Iron Abundance in the Intracluster Medium at High Redshift

Tozzi, P.; Rosati, P.; Ettori, S.; Borgani, S.; Mainieri, V.; Norman, C.

doi:10.1086/376731

Cited by 121 publications

(180 citation statements)

References 60 publications

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“…If metals produced and stored in LBG halos by z = 2.3 end up in clusters, than the average metallicity of the intracluster medium is Z I C M = Ω sf h Z /Ω I C M = 0.31Z , having assumed (Fukugita, Hogan & Peebles 1998) Ω I C M = 0.0026h −1.5 70 . Not only is this number tantalizingly close to the observed value at z = 1.2 (Tozzi et al 2003), but we also predict that little evolution will be found in the ICM metallicity up to z ≈ 2 as essentially all the metals that could have escaped galaxies during cosmic evolution had already done so by this epoch.…”

Section: Discussionsupporting

confidence: 81%

Cosmic metal enrichment

Ferrara¹

2008

Proc. IAU

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Abstract. I review the present understanding of the process by which the universe has been enriched in the course of its history with heavy elements produced by stars and transported into the surrounding intergalactic medium. This process goes under the name of "cosmic metal enrichment" and presents some of the most challenging puzzles in present day physical cosmology. These are reviewed along with some proposed explanations that all together form a coherent working scenario.Keywords. (galaxies:) intergalactic medium, cosmology: theory, galaxies: high-redshift PreliminariesAfter the Big Bang the cosmic gas had a composition which was (virtually) free of heavy elements. Yet, every single parcel of gas that we can probe today with our most powerful telescopes shows the sign of considerable amounts of metals, up to the highest redshift. When these metals where first produced, by what sources, and how these atomic species traveled away from their production sites are among the most challenging puzzles in current cosmological scenarios.A very simple, and yet robust, estimate of the amount of metals present at the end of reionization can be made. This is based on the fact that the sources of heavy elements and photons with energy > 1 Ryd responsible for hydrogen reionization are massive stars. Hence, as we know that reionization was complete by redshift z = 6, we can compute the metallicity of the cosmic gas associated with the ionizing photons required to reionize the universe, in the hypothesis that such process has been powered by stellar radiation. Obviously, as different type of sources, as quasars and/or decaying/annihilating dark matter particles may have contributed, the result of this simple exercise is an upper limit to the amount of metals. However, many arguments suggest that stars are by far the most viable reionization source candidates. In this case, we find that the mean metallicity of the cosmic gas (in practice, the intergalactic medium [IGM] which contains most of the baryons) at z = 6 iswhere y is the mean supernova metal yield, ν is the number of supernovae per unit stellar mass formed, C ≈ 1 − 10 is the IGM clumping factor and η is the number of ionizing photons per baryon into stars. The above result has been derived for a Salpeter stellar IMF but the value of Z is only mildly dependent on such quantity. The main point is that metal production associated with cosmic reionization is already substantial and comparable with the value derived from QSO absorption line experiments at lower redshifts. The next question concerns the sources that predominantly produced the metals and photons. Current data from a number of different experiments including CMB polarization anisotropies, Lyα and Lyβ Gunn-Peterson tests, cosmic star formation history and 86 available at https://www.cambridge.org/core/terms. https://doi

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Section: Discussionsupporting

confidence: 81%

Cosmic metal enrichment

Ferrara¹

2008

Proc. IAU

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“…We note here that the values of L bol and T of RDCS 1252 are consistent with the local L À T relation measured by Markevitch (1998), and, when combined with all the other data available on distant clusters in the Chandra archive, suggest only a mild positive evolution of the L X -T relation (see discussion in Ettori et al 2003a and references therein). Our best-fit value of the metallicity, Z ¼ 0:36 þ0:12 À0:10 Z , lends further support to a lack of evolution of the ICM mean metallicity measured out to z ' 1.3 (see the analysis by Tozzi et al 2003, which did not include RDCS 1252).…”

Section: Discussionsupporting

confidence: 59%

“…In more distant and complex systems, such as putative protoclusters dominated by a powerful radio galaxy, Chandra deep pointings have only revealed nonthermal components in the diffuse plasma so far (Fabian et al 2003a;Scharf et al 2003). XMM-Newton observations of very distant clusters, although affected by source confusion in some circumstances, have the ability to collect a large number of photons, thus improving temperature determinations and allowing an estimate of the ICM metallicity (Hashimoto et al 2002;Tozzi et al 2003).…”

Section: Introductionmentioning

confidence: 99%

ChandraandXMM-NewtonObservations of RDCS 1252.9-2927, A Massive Cluster atz=1.24

et al. 2004

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We present deep Chandra and XMM-Newton observations of the galaxy cluster RDCS 1252.9À2927, which was selected from the ROSAT Deep Cluster Survey (RDCS) and confirmed by extensive spectroscopy with the Very Large Telescope at redshift z = 1.237. With the Chandra data, the X-ray emission from the intracluster medium is well resolved and traced out to 500 kpc, thus allowing a measurement of the physical properties of the gas with unprecedented accuracy at this redshift. We detect a clear 6.7 keV iron K line in the Chandra spectrum providing a redshift within 1% of the spectroscopic one. By augmenting our spectroscopic analysis with the XMM-Newton data (MOS detectors only), we significantly narrow down the 1 error bar to 10% for the temperature and 30% for the metallicity, with best-fit values kT ¼ 6:0 þ0:7 À0:5 keV, Z ¼ 0:36 þ0:12 À0:10 Z . On the likely hypothesis of hydrostatic equilibrium, we measure a total mass of M 500 ¼ ð1:9 AE 0:3Þ Â 10 14 h À1 70 M within R Á=500 ' 536 kpc. Overall, these observations imply that RDCS 1252.9À2927 is the most X-ray luminous and likely the most massive bona fide cluster discovered to date at z > 1. When combined with current samples of distant clusters, these data lend further support to a mild evolution of the cluster scaling relations, as well the metallicity of the intracluster gas. Inspection of the cluster mass function in the current cosmological concordance model (h, m , Ã ) = (0.7, 0.3, 0.7) and 8 = 0.7-0.8 shows that RDCS 1252.9À2927 is an M* cluster at z = 1.24, in keeping with number density expectations in the RDCS survey volume.

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“…We performed a spectral temperature fit in a signal-to-noise optimized aperture of 40 following the procedure described in Tozzi et al (2003). Applying the same general procedure as for XMM-Newton with the local background measured in an onchip region with 60 diameter, we obtain a best fitting Chandra core temperature of 5.40 +1.27 −0.94 keV with the abundance fixed at 0.3 Z .…”

Section: Chandramentioning

confidence: 99%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

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Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

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Iron Abundance in the Intracluster Medium at High Redshift

Cited by 121 publications

References 60 publications

Cosmic metal enrichment

Cosmic metal enrichment

ChandraandXMM-NewtonObservations of RDCS 1252.9-2927, A Massive Cluster atz=1.24

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

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