Distribution of Si, Fe, and Ni in the Intracluster Medium of the Coma Cluster

Matsushita, Kyoko; Sato, Toshio; Sakuma, Eri; Sato, Kosuke

doi:10.1093/pasj/65.1.10

Cited by 14 publications

(21 citation statements)

References 72 publications

(148 reference statements)

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“…These profiles were obtained by first calculating the relative abundance profiles for the individual clusters and then taking the median. The observational data for Si/Fe are taken from observations of AWM7 (Sato et al 2008), Centaurus (Sakuma et al 2011), and Coma (Matsushita et al 2013). The observations of AWM7 and Centaurus also provided measurements of O/Fe.…”

Section: Median Silicon and Oxygen Profilesmentioning

confidence: 99%

Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations

Pearce

Kay

Barnes

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The abundance and distribution of metals in galaxy clusters contains valuable information about their chemical history and evolution. By looking at how metallicity evolves with redshift, it is possible to constrain the different metal production channels. We use the C-EAGLE clusters, a sample of 30 high resolution (mgas ≃ 1.8 × 106 M⊙) cluster zoom simulations, to investigate the redshift evolution of metallicity, with particular focus on the cluster outskirts. The early enrichment model, in which the majority of metals are produced in the core of cluster progenitors at high redshift, suggests that metals in cluster outskirts have not significantly evolved since z = 2. With the C-EAGLE sample, we find reasonable agreement with the early enrichment model as there is very little scatter in the metallicity abundance at large radius across the whole sample, out to at least z = 2. The exception is Fe for which the radial dependence of metallicity was found to evolve at low redshift as a result of being mainly produced by Type Ia supernovae, which are more likely to be formed at later times than core-collapse supernovae. We also found considerable redshift evolution of metal abundances in the cores of the C-EAGLE clusters which has not been seen in other simulations or observation based metallicity studies. Since we find this evolution to be driven by accretion of low metallicity gas, it suggests that the interaction between outflowing, AGN heated material and the surrounding gas is important for determining the core abundances in clusters.

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Section: Median Silicon and Oxygen Profilesmentioning

confidence: 99%

Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations

Pearce

Kay

Barnes

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Sato et al 2008;Sakuma et al 2011;Matsushita et al 2013a;Simionescu et al 2015;Mernier et al 2017, Mernier et al, subm., this issue). From the simulation side, recent results by Biffi et al (2017) show similarly flat abundance ratio profiles compared to X-ray data for the Coma, Centaurus and AWM7 galaxy clusters (Sato et al 2008;Sakuma et al 2011;Matsushita et al 2013a), with a mild increasing trend towards the center (see also Planelles et al 2014). These results are reported in Fig.…”

Section: Radial Metallicity Profilesmentioning

confidence: 99%

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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“…The Coma Cluster is thus an unrelaxed system. However, we will show that our model based on the hydrostatic equilibrium fits the data of the X-ray brightness profiles [32,33], the SZ effect profile from the Planck measurement [48], and the weak-lensing profile by Subaru observations [34]. In general, the assumption of hydrostatic equilibrium holds only at the intermediate region of clusters, because of the cooling of the gas at the innermost region and the environmental effects at the outermost region.…”

Section: Consistency Test With Newtonian Gravitymentioning

confidence: 80%

“…Dynamical states of the Coma Cluster would give a systematic difference between our results and temperature measurement. Our fitting results show that the temperature of the Coma Cluster is around 6.4 keV (see Table. 1), but this result seems lower than those of X-ray observations [32,33,40,41,[45][46][47], which estimate that the temperature of the Coma Cluster is around 8-9 keV. Comparing the mass-temperature scaling relation for a sample of relaxed clusters [68] with an X-ray temperature observation of the Coma Cluster [32,33], the observed temperature is higher that the temperature expected by the mass.…”

Section: Systematic Errorsmentioning

confidence: 90%

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Testing a generalized cubic Galileon gravity model with the Coma Cluster

Terukina

Yamamoto

Okabe

et al. 2015

J. Cosmol. Astropart. Phys.

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Abstract.We obtain a constraint on the parameters of a generalized cubic Galileon gravity model exhibiting the Vainshtein mechanism by using multi-wavelength observations of the Coma Cluster. The generalized cubic Galileon model is characterized by three parameters of the turning scale associated with the Vainshtein mechanism, and the amplitude of modifying a gravitational potential and a lensing potential. X-ray and Sunyaev-Zel'dovich (SZ) observations of the intra-cluster medium are sensitive to the gravitational potential, while the weak-lensing (WL) measurement is specified by the lensing potential. A joint fit of a complementary multi-wavelength dataset of X-ray, SZ and WL measurements enables us to simultaneously constrain these three parameters of the generalized cubic Galileon model for the first time. We also find a degeneracy between the cluster mass parameters and the gravitational modification parameters, which is influential in the limit of the weak screening of the fifth force.

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Distribution of Si, Fe, and Ni in the Intracluster Medium of the Coma Cluster

Cited by 14 publications

References 72 publications

Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations

Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations

Enrichment of the Hot Intracluster Medium: Numerical Simulations

Testing a generalized cubic Galileon gravity model with the Coma Cluster

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