Iron abundance distribution in the hot gas of merging galaxy clusters

Urdampilleta, I.; Mernier, F.; Kaastra, J. S.; Simionescu, A.; Plaa, J. de; Kara, Sinancan; Ercan, E. N.

doi:10.1051/0004-6361/201935452

Cited by 10 publications

(19 citation statements)

References 136 publications

(220 reference statements)

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“…Based on this value and using the self-similar quantities described in Appendix A of Arnaud et al (2010), we estimate r 500 = 0.81 Mpc = 7.82 (at this redshift) and T 500 = 3.14 keV. A3365 hosts one radio relic at the east (hereafter relic E) and one radio relic candidate at the west (hereafter, relic CW) discovered in the NVSS survey and observed by van Weeren et al (2011) with the VLA and WSRT at 1.4 GHz. As described by van Weeren et al ( 2011) relic E and relic CW have an angular extension of 5.5 or 560 kpc and 2.3 or 235 kpc, respectively, at this redshift (see Fig.…”

Section: Introductionmentioning

confidence: 88%

“…Next, we filter the soft-proton (SP) flares by building Good Time Interval (GTI) files. For this process we use the method detailed in Urdampilleta et al (2019) and extensively explained in Appendix A.1 of Mernier et al (2015). We identify and exclude the point sources in the complete FOV with a circular region of 10 radius (see Fig.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…In our spectral analysis of A3365, we assume that the observed spectra include the following components: optically thin thermal plasma emission from the ICM in collisional ionization equilibrium and the background consisting of the local hot bubble (LHB), the Milky Way halo (MWH), the cosmic X-ray background (CXB), the hard particle (HP) background, and residual soft-protons (SP). The models used for each of the background components are detailed in Urdampilleta et al (2019) and Mernier et al (2015). The estimation of the sky background components (LHB, MHW, and CXB) is obtained from a ROSAT observation of an offset annullus surrounding A3365, using the X-ray Background Tool 1 .…”

Section: Spectral Analysismentioning

confidence: 99%

“…All metal abundances are tied to the Fe abundance. We account for the effect of systematic uncertainties related to the ±10% variation in the normalization of the sky background and non X-ray background components (Mernier et al 2015;Urdampilleta et al 2019). The contribution of these systematic uncertainties is further included in our analysis and results.…”

Section: Spectral Analysismentioning

confidence: 99%

“…The study of the shock-relic connection and the relative radial distribution throughout the ICM serves to improve our understanding of the dynamical stage of the cluster, as well as the physics of cosmic ray acceleration. Moreover, a detailed spectral analysis along the merging axis, including a study of their metallicity distribution, can provide valuable information on the chemical evolution and dynamical history of the merged ICM (Urdampilleta et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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X-ray study of Abell 3365 with XMM-Newton

Urdampilleta

Simionescu

Kaastra

et al. 2021

A&A

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We present an X-ray spectral analysis using XMM-Newton/EPIC observations (∼100 ks) of the merging galaxy cluster Abell 3365 (z = 0.093). Previous radio observations suggested the presence of a peripheral elongated radio relic to the east and a smaller radio relic candidate to the west of the cluster center. We find evidence of temperature discontinuities at the location of both radio relics, indicating the presence of a shock with a Mach number of ℳ = 3.5 ± 0.6 towards the east and a second shock with ℳ = 3.9 ± 0.8 towards the west. We also identify a cold front at r ∼ 1.6′ from the X-ray emission peak. Based on the shock velocities, we estimate that the dynamical age of the main merger along the east-west direction is ∼0.6 Gyr. We find that the diffusive shock acceleration scenario from the thermal pool is consistent with the electron acceleration mechanism for both radio relics. In addition, we studied the distribution of the temperature, iron (Fe) abundance, and pseudo-entropy along the merging axis. Our results show that remnants of a metal-rich cool-core can partially or entirely survive after the merging activity. Finally, we find that the merger can displace the metal-rich and low entropy gas from the potential well towards the cold front, as has been suggested via numerical simulations.

