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

Filippis, E. De; Schindler, S.; Castillo-Morales, A.

doi:10.1051/0004-6361:20030481

Cited by 22 publications

(32 citation statements)

References 52 publications

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“…The area covers (2.5 Mpc) 2 in comoving space. The final X-ray surface brightness map has a drop of ∼ 2 magnitudes from the cluster centre to r 200 , which is consistent with observations of non-cooling flow clusters (Arnaud et al 2002, De Filippis et al 2003. The hierarchical formation of the cluster is clearly visible, especially at redshift 1, when the cluster is forming.…”

Section: X-ray Weighted Mapssupporting

confidence: 85%

Metal enrichment of the intra-cluster medium over a Hubble time for merging and relaxed galaxy clusters

Kapferer¹,

Kronberger²,

Weratschnig³

et al. 2007

A&A

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Abstract. We investigate the efficiency of galactic mass loss, triggered by ram-pressure stripping and galactic winds of cluster galaxies, on the chemical enrichment of the intra-cluster medium (ICM). We combine N-body and hydrodynamic simulations with a semi-numerical galaxy formation model. By including simultaneously different enrichment processes, namely ram-pressure stripping and galactic winds, in galaxy-cluster simulations, we are able to reproduce the observed metal distribution in the ICM. We find that the mass loss by galactic winds in the redshift regime z>2 is ∼10% to 20% of the total galactic wind mass loss, whereas the mass loss by ram-pressure stripping in the same epoch is up to 5% of the total ram-pressure stripping mass loss over the whole simulation time. In the cluster formation epochs z<2 ram-pressure stripping becomes more dominant than galactic winds. We discuss the non-correlation between the evolution of the mean metallicity of galaxy clusters and the galactic mass losses. For comparison with observations we present two dimensional maps of the ICM quantities and radial metallicity profiles. The shape of the observed profiles is well reproduced by the simulations in the case of merging systems. In the case of cool-core clusters the slope of the observed profiles are reproduced by the simulation at radii below ∼300 kpc, whereas at larger radii the observed profiles are shallower. We confirm the inhomogeneous metal distribution in the ICM found in observations. To study the robustness of our results, we investigate two different descriptions for the enrichment process interaction.

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Section: X-ray Weighted Mapssupporting

confidence: 85%

Metal enrichment of the intra-cluster medium over a Hubble time for merging and relaxed galaxy clusters

Kapferer¹,

Kronberger²,

Weratschnig³

et al. 2007

A&A

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“…Seitz et al (1996) used this deep HST/WFPC2 image to identify a few lensed objects, but no highly magnified gravitational arcs were detected. X-ray observations of A851, first with ROSAT and more recently with XMM-Newton, showed a very perturbed distribution with pronounced substructures and evidence for a dynamically young cluster (De Filippis et al 2003). Tentative 2D spectro-imaging led to the identification of a hot region between the two main sub-clusters, a characteristic of a major merger in an early phase.…”

Section: A4 Rx J09430+4659 (Z = 0407)mentioning

confidence: 99%

The matter distribution inz~ 0.5 redshift clusters of galaxies

Soucail

Foëx

Pointecouteau

et al. 2015

A&A

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We present an optical analysis of a sample of 11 clusters built from the EXCPRES sample of X-ray selected clusters at intermediate redshift (z ∼ 0.5). With a careful selection of the background galaxies, we provide the mass maps reconstructed from the weak lensing by the clusters. We compare them with the light distribution traced by the early-type galaxies selected along the red sequence for each cluster. The strong correlations between dark matter and galaxy distributions are confirmed, although some discrepancies arise, mostly for merging or perturbed clusters. The average M/L ratio of the clusters is found to be M/L r = 160 ± 60 in solar units (with no evolutionary correction), in excellent agreement with similar previous studies. No strong evolutionary effects are identified, although the small sample size reduces the significance of the result. We also provide a individual analysis of each cluster in the sample with a comparison between the dark matter, the galaxies, and the gas distributions. Some of the clusters are studied in the optical for the first time.

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“…However, we must caution that within the intermediate-luminosity range there are a number of galaxies for which we could not carry out line ratio diagnostics for AGN activity ( Paper I), which are indicated by crosses in the figure. Also, none of the cluster [O ii] emitters are spatially coincident with the XMM-Newton X-ray point sources detected at the level of L X (bol) k1:6 ; 10 43 ergs s À1 by De Filippis et al (2003). The X-ray observation does not exclude the possibility of these galaxies hosting nuclear activities, however.…”

Section: Luminosity Distributionmentioning

confidence: 79%

“…A rich, moderately distant (z ' 0:4069) galaxy cluster, Abell 851 (Cl 0939+4713; R:A: ¼ 09 h 42 m 56: s 2, decl: ¼ 46 59 0 12B0 [J2000.0]), offers evidence of filaments observed via the photometric redshift technique (Kodama et al 2001, hereafter K01). Since few clusters at this epoch have been studied well beyond their virial radii, it remains unclear whether the observed structures are actually filaments of cosmological origin or are related to an ongoing merger event (De Filippis et al 2003). In either case, Abell 851 presents a unique opportunity to study cluster galaxy evolution in a dynamically active environment on the large scale.…”

Section: Introductionmentioning

confidence: 99%

Infalling Faint [Oii] Emitters in Abell 851. II. Environment, Kinematics, and Star Formation History

Sato

Martin

2006

ApJ

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We report on the local environment, kinematics, and star formation history of [O ii]-selected objects in the z % 0:4 galaxy cluster Abell 851, using Keck optical spectra. A large fraction (%55%) of cluster [O ii] emitters show strong Balmer absorptions (k4 8 in H equivalent width). These e(a)-type spectra have been attributed to dusty starburst galaxies by Poggianti & Wu, an interpretation supported by our reddening measurements, which show a high frequency of very reddened [E(B À V ) k 0:5] galaxies. Our spectral modeling requires starburst ages of P1 Gyr, which is shorter than the cluster crossing timescale. We argue that this starburst phase occurs during cluster infall on the basis of the radial velocity distribution of the [O ii] emitters, which present a deficit of systems near the cluster systemic velocity when compared to a virialized population (or a backsplash population). The spatial segregation of some redshifted and blueshifted groups strongly indicates that the accretion was recent. Throughout the cluster, the presence of [O ii] emitters is strongly suppressed in dense environments. Our analysis supports previous suggestions that dusty starburst galaxies arise at the expense of gas-rich spiral galaxies [i.e., the e(c) type; Dressler and coworkers]. In addition, we describe a fainter population comprised largely of dwarf galaxies (Martin and coworkers) and find an even stronger suppression of [O ii] emitters in high-density environments, indicative of more effective destruction by harassment and/or gas stripping. Comparison to previous morphological studies, limited to the cluster core, suggests that galaxy-galaxy interactions may trigger the starbursts. The high e(a) galaxy fraction in Abell 851 as compared to that in the field, however, suggests that some cluster-specific mechanism, likely related to the dynamical assembly of the cluster, also contributes to the high number of starbursts.

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

Cited by 22 publications

References 52 publications

Metal enrichment of the intra-cluster medium over a Hubble time for merging and relaxed galaxy clusters

Metal enrichment of the intra-cluster medium over a Hubble time for merging and relaxed galaxy clusters

The matter distribution inz~ 0.5 redshift clusters of galaxies

Infalling Faint [Oii] Emitters in Abell 851. II. Environment, Kinematics, and Star Formation History

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