Morphological classification and structural parameters 
of galaxies in the Coma and Perseus clusters

Andreon, S.; Davoust, E.; Poulain, P.

doi:10.1051/aas:1997249

Cited by 53 publications

(109 citation statements)

References 6 publications

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“…Considering first the structure and morphology of the cluster members, we found some evidence for a lack of quiescent disk-like galaxies relative to the field population. In the context of cluster studies at lower redshift, this is consistent with the idea that the cluster ellipticals are formed early (z > 2) in dissipative mergers, probably continuing to evolve via dry mergers, whereas many S0's are formed much later at z 0.5 and decline in numbers toward higher redshifts (e.g., Dressler et al 1997;Andreon et al 1997;Smith et al 2005;Postman et al 2005;Poggianti et al 2009). An interesting related development is the observation that the fraction of quiescent galaxies in the field with disklike components appears to increase at z > 1, particular among massive (M * > 10 11 M ) systems (see references in Section 6.2).…”

Section: Discussionsupporting

confidence: 82%

SPECTROSCOPIC CONFIRMATION OF THE RICHz= 1.80 GALAXY CLUSTER JKCS 041 USING THE WFC3 GRISM: ENVIRONMENTAL TRENDS IN THE AGES AND STRUCTURE OF QUIESCENT GALAXIES

Newman

Ellis

Andreon

et al. 2014

ApJ

177

270

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We present Hubble Space Telescope imaging and grism spectroscopy in the field of the distant galaxy cluster JKCS 041 using the Wide Field Camera 3. We confirm that JKCS 041 is a rich cluster and derive a redshift z = 1.80 via the spectroscopic identification of 19 member galaxies, of which 15 are quiescent. These are centered upon diffuse X-ray emission seen by the Chandra observatory. As JKCS 041 is the most distant known cluster with such a large, spectroscopically confirmed quiescent population, it provides a unique opportunity to study the effect of the environment on galaxy properties at early epochs. We construct high-quality composite spectra of the quiescent cluster members that reveal prominent Balmer and metallic absorption lines. Using these, we measure the mean stellar ages in two bins of stellar mass. The quiescent cluster members' ages agree remarkably closely with that inferred by Whitaker et al. for similarly selected samples in the field, supporting the idea that the cluster environment is more efficient at truncating star formation while not having a strong effect on the mean epoch of quenching. We find some evidence (90% confidence) for a lower fraction of disk-like quiescent systems in JKCS 041 compared to a sample of coeval field galaxies drawn from the CANDELS survey. Taking this into account, we do not detect a significant difference between the mass-radius relations of the quiescent JKCS 041 members and our z ∼ 1.8 field sample. Finally, we demonstrate how differences in the morphological mixture of quenched systems can complicate measures of the environmental dependence of size growth.

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Section: Discussionsupporting

confidence: 82%

SPECTROSCOPIC CONFIRMATION OF THE RICHz= 1.80 GALAXY CLUSTER JKCS 041 USING THE WFC3 GRISM: ENVIRONMENTAL TRENDS IN THE AGES AND STRUCTURE OF QUIESCENT GALAXIES

Newman

Ellis

Andreon

et al. 2014

ApJ

177

270

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“…The stripping of the interstellar medium causes a decrease of the star formation rate, with a subsequent increase of the post starburst galaxy fraction. 6) Andreon et al (1997) found that early-type galaxies in CL 0939+4713 do not show a radial symmetry, but are distributed along a privileged direction. This direction roughly coincides with the X-ray major axis and therefore with the possible collision axis.…”

Section: Discussion Of the Merger Hypothesismentioning

confidence: 99%

XMM observation of the dynamically young galaxy cluster CL 0939+4713

Filippis

Schindler

Castillo-Morales

2003

A&A

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Abstract. We present an XMM observation of the distant galaxy cluster CL 0939+4713. The X-ray image shows pronounced substructure, with two main subclusters which have even some internal structure. This is an indication that the cluster is a dynamically young system. This conclusion is supported by the temperature distribution: a hot region is found between the two main subclusters indicating that they are at the beginning of a major merger, and that they will probably collide in a few hundreds of Myr. The intra-cluster gas of CL 0939+4713 shows inhomogeneities in the metal distribution, with the optically richer subcluster having a higher metallicity.

