Metal-Mass-to-Light Ratios of the Perseus Cluster Out to the Virial Radius

Matsushita, Kyoko; Sakuma, Eri; Sasaki, Toru; Sato, Kosuke; Simionescu, A.

doi:10.1088/0004-637x/764/2/147

Cited by 26 publications

(32 citation statements)

References 61 publications

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“…However, simulations based on stellar feedback only typically produce central cluster galaxies that are bluer and more star forming than observed. A recent investigation by Martizzi et al (2016), including both stellar and AGN feedback, also showed metallicity gradients in clusters simulated with an AMR code that are fairly consistent with the observational data by Leccardi and Molendi (2008) and Matsushita et al (2013b), despite a disagreement in the normalization. A flatter shape towards the outskirts is also recovered, when the emission-weighted metallicities are computed.…”

Section: Radial Metallicity Profilessupporting

confidence: 73%

Enrichment of the Hot Intracluster Medium: Numerical Simulations

2018

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The distribution of chemical elements in the hot intracluster medium (ICM) retains valuable information about the enrichment and star formation histories of galaxy clusters, and on the feedback and dynamical processes driving the evolution of the cosmic baryons. In the present study we review the progresses made so far in the modelling of the ICM chemical enrichment in a cosmological context, focusing in particular on cosmological hydrodynamical simulations. We will review the key aspects of embedding chemical evolution models into hydrodynamical simulations, with special attention to the crucial assumptions on the initial stellar mass function, stellar lifetimes and metal yields, and to the numerical limitations of the modelling. At a second stage, we will overview the main simulation results obtained in the last decades and compare them to X-ray observations of the ICM enrichment patterns. In particular, we will discuss how state-of-the-art simulations are able to reproduce the observed radial distribution of metals in the ICM, from the core to the outskirts, the chemical diversity depending on cluster thermo-dynamical properties, the evolution of ICM metallicity and its dependency on the system mass

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Section: Radial Metallicity Profilessupporting

confidence: 73%

Enrichment of the Hot Intracluster Medium: Numerical Simulations

2018

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“…We argue above that the fact that metallicity dispersion as a function of cluster mass is not observed to change in the outer regions, while it does vary in inner regions can be explained if, outside the cluster core, most of the metals are the result of pre-enrichment, which is the metallicity level set before cluster formation (e.g. Fujita et al 2008;Matsushita et al 2013;Werner et al 2013). The pre-enriched gas would have an approximately universal metallicity level, compared to the cold infalling haloes contributing metals at later times, whose gas metallicity values are more diverse.…”

Section: Support For Pre-enrichment?mentioning

confidence: 95%

Are the Effects of Structure Formation Seen in the Central Metallicity of Galaxy Clusters?

Elkholy¹,

Bautz²,

Canizares³

2015

ApJ

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A sample of 46 nearby clusters observed with Chandra is analyzed to produce radial density, temperature, entropy and metallicity profiles, as well as other morphological measurements. The entropy profiles are computed to larger radial extents than in previous Chandra cluster sample analyses. We find that the iron mass fraction measured in the inner 0.15R 500 shows a larger dispersion across the sample of low-mass clusters, than it does for the sample of high-mass clusters. We interpret this finding as the result of the mixing of more haloes in large clusters than in small clusters, which leads to an averaging of the metal content in the large clusters, and thus less dispersion of metallicity for high-mass clusters. This interpretation lends support to the idea that the low-entropy, metal-rich gas of merging haloes reaches clusters' centers, which explains observations of Core-Collapse Supernova products metallicity peaks, and which is seen in hydrodynamical simulations. The gas in these merging haloes would have to reach the centers of clusters without mixing in the outer regions, in order to support our interpretation. On the other hand, metallicity dispersion does not change with mass in the outer regions of clusters, suggesting that most of the outer metals come from a source with a more uniform metallicity level, such as during pre-enrichment. We also measure a correlation between the metal content in low-mass clusters and the degree to which their Intra-Cluster Medium (ICM) is morphologically disturbed, as measured by centroid shift. This suggests an alternative interpretation of the large width of the metallicity distribution in low-mass clusters, whereby a metallicity boost in the center of low-mass clusters is induced as a transitional state, during mergers.

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“…Since enrichment of the ICM at late times by ram-pressure stripping or galactic outflows generically predicts a non-uniform metal distribution over this radial range (e.g. Gunn & Gott 1972;Domainko et al 2006;Matsushita et al 2013), and since large-scale mixing is prohibited by the steep entropy gradients in clusters, these observations have been taken as evidence that most of the metals in the ICM are produced prior to cluster formation. In this scenario, metals would need to be expelled from galaxies and mixed throughout the intergalactic medium in the protocluster environment; once accreted onto a cluster and virialized, significant further enrichment of the ICM can only occur in regions where the stellar density is relatively high (cluster cores).…”

Section: The History Of Icm Enrichmentmentioning

confidence: 99%

The metallicity of the intracluster medium over cosmic time: further evidence for early enrichment

Mantz

Allen

Morris

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use Chandra X-ray data to measure the metallicity of the intracluster medium (ICM) in 245 massive galaxy clusters selected from X-ray and Sunyaev-Zel'dovich (SZ) effect surveys, spanning redshifts 0 < z < 1.2. Metallicities were measured in three different radial ranges, spanning cluster cores through their outskirts. We explore trends in these measurements as a function of cluster redshift, temperature, and surface brightness "peakiness" (a proxy for gas cooling efficiency in cluster centers). The data at large radii (0.5-1 r 500 ) are consistent with a constant metallicity, while at intermediate radii (0.1-0.5 r 500 ) we see a late-time increase in enrichment, consistent with the expected production and mixing of metals in cluster cores. In cluster centers, there are strong trends of metallicity with temperature and peakiness, reflecting enhanced metal production in the lowest-entropy gas. Within the cool-core/sharply peaked cluster population, there is a large intrinsic scatter in central metallicity and no overall evolution, indicating significant astrophysical variations in the efficiency of enrichment. The central metallicity in clusters with flat surface brightness profiles is lower, with a smaller intrinsic scatter, but increases towards lower redshifts. Our results are consistent with other recent measurements of ICM metallicity as a function of redshift. They reinforce the picture implied by observations of uniform metal distributions in the outskirts of nearby clusters, in which most of the enrichment of the ICM takes place before cluster formation, with significant later enrichment taking place only in cluster centers, as the stellar populations of the central galaxies evolve.

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Metal-Mass-to-Light Ratios of the Perseus Cluster Out to the Virial Radius

Cited by 26 publications

References 61 publications

Enrichment of the Hot Intracluster Medium: Numerical Simulations

Enrichment of the Hot Intracluster Medium: Numerical Simulations

Are the Effects of Structure Formation Seen in the Central Metallicity of Galaxy Clusters?

The metallicity of the intracluster medium over cosmic time: further evidence for early enrichment

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