Inhomogeneous metal distribution in the intracluster medium

Lovisari, Lorenzo; Schindler, S.; Kapferer, W.

doi:10.1051/0004-6361/201015400

Cited by 34 publications

(62 citation statements)

References 57 publications

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“…Comparison of the measured average radial Si/Fe profile ( Fig. 5) with previous observations for galaxy groups (Rasmussen & Ponman 2007) and Virgo (Simionescu et al 2010(Simionescu et al , 2015, and with the AGN simulation set of Planelles et al (2014). contrary, this trend is consistent with the peaked O profiles found in, for example A S1101 (de Plaa et al 2006), A 3526 (Sanders & Fabian 2006a), Hydra A (Simionescu et al 2009), A 3112 (Bulbul et al 2012b), A 4059 (Mernier et al 2015), and 5 cool-core clusters Lovisari et al (2011).…”

Section: Radial Contribution Of Snia and Sncc Productssupporting

confidence: 88%

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Mernier

Plaa

Kaastra

et al. 2017

A&A

120

161

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The hot intra-cluster medium (ICM) permeating galaxy clusters and groups is not pristine, as it has been continuously enriched by metals synthesised in Type Ia (SNIa) and core-collapse (SNcc) supernovae since the major epoch of star formation (z 2-3). The cluster/group enrichment history and mechanisms responsible for releasing and mixing the metals can be probed via the radial distribution of SNIa and SNcc products within the ICM. In this paper, we use deep XMM-Newton/EPIC observations from a sample of 44 nearby cool-core galaxy clusters, groups, and ellipticals (CHEERS) to constrain the average radial O, Mg, Si, S, Ar, Ca, Fe, and Ni abundance profiles. The radial distributions of all these elements, averaged over a large sample for the first time, represent the best constrained profiles available currently. Specific attention is devoted to a proper modelling of the EPIC spectral components, and to other systematic uncertainties that may affect our results. We find an overall decrease of the Fe abundance with radius out to ∼0.9r 500 and ∼0.6r 500 for clusters and groups, respectively, in good agreement with predictions from the most recent hydrodynamical simulations. The average radial profiles of all the other elements (X) are also centrally peaked and, when rescaled to their average central X/Fe ratios, follow well the Fe profile out to at least ∼0.5r 500 . As predicted by recent simulations, we find that the relative contribution of SNIa (SNcc) to the total ICM enrichment is consistent with being uniform at all radii, both for clusters and groups using two sets of SNIa and SNcc yield models that reproduce the X/Fe abundance pattern in the core well. In addition to implying that the central metal peak is balanced between SNIa and SNcc, our results suggest that the enriching SNIa and SNcc products must share the same origin and that the delay between the bulk of the SNIa and SNcc explosions must be shorter than the timescale necessary to diffuse out the metals. Finally, we report an apparent abundance drop in the very core of 14 systems (∼32% of the sample). Possible origins of these drops are discussed.

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Section: Radial Contribution Of Snia and Sncc Productssupporting

confidence: 88%

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Mernier

Plaa

Kaastra

et al. 2017

A&A

120

161

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“…2, we present the iron and oxygen profiles. The measure of oxygen abundances might be problematic (although used in abundance analysis as in de Werner et al 2006;David et al 2011;Lovisari et al 2011;Bulbul et al 2012) because the spectrum of the Galactic warm-hot X-ray emitting gas also contains O VIII lines that cannot be separately detected with the spectral resolution of EPIC (e.g. de Plaa et al 2007) and also because the obtained value is sensitive to the choice of n H value.…”

Section: X-ray Results Of the Ngc 4325 Groupmentioning

confidence: 99%

“…This filament was also confirmed by the metallicity profile extracted in identical regions along and across this structure in the Chandra and XMM-Newton data. Possible reasons for not observing the feature in the temperature map are the difficulty in observing an anti-correlation between temperature and metallicity because of projection effects (as suggested in Lovisari et al 2011) and the fact that the gas thermalize faster than the mixing. In this way, metal inhomogeneities are observed for a longer time than temperature substructures.…”

