Iron Abundance Profiles of 12 Clusters of Galaxies Observed with<i>BeppoSAX</i>

Irwin, Jimmy A.; Bregman, Joel N.

doi:10.1086/318240

Cited by 32 publications

(33 citation statements)

References 35 publications

(48 reference statements)

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“…Gradients in the iron abundance have been detected with ASCA data (Finoguenov et al 2000(Finoguenov et al , 2001White 2000), and confirmed by BeppoSax data (Irwin & Bregman 2001;De Grandi & Molendi 2001); in particular, sharp metallicity peaks in the central region seem to be typical of cooling flows/cD clusters (Fukazawa et al 2000;Irwin & Bregman 2001;De Grandi & Molendi 2001). [α/Fe] ratios also seem to display a composite behaviour, increasing with cluster radius from ∼solar in the central regions to supersolar, typical type II supernova (SN), values in the outer regions (Finoguenov et al 2000).…”

Section: Introductionmentioning

confidence: 59%

“…Metallicities are in fact typically measured at most within half of the virial radius (Finoguenov et al 2000(Finoguenov et al , 2001De Grandi & Molendi 2001;Irwin & Bregman 2001); measurements hardly reach r 500 , which is typically 63% of r 200 , and in terms of cluster mass M 500 ∼ 0.63 M 200 as well (see Reiprich & Böhringer 2002) 1 . For the sake of the chemical enrichment what matters is the mass averaged metallicity, obtained by convolving metallicity distributions with gas profiles within the same radius, and the IMLR should also be evaluated from the gas, metals and galactic luminosity within the same radius (as in Finoguenov et al 2000Finoguenov et al , 2001Finoguenov et al , 2003.…”

Section: M/l Ratio and Imlr Of Galaxies: Pnj Vs Salpetermentioning

confidence: 99%

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Chemical evolution of the intra-cluster medium

Moretti¹,

Portinari²,

Chiosi³

2003

A&A

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Abstract. The high metallicity of the intra-cluster medium (ICM) is generally interpreted on the basis of the galactic wind scenario for elliptical galaxies. In this framework, we develop a toy model to follow the chemical evolution of the ICM, formulated in analogy to chemical models for individual galaxies. The model computes the galaxy formation history (GFH) of cluster galaxies, connecting the final luminosity function (LF) to the corresponding metal enrichment history of the ICM. The observed LF can be reproduced with a smooth, Madau-plot like GFH peaking at z ∼ 1−2, plus a "burst" of formation of dwarf galaxies at high redshift. The model is used to test the response of the predicted metal content and abundance evolution of the ICM to varying input galactic models. The chemical enrichment is computed from "galactic yields" based on models of elliptical galaxies with a variable initial mass function (IMF), favouring the formation of massive stars at high redshift and/or in more massive galaxies. For a given final galactic luminosity, these model ellipticals eject into the ICM a larger quantity of gas and of metals than do standard models based on the Salpeter IMF. However, a scenario in which the IMF varies with redshift as a consequence of the effect of the cosmic background temperature on the Jeans mass scale appears to be too mild to account for the observed metal production in clusters. The high iron-massto-luminosity-ratio of the ICM can be reproduced only by assuming a more dramatic variation of the typical stellar mass, in line with other recent findings. The mass in the wind-ejected gas is predicted to exceed the mass in galaxies by a factor of 1.5-2 and to constitute roughly half of the intra-cluster gas.

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Section: Introductionmentioning

confidence: 59%

Section: M/l Ratio and Imlr Of Galaxies: Pnj Vs Salpetermentioning

confidence: 99%

Chemical evolution of the intra-cluster medium

Moretti¹,

Portinari²,

Chiosi³

2003

A&A

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“…Future X-ray Tozzi et al (2003). For comparison, the low redshift samples from Mushotzky & Loewenstein (1997), and Irwin & Bregman (2001) are also plotted.…”

Section: Dynamical State Of the Clustermentioning

confidence: 99%

Abundance constraints and direct redshift measurement of the diffuse X-ray emission from a distant cluster of galaxies

Hashimoto

Barcons

Böhringer

et al. 2004

A&A

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Abstract. We report on the XMM-Newton (XMM) observation of RX J1053.7+5735, one of the most distant X-ray selected clusters of galaxies, which also shows an unusual double-lobed X-ray morphology, indicative of a possible equal-mass cluster merger. The cluster was discovered during the ROSAT deep pointings in the direction of the Lockman Hole. All XMM Lockman Hole observations (PV, AO-1 & AO-2 phases) with the European Photon Imaging Camera (EPIC) were combined for the analysis, totaling exposure times ∼648 ks, 738 ks, and 758 ks for pn, MOS1, and MOS2, respectively. With this "deep" dataset, we could detect the Fe K line and obtain a strong constraint on cluster metallicity, which is difficult to achieve for clusters at z > 1. The best-fit abundance is 0.46−0.07 times the solar value. The Fe line emission also allows us to directly estimate the redshift of diffuse gas, with a value z = 1.14 +0.01 −0.01 . This is one of the first clusters whose X-ray redshift is directly measured prior to the secure knowledge of cluster redshift by optical/NIR spectroscopy. We could also estimate the X-ray redshift separately for each of the two lobes in the double-lobed structure, and the result is consistent with the two lobes being part of one cluster system at the same redshift. Comparison with other metallicity measurements of nearby and distant clusters shows that there is little evolution in the ICM metallicity from z ∼ 1 to the present.

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“…Gas dynamic stripping may be related to the chemical enrichment of the ICM, and possibly also its dynamics (Deiss & Just 1996). A preliminary conclusion from the analysis of X‐ray spectra of the ICM is that the metal abundances in the ICM vary from one type of cluster to another, and that the distribution of metals within clusters, especially ‘cooling flow’ clusters, can be non‐uniform (Finoguenov, David & Ponman 1999; Irwin & Bregman 2001; De Grandi & Molendi 2001). This suggests that both winds (mainly responsible for [Si] enrichment) and galaxy stripping (resulting mainly in [Fe] enrichment) contribute to the chemical enrichment of the ICM to variable extents, possibly according to the structure of the cluster and the age of the brightest cluster galaxies.…”

Section: Introductionmentioning

confidence: 99%

Gas dynamic stripping and X-ray emission of cluster elliptical galaxies

Toniazzo

Schindler

2001

Monthly Notices of the Royal Astronomical Society

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Detailed three‐dimensional numerical simulations of an elliptical galaxy orbiting in a gas‐rich cluster of galaxies indicate that gas dynamic stripping is less efficient than the results from previous, simpler calculations by Takeda et al. and Gaetz et al. implied. This result is consistent with X‐ray data for cluster elliptical galaxies. Hydrodynamic torques and direct accretion of orbital angular momentum can result in the formation of a cold gaseous disc, even in a non‐rotating galaxy. The gas lost by cluster galaxies via the process of gas dynamic stripping tends to produce a colder, chemically enriched cluster gas core. A comparison of the models with the available X‐ray data of cluster galaxies shows that the X‐ray luminosity distribution of cluster galaxies may reflect hydrodynamic stripping, but also that a purely hydrodynamic treatment is inadequate for the cooler interstellar medium near the centre of the galaxy.

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Iron Abundance Profiles of 12 Clusters of Galaxies Observed withBeppoSAX

Cited by 32 publications

References 35 publications

Chemical evolution of the intra-cluster medium

Chemical evolution of the intra-cluster medium

Abundance constraints and direct redshift measurement of the diffuse X-ray emission from a distant cluster of galaxies

Gas dynamic stripping and X-ray emission of cluster elliptical galaxies

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