Enrichment of the Hot Intracluster Medium: Numerical Simulations

Biffi, V.; Mernier, F.; Медведев, П. С.

doi:10.1007/s11214-018-0557-7

Cited by 54 publications

(47 citation statements)

References 140 publications

(225 reference statements)

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“…Therefore, we choose to include both the CHEERS dataset and that of Yates et al (2017) in this highertemperature regime. For a more detailed investigation into the differences these two improvements make to the modelling of the ICM metallicity in L-galaxies, see our followup paper, Yates et al, in prep. Our analysis of the iron abundance of the intragroup and intracluster medium within r 500 suggests that the mean Z Fe varies little with temperature over around 2 orders of magnitude in gravitating mass (see also Biffi et al 2018;Mernier et al 2018a). We also find an increasing scatter around in Z Fe with decreasing temperature in the model.…”

Section: Metal Content In the Icmmentioning

confidence: 54%

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Henriques

Yates

et al. 2019

Monthly Notices of the Royal Astronomical Society

103

112

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We have updated the Munich galaxy formation model, L-galaxies, to follow the radial distributions of stars and atomic and molecular gas in galaxy discs. We include an H 2 -based star-formation law, as well as a detailed chemical-enrichment model with explicit mass-dependent delay times for SN-II, SN-Ia and AGB stars. Information about the star formation, feedback and chemical-enrichment histories of discs is stored in 12 concentric rings. The new model retains the success of its predecessor in reproducing the observed evolution of the galaxy population, in particular, stellar mass functions and passive fractions over the redshift range 0 z 3 and mass range 8 log(M * / M ) 12, the black hole-bulge mass relation at z = 0, galaxy morphology as a function of stellar mass and the mass-metallicity relations of both stellar and gas components. In addition, its detailed modelling of the radial structure of discs allows qualitatively new comparisons with observation, most notably with the relative sizes and masses of the stellar, atomic and molecular components in discs. Good agreement is found with recent data. Comparison of results obtained for simulations differing in mass resolution by more than two orders of magnitude shows that all important distributions are numerically well converged even for this more detailed model. An examination of metallicity and surface-density gradients in the stars and gas indicates that our new model, with star formation, chemical enrichment and feedback calculated self-consistently on local disc scales, reproduces some but not all of the trends seen in recent many-galaxy IFU surveys.

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Section: Metal Content In the Icmmentioning

confidence: 54%

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Henriques

Yates

et al. 2019

Monthly Notices of the Royal Astronomical Society

103

112

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“…In fact, the presence of emission lines in the X‐ray spectra of the hot (10 6 –10 8 K), highly ionized atmospheres surrounding the most massive galaxies and pervading galaxy groups and clusters is the smoking gun evidence that chemical enrichment is at play even within these large‐scale structures (Lea et al ; Mitchell et al ). The presence of metals in the intracluster medium (ICM) naturally poses several fundamental questions (for recent reviews, see Biffi et al ; Mernier et al ): for example, when (and how) did the ICM get enriched? The key to answer this question resides in the overall evolution of the ICM metallicity with cosmic time.…”

Section: Metals In the Intracluster Mediummentioning

confidence: 99%

How do atomic code uncertainties affect abundance measurements in the intracluster medium?

et al. 2020

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Accurate chemical abundance measurements of X‐ray‐emitting atmospheres pervading massive galaxies, galaxy groups, and clusters provide essential information on the star formation and chemical enrichment histories of these large‐scale structures. Although the collisionally ionized nature of the intracluster medium (ICM) makes these abundance measurements relatively easy, the underlying spectral models can rely on different atomic codes, which brings additional uncertainties on the inferred abundances. Here we provide a simple, yet comprehensive comparison between the codes SPEXACT v3.0.5 (cie model) and AtomDB v3.0.9 (vapec model) in the case of moderate, charged‐coupled device‐like resolution spectroscopy. We show that in cool plasmas (kT ≲ 2 keV), systematic differences up to ∼20% for the Fe abundance and ∼45% for the O/Fe, Mg/Fe, Si/Fe, and S/Fe ratios may still occur. Importantly, these discrepancies are also found to be instrument‐dependent, at least for the absolute Fe abundance. Future improvements in these two codes will be necessary to better address questions on ICM enrichment.