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Section: Introductionmentioning

confidence: 88%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Spectral Analysismentioning

confidence: 99%

Section: Spectral Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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X-ray study of Abell 3365 with XMM-Newton

Urdampilleta

Simionescu

Kaastra

et al. 2021

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The chemical evolution of galaxy clusters: Dissecting the iron mass budget of the intracluster medium

Liu

Tozzi

Ettori

et al. 2020

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Aims. We study the chemical evolution of galaxy clusters by measuring the iron mass in the ICM after dissecting the abundance profiles into different components. Methods. We use Chandra archival observations of 186 morphologically regular clusters in the redshift range [0.04, 1.07]. For each cluster we compute the azimuthally-averaged iron abundance and gas density profiles. In particular, we aim at identifying a central peak in the iron distribution, associated with the central galaxy, and an approximately constant plateau reaching the largest observed radii, possibly associated with early enrichment occurred before and/or shortly after the virialization of the cluster. We are able to firmly identify the two components in the iron distribution in a significant fraction of the sample, simply relying on the fit of the iron abundance profile. From the abundance and ICM density profiles we compute the iron mass included in the iron peak and iron plateau, and the gas mass-weighted iron abundance of the ICM, out to an extraction radius of 0.4 r 500 and, extending the abundance profile as a constant, to r 500 . Results. We find that the iron plateau shows no evolution with redshift. On the other hand, we find marginal (< 2σ c.l.) decrease with redshift in the iron mass included in the iron peak rescaled by the gas mass. We measure that the fraction of iron peak mass is typically a few percent (∼ 1%) of the total iron mass within r 500 . Therefore, since the total iron mass budget is dominated by the plateau, we find consistently that the global gas mass-weighted iron abundance does not evolve significantly across our sample. We are also able to reproduce past claims of evolution in the global iron abundance, which turn out to be due to the use of cluster samples with different selection methods combined to the use of emission-weighted instead of gas mass-weighted abundance values. Finally, while the intrinsic scatter in the iron plateau mass is consistent with zero, the iron peak mass exhibits a large scatter, in line with the fact that the peak is produced after the virialization of the halo and depends on the formation history of the hosting cool core and the strength of the associated feedback processes. Conclusions. We conclude that only a spatially-resolved approach can resolve the issue of the iron abundance evolution in the ICM, reconciling the contradictory results obtained in the last ten years. Evolutionary effects below z ∼ 1 are marginally measurable with present-day data, while at z > 1 the constraints are severely limited by the poor knowledge of the high-z cluster population. The path towards a full and comprehensive chemical history of the ICM necessarily requires the use of high-angular resolution X-ray bolometers and a dramatic increase in the statistics of faint, extended X-ray sources.

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Iron in X-COP: Tracing enrichment in cluster outskirts with high accuracy abundance profiles

Ghizzardi

Molendi

Burg

et al. 2021

A&A

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We present the first metal abundance profiles for a representative sample of massive clusters. Our measurements extend to R500 and are corrected for a systematic error plaguing previous outskirt estimates. Our profiles flatten out at large radii, admittedly not a new result, however the radial range and representative nature of our sample extends its import well beyond previous findings. We find no evidence of segregation between cool-core and non-cool-core systems beyond ∼0.3 R500, implying that, as was found for thermodynamic properties, the physical state of the core does not affect global cluster properties. Our mean abundance within R500 shows a very modest scatter, < 15%, suggesting the enrichment process must be quite similar in all these massive systems. This is a new finding and has significant implications for feedback processes. Together with results from the thermodynamic properties presented in a previous X-COP paper, it affords a coherent picture in which feedback effects do not vary significantly from one system to another. By combining intra-cluster medium with stellar measurements we have found the amount of Fe diffused in the intra-cluster medium to be about ten times higher than that locked in stars. Although our estimates suggest, with some strength, that the measured iron mass in clusters is well in excess of the predicted one, systematic errors prevent us from making a definitive statement. Further advancements will only be possible when systematic uncertainties, principally those associated with stellar masses, both within and beyond R500, can be reduced.

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Iron abundance distribution in the hot gas of merging galaxy clusters

Cited by 10 publications

References 136 publications

X-ray study of Abell 3365 with XMM-Newton

X-ray study of Abell 3365 with XMM-Newton

The chemical evolution of galaxy clusters: Dissecting the iron mass budget of the intracluster medium

Iron in X-COP: Tracing enrichment in cluster outskirts with high accuracy abundance profiles

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