Hα‐derived Star Formation Rates for Three<i>z</i>≃0.75 EDisCS Galaxy Clusters

Finn, Rose; Zaritsky, Dennis; McCarthy, Donald W.; Poggianti, Bianca M.; Rudnick, Gregory; Halliday, C.; Milvang-Jensen, B.; Pelló, R.; Simard, Luc

doi:10.1086/431642

Cited by 151 publications

(209 citation statements)

References 55 publications

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“…as in Finn et al (2005). In practice, the redshift distributions of high-z and the mid-z samples partly overlap as can be seen from Table 1.…”

Section: Sample Selection and Vlt/fors2 Optical Imagingmentioning

confidence: 72%

“…X-ray observations with the XMM-Newton satellite of three EDisCS clusters have been published in Johnson et al (2006) with more clusters being observed. H-alpha observations of three clusters have been published in Finn et al (2005) with more clusters also being observed. Finally, the analysis of Spitzer/IRAC observations of all EDisCS clusters is in progress (Finn et al, in preparation).…”

Section: Introductionmentioning

confidence: 99%

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Evolution of the early-type galaxy fraction in clusters since z = 0.8

Simard

Clowe

Desai

et al. 2009

A&A

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We study the morphological content of a large sample of high-redshift clusters to determine its dependence on cluster mass and redshift. Quantitative morphologies are based on PSF-convolved, 2D bulge+disk decompositions of cluster and field galaxies on deep Very Large Telescope FORS2 images of eighteen, optically-selected galaxy clusters at 0.45 < z < 0.80 observed as part of the ESO Distant Cluster Survey ("EDisCS"). Morphological content is characterized by the early-type galaxy fraction f et , and early-type galaxies are objectively selected based on their bulge fraction and image smoothness. This quantitative selection is equivalent to selecting galaxies visually classified as E or S0. Changes in early-type fractions as a function of cluster velocity dispersion, redshift and star-formation activity are studied. A set of 158 clusters extracted from the Sloan Digital Sky Survey is analyzed exactly as the distant EDisCS sample to provide a robust local comparison. We also compare our results to a set of clusters from the Millennium Simulation. Our main results are: (1) the early-type fractions of the SDSS and EDisCS clusters exhibit no clear trend as a function of cluster velocity dispersion. (2) Mid-z EDisCS clusters around σ = 500 km s −1 have f et 0.5 whereas high-z EDisCS clusters have f et 0.4. This represents a ∼25% increase over a time interval of 2 Gyr. (3) There is a marked difference in the morphological content of EDisCS and SDSS clusters. None of the EDisCS clusters have early-type galaxy fractions greater than 0.6 whereas half of the SDSS clusters lie above this value. This difference is seen in clusters of all velocity dispersions. (4) There is a strong and clear correlation between morphology and star formation activity in SDSS and EDisCS clusters in the sense that decreasing fractions of [OII] emitters are tracked by increasing early-type fractions. This correlation holds independent of cluster velocity dispersion and redshift even though the fraction of [OII] emitters decreases from z ∼ 0.8 to z ∼ 0.06 in all environments. Our results pose an interesting challenge to structural transformation and star formation quenching processes that strongly depend on the global cluster environment (e.g., a dense ICM) and suggest that cluster membership may be of lesser importance than other variables in determining galaxy properties.

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“…as in Finn et al (2005). In practice, the redshift distributions of high-z and the mid-z samples partly overlap as can be seen from Table 1.…”

Section: Sample Selection and Vlt/fors2 Optical Imagingmentioning

confidence: 72%

Section: Introductionmentioning

confidence: 99%

Evolution of the early-type galaxy fraction in clusters since z = 0.8

Simard

Clowe

Desai

et al. 2009

A&A

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“…The grey histogram shows the distribution of all galaxies; the red, green, and blue histograms are those objects belonging to the red sequence, the green valley, and the blue cloud, respectively. dictated by the possibility that the identification of virial entities here using analytic prescriptions, such as the one proposed by Finn et al (2005), might be not appropriate given the unrelaxed nature of these substructures. The resulting distribution of galaxies belonging to the different substructures in the velocity space is shown in Fig.…”

