The Morphological Content of 10 EDisCS Clusters at 0.5 &lt;<i>z</i>&lt; 0.8

Desai, Vandana; Dalcanton, Julianne J.; Aragón-Salamanca, Alfonso; Jablonka, P.; Poggianti, B. M.; Gogarten, Stephanie M.; Simard, Luc; Milvang-Jensen, B.; Rudnick, G.; Zaritsky, Dennis; Clowe, Douglas; Halliday, C.; Pelló, R.; Saglia, R. P.; White, Sarah V.

doi:10.1086/513310

Cited by 154 publications

(293 citation statements)

References 58 publications

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“…For all 20 fields deep optical multiband photometry obtained with FORS2/VLT (White et al 2005) and near-IR photometry obtained with SOFI/NTT is available. ACS/HST mosaic F814W imaging was also acquired for 10 of the highest redshift clusters (Desai et al 2007). FORS2/VLT was additionally used to obtain spectroscopy for 18 of the fields (Halliday et al 2004;Milvang-Jensen et al 2008).…”

Section: Ediscsmentioning

confidence: 99%

The galaxy stellar mass function and its evolution with time show no dependence on global environment

Vulcani

Poggianti

Oemler

et al. 2013

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We present an analysis of the galaxy stellar mass function in different environments at intermediate redshift (0.3 ≤ z ≤ 0.8) for two mass-limited galaxy samples. We use the IMACS Cluster Building Survey (ICBS; M * ≥ 10 10.5 M ) to study cluster, group and field galaxies at z = 0.3-0.45, and the ESO Distant Cluster Survey (EDisCS; M * ≥ 10 10.2 M ) to investigate cluster and group galaxies at z = 0.4-0.8. Our analysis thus includes galaxies with masses reaching just below that of the Milky Way. Excluding the brightest cluster galaxies, we show that the shape of the mass distribution does not seem to depend on global environment, Our two main results are: (1) Galaxies in the virialised regions of clusters, in groups, and in the field follow similar mass distributions. (2) Comparing the ICBS and EDisCS mass functions to mass functions in the local universe, we detect evolution from z ∼ 0.4-0.6 to z ∼ 0.07 in the sense that the population of low-mass galaxies has grown with time with respect to the population of massive galaxies. This evolution is independent of environment, i.e., the same for clusters and the field. Furthermore, considering only cluster galaxies, we find that no differences can be detected in their mass functions either within the virialised regions, or when we compare galaxies inside and outside the virial radius. Finally, we find that red and blue galaxies have different mass functions. However, the shapes of the mass functions of blue and red galaxies do not seem to depend on their environment (clusters groups and the field).

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Section: Ediscsmentioning

confidence: 99%

The galaxy stellar mass function and its evolution with time show no dependence on global environment

Vulcani

Poggianti

Oemler

et al. 2013

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“…2.1) and a quantitative analysis of their structural parameters (Desai et al 2007;Simard et al 2009). The visual classification was completed for all galaxies brighter than I auto = 23 mag, where I auto is the SExtractor AUTO magnitude measured on the I-band VLT images.…”

Section: Sample Selection From Ediscsmentioning

confidence: 99%

“…This classification has been described in detail in Desai et al (2007). We recall here its main features in particular those related to our purpose, i.e., the spiral galaxies.…”

Section: The Visual Classification Of the Galaxiesmentioning

confidence: 99%

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Barazza¹,

Jablonka

Desai

et al. 2009

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We present a study of large-scale bars in field and cluster environments out to redshifts of ∼0.8 using a final sample of 945 moderately inclined disk galaxies drawn from the EDisCS project. We characterize bars and their host galaxies and look for relations between the presence of a bar and the properties of the underlying disk. We investigate whether the fraction and properties of bars in clusters are different from their counterparts in the field. The properties of bars and disks are determined by ellipse fits to the surface brightness distribution of the galaxies using HST/ACS images in the F814W filter. The bar identification is based on quantitative criteria after highly inclined (>60 • ) systems have been excluded. The total optical bar fraction in the redshift range z = 0.4−0.8 (median z = 0.60), averaged over the entire sample, is 25% (20% for strong bars). For the cluster and field subsamples, we measure bar fractions of 24% and 29%, respectively. We find that bars in clusters are on average longer than in the field and preferentially found close to the cluster center, where the bar fraction is somewhat higher (∼31%) than at larger distances (∼18%). These findings however rely on a relatively small subsample and might be affected by small number statistics. In agreement with local studies, we find that disk-dominated galaxies have a higher optical bar fraction (∼45%) than bulge-dominated galaxies (∼15%). This result is based on Hubble types and effective radii and does not change with redshift. The latter finding implies that bar formation or dissolution is strongly connected to the emergence of the morphological structure of a disk and is typically accompanied by a transition in the Hubble type. The question whether internal or external factors are more important for bar formation and evolution cannot be answered definitely. On the one hand, the bar fraction and properties of cluster and field samples of disk galaxies are quite similar, indicating that internal processes are crucial for bar formation. On the other hand, we find evidence that cluster centers are favorable locations for bars, which suggests that the internal processes responsible for bar growth are supported by the typical interactions taking place in such environments.