Section: Discussionmentioning

confidence: 99%

A metal-rich elongated structure in the core of the group NGC 4325

Laganá

Lovisari

Martins

et al. 2014

A&A

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Aims. Based on XMM-Newton, Chandra, and optical DR10-SDSS data, we investigate the metal enrichment history of the group NGC 4325 (z = 0.026). To complete the analysis we used chemical evolution models and studied the optical spectrum of the central dominant galaxy through its stellar population analysis and emission line diagnostics to analyse its role in the metal enrichment of the intra-group medium. Methods. We used X-ray 2D spectrally resolved maps to resolve structure in temperature and metallicity. We also derived gas and total masses within r 2500 and r 500 assuming hydrostatic equilibrium and spherical symmetry. To perform stellar population analysis we applied the spectral fitting technique with STARLIGHT to the optical spectrum of the central galaxy. We simulated the chemical evolution of the central galaxy.Results. While the temperature, pseudo-pressure, and pseudo-entropy maps showed no inhomogeneities, the spatial distribution of the metallicity shows a filamentary structure in the core of this group, which is spatially correlated with the central galaxy, suggesting a connection between the two. The analysis of the optical spectrum of the central galaxy showed no contribution by any recent AGN activity. Using the star formation history as input to chemical evolution models, we predicted the iron and oxygen mass released by supernovae (SNe) winds in the central galaxy up to the present time.Conclusions. Comparing the predicted amount of mass released by the NGC 4325 galaxy to the ones derived through X-ray analysis we conclude that the winds from the central galaxy alone play a minor role in the IGM metal enrichment of this group inside r 2500 . The SNe winds are responsible for no more than 3% of it and of the iron mass and 21% of the oxygen mass enclosed within r 2500 . Our results suggest that oxygen has been produced in the early stages of the group formation, becoming well mixed and leading to an almost flat profile. Instead, the iron distribution is centrally peaked, indicating that this element is still being added to the IGM specifically in the core by the SNIa. A possible scenario to explain the elongated metal-rich structure in the core of the NGC 4325 is a past AGN activity, in which our results suggest an episode older than ∼10 7 −10 8 yrs and younger than 5 × 10 8 . Through the overall distribution of the galaxies, we found no signs of recent merger in the group centre that could explain the metal-rich structure.

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“…Moreover, gas temperature maps show that even at a given radius, a wide distribution of temperatures can exist (e.g., Reiprich et al 2004;Million & Allen 2009;Randall et al 2010;Lovisari et al 2011), possibly depending on dynamical state (e.g., Zhang et al 2009). Additionally, in cluster outskirts, emission from new matter infalling along filaments and possible cooler clumps might become more important (Fig.…”

Section: Ionization Equilibrium T X = Te?mentioning

confidence: 99%

Outskirts of Galaxy Clusters

et al. 2013

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Until recently, only about 10% of the total intracluster gas volume had been studied with high accuracy, leaving a vast region essentially unexplored. This is now changing and a wide area of hot gas physics and chemistry awaits discovery in galaxy cluster outskirts. Also, robust large-scale total mass profiles and maps are within reach. First observational and theoretical results in this emerging field have been achieved in recent years with sometimes surprising findings. Here, we summarize and illustrate the relevant underlying physical and chemical processes and review the recent progress in X-ray, Sunyaev-Zel'dovich, and weak gravitational lensing observations of cluster outskirts, including also brief discussions of technical challenges and possible future improvements.Keywords Galaxy clusters · large-scale structure of the Universe · intracluster matter

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Inhomogeneous metal distribution in the intracluster medium

Cited by 34 publications

References 57 publications

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

A metal-rich elongated structure in the core of the group NGC 4325

Outskirts of Galaxy Clusters

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