolution of galaxy populations. A2218 is a dense, elliptical-rich cluster (Bautz-Morgan type II) similar to the Coma Cluster in its evolutionary appearance, whereas A2125 is a less dense, more open cluster (Bautz-Morgan type II-III), although similar in richness to A2218. The color-magnitude relation indicates that A2125 has a more developed blue population than A2218 (the Butcher-Oemler effect), although both clusters have significant numbers of blue galaxies (ranging in star formation rate from normal, star-forming disks to starburst systems) as compared to a present-day cluster. The colors of the red populations are identical in A2125 and A2218 and are well fitted by passive evolution models. We are able, for the first time, to combine archived WFPC2 images with our narrowband photometry for a color, morphological, and structural analysis of the blue Butcher-Oemler population. We find the blue population to be composed of two subpopulations, a bright, spiral population and a fainter, dwarf starburst population. A2125 is richer in bright starburst systems, a phenomenon apparently induced by the cluster's younger dynamical state. In addition, a majority of the S0 population in A2125 and A2218 is composed of bulge + disk systems, whereas nearby clusters such as Coma are composed primarily of lenticulars ( pure disk S0s). The structural parameters of the S0 bulges in A2125 and A2218 are identical to the structure parameters of cluster ellipticals, suggesting that the disks of some S0s in intermediate-redshift clusters are stripped away, with the leftover bulges evolving into present-day ellipticals.

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At the Vigintennial of the Butcher–Oemler Effect

Cited by 17 publications

References 83 publications

H I in nearby low-luminosity QSO host galaxies

H I in nearby low-luminosity QSO host galaxies

The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Cluster Populations in Abell 2125 and 2218

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