Metal Enrichment Processes

Schindler, S.; Diaferio, Antonaldo

doi:10.1007/s11214-008-9321-8

Cited by 74 publications

(62 citation statements)

References 161 publications

(162 reference statements)

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“…Several processes have been proposed to explain the observed enrichment in the ICM: ram-pressure stripping (Gunn & Gott 1972), galactic winds (De Young 1978), galaxy-galaxy interactions (Gnedin 1998), AGN outflows (De Young 1986;Hasinger et al 2002), intracluster supernovae (Gerhard et al 2002), and others. Simulations show an inhomogeneous distribution of the metals independent of the enrichment processes (Kapferer et al 2006;Schindler & Diaferio 2008). Although both AGN outflows and galaxy-galaxy interactions can add metals to the ICM (Kapferer et al 2005;Heath et al 2007), simulations suggest that the metal enrichment of the ICM is caused primarily by galactic winds and ram-pressure stripping.…”

Section: Introductionmentioning

confidence: 93%

Inhomogeneous metal distribution in the intracluster medium

Lovisari

Schindler

Kapferer

2011

A&A

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Context. The hot gas that fills the space between galaxies in clusters is rich in metals. In their large potential wells, galaxy clusters accumulate metals over the whole cluster history and hence retain important information on cluster formation and evolution. Aims. We use a sample of five cool core clusters to study the distribution of metals in the ICM. We investigate whether the X-ray observations yield good estimates for the metal mass and whether the heavy elements abundances are consistent with a certain relative fraction of SN Ia to SNCC. Methods. We derived detailed metallicity maps of the clusters from XMM-Newton observations and used them as a measure for the metal mass in the ICM. We determined radial profiles for several elements, and using population synthesis and chemical enrichment models, we studied the agreement between the measured abundances and the theoretical yields. Results. We show that the distribution of metals show a lot of inhomogeneities even in relaxed clusters. Using metal maps usually gives a metal mass 10-30% higher than the metal mass computed using a single extraction region, so it is expected that most previous metal mass determination have underestimated metal mass. The abundance ratio of α-elements to Fe, even in the central parts of clusters, are consistent with an enrichment thanks to the combination of SN Ia and SNCC.

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Section: Introductionmentioning

confidence: 93%

Inhomogeneous metal distribution in the intracluster medium

Lovisari

Schindler

Kapferer

2011

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“…the intracluster medium, ICM) is enriched with metals ejected form supernovae (SNe) explosions through subsequent episodes of star formation and subsequent diffusion through several mechanisms, e.g., ram pressure stripping, galactic winds, outflows from active Galactic nuclei, galaxy-galaxy interactions (e.g. Renzini 1997;Schindler & Diaferio 2008).…”

Section: Introductionmentioning

confidence: 99%

The evolution of the spatially resolved metal abundance in galaxy clusters up toz= 1.4

Ettori

Baldi

Balestra

et al. 2015

A&A

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Context. We present the combined analysis of the metal content of 83 objects in the redshift range 0.09−1.39, and spatially resolved in the three bins (0−0.15, 0.15−0.4, >0.4) R 500 , as obtained with similar analysis using XMM-Newton data in our previous two papers. Aims. By combining these two large data sets, we investigate the relations between abundance, temperature, radial position and redshift holding in the intracluster medium. Methods. We fit functional forms to the combination of the different physical quantities of interest, i.e., intracluster medium (ICM) metal abundance, radius, and redshift. We use the pseudo-entropy ratio to separate the cool core (CC) cluster population, where the central gas density tends to be relatively higher, cooler and more metal rich, from the non-cool core systems. Results. The average, redshift-independent, metal abundance measured in the three radial bins decreases moving outwards, with a mean metallicity in the core that is even three (two) times higher than the value of 0.16 times the solar abundance in Anders & Grevesse (1989, Geochim. Cosmochim. Acta, 53, 197) estimated at r > 0.4 R 500 in CC (NCC) objects. We find that the values of the emission-weighted metallicity are well fitted by the relation Z(z) = Z 0 (1 + z) −γ at the given radius. A significant scatter, intrinsic to the observed distribution and of the order of 0.05−0.15, is observed below 0.4 R 500 . The nominal best-fit value of γ is significantly different from zero (>3σ) in the inner cluster regions (γ = 1.6 ± 0.2) and in CC clusters only. These results are also confirmed with a bootstrap analysis, which provides a still significant negative evolution in the core of CC systems (P > 99.9 per cent, when counting the number of random repetitions, which yields γ > 0). No redshift evolution is observed when regions above the core (r > 0.15 R 500 ) are considered. A reasonable good fit of both the radial and redshift dependence is provided from the functional form Z(r, z) = Z 0 (1 + (r/0.15 R 500 ) 2 ) −β (1 + z) −γ , with (Z 0 , β, γ) = (0.83 ± 0.13, 0.55 ± 0.07, 1.7 ± 0.6) in CC clusters and (0.39 ± 0.04, 0.37 ± 0.15, 0.5 ± 0.5) for NCC systems. Conclusions. Our results represent the most extensive study of the spatially resolved metal distribution in the cluster plasma as function of redshift. Our study defines the limits that numerical and analytic models describing the metal enrichment in the ICM have to meet.

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“…An overview of these mechanisms is given by Schindler & Diaferio (2008). Simulations suggest that the gas is mainly enriched by galactic winds, which are powered by core-collapse supernovae at early stages of the evolution.…”

Section: Introductionmentioning

confidence: 99%

The metal contents of two groups of galaxies

Grange

Plaa

Kaastra

et al. 2011

A&A

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Context. The hot gas in clusters and groups of galaxies is continuously being enriched with metals from supernovae and stars. It is well established that the enrichment of the gas with elements from oxygen to iron is mainly caused by supernova explosions. The origins of nitrogen and carbon are still being debated. Possible candidates include massive, metal-rich stars, early generations of massive stars, intermediate-or low-mass stars and asymptotic giant branch (AGB) stars. Aims. In this paper we accurately determine the metal abundances of the gas in the groups of galaxies NGC 5044 and NGC 5813, and discuss the nature of the objects that create these metals. We mainly focus on carbon and nitrogen. Methods. We use spatially-resolved high-resolution X-ray spectroscopy from XMM-Newton. For the spectral fitting, multitemperature hot gas models are used. Results. The abundance ratios of carbon over oxygen and nitrogen over oxygen that we find are high compared to the ratios in the stars in the disk of our Galaxy. The oxygen and nitrogen abundances we derive are similar to what has been found in earlier work on other giant ellipticals in comparable environments. We show that the iron abundances in both our sources have a gradient along the cross-dispersion direction of the reflection grating spectrometer (RGS). Conclusions. We conclude that it is unlikely that the creation of nitrogen and carbon takes place in massive stars, which end their lives as core-collapse supernovae, enriching the medium with oxygen because oxygen should then also be enhanced. Therefore we favour low-and intermediate-mass stars as sources of these elements. The abundances in the hot gas can be explained best by a 30-40% contribution of type Ia supernovae based on the measured oxygen and iron abundances and under the assumption of a Salpeter initial mass function (IMF).

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Metal Enrichment Processes

Cited by 74 publications

References 161 publications

Inhomogeneous metal distribution in the intracluster medium

Inhomogeneous metal distribution in the intracluster medium

The evolution of the spatially resolved metal abundance in galaxy clusters up toz= 1.4

The metal contents of two groups of galaxies

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