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“…Besides the three distinct and independent sources of enrichment considered here -AGB, SN cc , or SN Ia , we also assume that the bulk of the enrichment is completed at z = 0.1 and does not differ from local clusters, which is a fair hypothesis supported by numerical and observational results (e.g. Ettori et al 2015;McDonald et al 2016;Biffi et al 2017Biffi et al , 2018bUrban et al 2017;Mantz et al 2017;Liu et al 2020). Section 3.4 further extends the comparison to the case of z = 1 clusters.…”

Section: Constraining Chemical Enrichment Models With the X-ifumentioning

confidence: 94%

“…Measurements through X-ray spectroscopy of the intracluster medium (ICM) performed by missions such as XMM-Newton, Chandra, or Suzaku provide outstanding results in recovering the chemical composition of the ICM and in probing the enrichment of the largest scales of the Universe (for recent reviews, see Werner et al 2008;Mernier et al 2018a). In fact, the investigation of radial metallicity profiles in the outskirts of these systems (Werner et al 2013;Urban et al 2017) highlighted strong evidence of an early metal-production scenario (z > 2-3), which predates the formation of clusters (Fabjan et al 2010;McCarthy et al 2010;Biffi et al 2017Biffi et al , 2018a, for a review on metallicity profiles in numerical simulations, see Biffi et al 2018b) and is likely contemporary to the stelliferous epoch of the Universe (Madau & Dickinson 2014). Although active galactic nucleus (AGN) feedback of the dominant galaxy can in principle induce significant central metallicity variations as a function of outflow and/or jet events (e.g.…”

Section: Introductionmentioning

confidence: 99%

Constraining the origin and models of chemical enrichment in galaxy clusters using theAthenaX-IFU

Mernier

Cucchetti

Tornatore

et al. 2020

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Chemical enrichment of the Universe at all scales is related to stellar winds and explosive supernovae phenomena. Metals produced by stars and later spread throughout the intracluster medium (ICM) at the megaparsec scale become a fossil record of the chemical enrichment of the Universe and of the dynamical and feedback mechanisms determining their circulation. As demonstrated by the results of the soft X-ray spectrometer onboard Hitomi, high-resolution X-ray spectroscopy is the path to differentiating among the models that consider different metal-production mechanisms, predict the outcoming yields, and are a function of the nature, mass, and/or initial metallicity of their stellar progenitor. Transformational results shall be achieved through improvements in the energy resolution and effective area of X-ray observatories, allowing them to detect rarer metals (e.g. Na, Al) and constrain yet-uncertain abundances (e.g. C, Ne, Ca, Ni). The X-ray Integral Field Unit (X-IFU) instrument onboard the next-generation European X-ray observatory Athena is expected to deliver such breakthroughs. Starting from 100 ks of synthetic observations of 12 abundance ratios in the ICM of four simulated clusters, we demonstrate that the X-IFU will be capable of recovering the input chemical enrichment models at both low (z = 0.1) and high (z = 1) redshifts, while statistically excluding more than 99.5% of all the other tested combinations of models. By fixing the enrichment models which provide the best fit to the simulated data, we also show that the X-IFU will constrain the slope of the stellar initial mass function within ∼12%. These constraints will be key ingredients in our understanding of the chemical enrichment of the Universe and its evolution.

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Enrichment of the Hot Intracluster Medium: Numerical Simulations

Cited by 54 publications

References 140 publications

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

How do atomic code uncertainties affect abundance measurements in the intracluster medium?

Constraining the origin and models of chemical enrichment in galaxy clusters using theAthenaX-IFU

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