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“…Spectroscopic redshifts for almost all galaxies of interest are available in Treu et al (2015) and Ebeling et al (2014), making the photo-z pre-selection necessary only for excluding a few galaxies without a spectroscopic redshift but with a SED pointing toward a manifestly different redshift. Similarly, the passive pre-selection is in principle unnecessary because all non-passive galaxies are clearly A2, page 3 of 17 A&A 593, A2 (2016) Andreon et al (1996Andreon et al ( , 1997; numbers in boldface identify the band used for the isophotal analysis.…”

Section: Z < 1 Clustersmentioning

confidence: 99%

“…Abell 1656 (Coma) galaxies use ground-based V-or r-band observations, typically 20 min long with <1.2 arcsec seeing at a 2 m telescope (from Andreon et al 1996Andreon et al , 1997. Effective radii, derived as in this work and using the same software, are available in the references mentioned.…”

Section: Z < 1 Clustersmentioning

confidence: 99%

Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr

Andreon

Dong

Raichoor

2016

A&A

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We carried out a photometric and structural analysis in the rest-frame V band of a mass-selected (log M/M > 10.7) sample of red-sequence galaxies in 14 galaxy clusters, 6 of which are at z > 1.45, namely JKCS041, IDCS J1426.5+3508, SpARCS104922.6+564032.5, SpARCSJ021524-034331, XDCPJ0044.0-2033, and SPT-CLJ2040-4451. To this end, we reduced/analyzed about 300 orbits of multicolor images taken with the Advanced Camera for Survey and the Wide Field Camera 3 on the Hubble Space Telescope. We uniformly morphologically classified galaxies from z = 0.023 to z = 1.803, and we homogeneously derived sizes (effective radii) for the entire sample. Furthermore, our size derivation allows, and therefore is not biased by, the presence of the usual variety of morphological structures seen in early-type galaxies, such as bulges, bars, disks, isophote twists, and ellipiticy gradients. By using such a mass-selected sample, composed of 244 red-sequence early-type galaxies, we find that the log of the galaxy size at a fixed stellar mass, log M/M = 11, has increased with time at a rate of 0.023 ± 0.002 dex per Gyr over the last 10 Gyr, in marked contrast with the threefold increase found in the literature for galaxies in the general field over the same period. This suggests, at face value, that secular processes should be excluded as the primary drivers of size evolution because we observed an environmental dependent size growth. Using spectroscopic ages of Coma early-type galaxies we also find that recently quenched early-type galaxies are a numerically minor population not different enough in size to alter the mean size at a given mass, which implies that the progenitor bias is minor, i.e., that the size evolution measured by selecting galaxies at the redshift of observation is indistinguishable from the one that compares ancestors and descendents.

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Morphological classification and structural parameters of galaxies in the Coma and Perseus clusters

Cited by 53 publications

References 6 publications

SPECTROSCOPIC CONFIRMATION OF THE RICHz= 1.80 GALAXY CLUSTER JKCS 041 USING THE WFC3 GRISM: ENVIRONMENTAL TRENDS IN THE AGES AND STRUCTURE OF QUIESCENT GALAXIES

SPECTROSCOPIC CONFIRMATION OF THE RICHz= 1.80 GALAXY CLUSTER JKCS 041 USING THE WFC3 GRISM: ENVIRONMENTAL TRENDS IN THE AGES AND STRUCTURE OF QUIESCENT GALAXIES

XMM observation of the dynamically young galaxy cluster CL 0939+4713

Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr

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