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“…This change is stronger in lower-mass clusters ). The cluster velocity dispersion is mildly dependent on the morphological fraction (Desai et al 2007), not only in low-z but also in high-z clusters, up to z ≈ 1 at least. Fasano et al (2015) have recently revisited the morphologydensity paradigm, using the WIde-field Nearby Galaxy-cluster Survey (WINGS) database of galaxies in nearby clusters.…”

Section: Introductionmentioning

confidence: 96%

“…The morphological content of clusters changes rapidly up to z ≈ 0.5, with a decreasing fraction of S0 and an increasing fraction of S with z (Dressler et al 1997;Fasano et al 2000;Postman et al 2005;D'Onofrio et al 2015), but then this evolution slows down at higher z (Desai et al 2007). This change is stronger in lower-mass clusters ).…”

Section: Introductionmentioning

confidence: 99%

Structural and dynamical modeling of WINGS clusters

Cava

Biviano

Mamon

et al. 2017

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Context. We study the distribution of galaxies in nearby clusters to shed light on the evolutionary processes at work within clusters and prepare for a full dynamical analysis to be conducted in forthcoming papers of this series. Aims. We use the Wide-field Nearby Galaxy-clusters Survey (WINGS) database complemented with literature data. We assign galaxy membership to individual clusters, then select a sample of 67 clusters with at least 30 spectroscopic members each. 53 of these clusters do not show evidence of substructures in phase-space, as measured by the Dressler-Shectman test, while 14 do. We estimate the virial radii and circular velocities of the 67 clusters by a variety of proxies (velocity dispersion, X-ray temperature, and richness) and use these estimates to build stack samples from these 53 and 14 clusters, that we call 'Reg' and 'Irr' stacks, respectively. We show that our results are robust with regard to the choice of the virial radii and circular velocities used to scale galaxy radii and velocities in the stacking procedure. We determine the number-density and velocity-dispersion profiles of Elliptical (E), S0, and Spiral+Irregular (S) galaxies in the Reg and Irr samples, separately, and fit models to these profiles. Methods. The number density profiles of E, S0, and S galaxies are adequately described by either a Navarro, Frenk, & White (NFW) or a cored King model, both for the Reg and Irr samples, with a slight preference for the NFW model. The spatial distribution concentration increases from the S to the S0 and to the E populations, both in the Reg and the Irr stacks, reflecting the well-known morphology-radius relation. Reg clusters have a more concentrated spatial distribution of E and S0 galaxies than Irr clusters, while the spatial distributions of S galaxies in Reg and Irr clusters have a similar concentration. We propose a new phenomenological model that provides acceptable fits to the velocity dispersion profile of all our galaxy samples. The velocity dispersion profiles become steeper and with a higher normalization from E to S0 to S galaxies. The S0 velocity dispersion profile is close to that of E galaxies in Reg clusters, and intermediate between those of E and S galaxies in Irr clusters. Results. Our results suggest that S galaxies are a recently accreted cluster population, that take ≤ 3 Gyr to evolve into S0 galaxies after accretion, and in doing so modify their phase-space distribution, approaching that of cluster ellipticals. While in Reg clusters this evolutionary process is mostly completed, it is still ongoing in Irr clusters.

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The Morphological Content of 10 EDisCS Clusters at 0.5 <z< 0.8

Cited by 154 publications

References 58 publications

The galaxy stellar mass function and its evolution with time show no dependence on global environment

The galaxy stellar mass function and its evolution with time show no dependence on global environment

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Structural and dynamical modeling of WINGS clusters

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