Section: Identification Of the Substructures In The Velocity Spacementioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

150

254

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We study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions that are selected from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) with the purpose of understanding the origin of the red sequence in dense environments. The sample spans a wide range in morphological types (from dwarf ellipticals to Im and BCD) and stellar masses (10 7 M star 10 11.5 M ). We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies, including UV, optical, mid-and far-infrared imaging data, as well as optical and HI spectroscopic data. We first identify the different dynamical substructures that compose the Virgo cluster, and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures or as a function of galaxy density. Our analysis indicates that all the most massive galaxies (M star 10 11 M ) are slow rotators and are the dominant galaxies of the different cluster substructures, which are generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs, as also indicated by their very old stellar populations. Slow rotators of lower stellar mass (10 8.5M star 10 11 M ) are also preferentially located within the different high-density substructures of the cluster. Their position in the velocity space indicates that they are virialised within the cluster; thus, they are Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later form the cluster (pre-processing). On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star-formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies, which still have rotation curves typical of star-forming systems.

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“…Using the redshift dependence of the critical density and the virial mass to relate the line-of-sight velocity dispersion to the cluster mass, R 200 can be expressed as (see Finn et al 2005)…”

Section: Velocity Dispersionmentioning

confidence: 99%

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Kurk

Cimatti

Zamorani

et al. 2009

A&A

108

142

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Context. Clusters of galaxies represent important laboratories for studying galaxy evolution and formation. Well established and relaxed clusters are known below z < 1.4, as well as, clusters in formation found close to radio galaxies at z > 2, but the in-between redshift range, during which clusters are expected to undergo significant changes, is almost unexplored. Aims. By studying a galaxy overdensity in redshift and angular distribution at z = 1.6, uncovered in the Galaxy Mass Assembly ultra-deep Spectroscopic Survey (GMASS), we provide insight into the evolution of cluster galaxies at high redshift. Methods. We present a study of the significance of the galaxy overdensity at z = 1.6, Cl 0332-2742, its velocity dispersion, and X-ray emission. We identify the colour bimodality of the cluster members and compare the properties of members of Cl 0332-2742 with galaxies outside the overdensity. Results. From the redshifts of the 42 overdensity members, we measure a velocity dispersion of 500 km s −1 . We conservatively estimate the overdensity in redshift space for the spike at z = 1.6 in the GMASS field to be 8.3 ± 1.5. A map of the surface density of galaxies at z = 1.6 in the GMASS field shows that its structure is irregular with several filaments and local overdensities. The differences in the physical properties of Cl 0332-2742 member and field galaxies agree with the latest hierarchical galaxy formation models: for overdensity members, the star formation rate (SFR), and specific SFR, is approximately 50% lower than for the field galaxies; overdensity galaxies are twice the age, on average, of field galaxies; and there is a higher proportion of both massive (M > 10 10.7 M ), and early-type galaxies, inside Cl 0332-2742 than in the field. Among the 42 members, seven have spectra consistent with being passively evolving, massive galaxies. These are all located within an area where the surface density of z = 1.6 galaxies is highest. In a z − J colour-magnitude diagram, the photometric data of these early-type galaxies are in close agreement with a theoretical red sequence of a galaxy cluster at redshift z = 1.6, which formed most of its stars in a short burst of star formation at z ∼ 3. Conclusions. We conclude that the redshift spike at z = 1.6 in the GMASS field represents a sheet-like structure in the cosmic web, and that the area with the highest surface density within this structure, containing already seven passively evolving galaxies, will evolve into a cluster of galaxies at a later time.

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Hα‐derived Star Formation Rates for Threez≃0.75 EDisCS Galaxy Clusters

Cited by 151 publications

References 55 publications

Evolution of the early-type galaxy fraction in clusters since z = 0.8

Evolution of the early-type galaxy fraction in clusters since z = 0.8

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

GMASS ultradeep spectroscopy of galaxies at z ~ 2

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