Measurement of the Elemental Abundances in Four Rich Clusters of Galaxies. I. Observations

Mushotzky, R. F.; Loewenstein, M.; Arnaud, K. A.; Tamura, Takayuki; Fukazawa, Yasushi; Matsushita, Kyoko; Kikuchi, K.; Hatsukade, Isamu

doi:10.1086/177541

Cited by 187 publications

(217 citation statements)

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“…The results presented in Table 4 are somewhat in disagreement with those found by Mushotzky et al (1996) (see also using ASCA-SIS data for four rich clusters of galaxies (A496, A1060, A2199 and AWM7). Although we also find an overabundance of Si, our abundance rates for S, Ar and Ca relative to iron are higher than theirs.…”

Section: Metallicitycontrasting

confidence: 48%

BeppoSAX observation of the rich cluster of galaxies Abell 85

Neto¹,

Pislar²

2001

A&A

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Abstract.We report the observation of the Intra-Cluster Medium (ICM) of Abell 85 by the X-ray satellite BeppoSAX. We have analysed both the spectrum obtained in the central 8 arcmin circular region centred on the Very Steep Spectrum Radio Source (VSSRS) and the spectra from a number of sub-regions. Analysis of the spectra allowed us to independently obtain new estimates of the temperature, metallicity and line-of-sight hydrogen density column, both globally (T = 6.6 ± 0.3 keV, Z = 0.38 ± 0.06 Z and NH = 5.5 +0.9 −0.7 10 20 cm −2 ) and locally. These measures are in good agreement with previous measures based on ROSAT and ASCA data. In the region of the VSRSS, we attempted to discriminate between thermal and non-thermal X-ray emission. Although we could not do this unambiguously, we have nonetheless estimated the extended magnetic field using the radio spectrum available for this region. We obtain a lower limit intensity of 0.9 µG, consistent with our previous estimate. We also derive α-elements/iron abundance ratios that turn out to be higher than 1. Such a result tends to support the burst model for elliptical galaxies, where a strong galactic wind develops early in the galaxy history and type II supernovae (SN) may be the major contributors to the enrichment of the ICM. A two-temperature ICM model was fitted in the central region, yielding a main component with roughly the mean cluster temperature and a cooler component with temperature less than 0.1 keV.

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Section: Metallicitycontrasting

confidence: 48%

BeppoSAX observation of the rich cluster of galaxies Abell 85

Neto¹,

Pislar²

2001

A&A

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“…Mushotzky et al 1996;Fukazawa et al 1998) clearly indicates that the ICM contains a processed component, likely the result of galactic winds, stripping of the interstellar medium (ISM) of cluster members by ram pressure, or tidally removed ISM during merging with other galaxy groups. These processes also add dust to the ICM, which in turn is a possible candidate for the excess X-ray absorber.…”

Section: Introductionmentioning

confidence: 99%

Far-infrared emission from intracluster dust in Abell clusters

Stickel

Klaas

Lemke

et al. 2002

A&A

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Abstract. The ISOPHOT instrument aboard ISO has been used to observe extended FIR emission of six Abell clusters. Strip scanning measurements with crossing position angles centered on the clusters were carried out at 120 µm and 180 µm. The raw profiles of the I120 µm/I180 µm surface brightness ratio including zodiacal light show a bump towards Abell 1656 (Coma), dips towards Abell 262 and Abell 2670, and are without clear structure towards Abell 400, Abell 496, and Abell 4038. After subtraction of the zodiacal light, the bump towards Abell 1656 is still present, while the dips towards Abell 262 and Abell 2670 are no longer noticable. This indicates a localized excess of emitting material outside the Galaxy towards Abell 1656 with properties different from the galactic foreground cirrus, while the behavior in Abell 262 and Abell 2670 can be reconciled with galactic cirrus structures localized on the line-of-sight to these clusters. The excess of ≈0.2 MJy/sr seen at 120 µm towards Abell 1656 (Coma) is interpreted as being due to thermal emission from intracluster dust distributed in the hot X-ray emitting intracluster medium. The integrated excess flux within the central region of 10 -15 diameter is ≈2.8 Jy. Since the dust temperature is poorly constrained, only a rough estimate of the associated dust mass of MD ≈ 10 7 M can be derived. The associated visual extinction is negligible (AV 0.1 mag) and much smaller than claimed from optical observations. No evidence is found for intracluster dust in the other five clusters observed. The absence of any signature for intracluster dust in five clusters and the rather low inferred dust mass in Abell 1656 indicates that intracluster dust is likely not responsible for the excess X-ray absorption seen in cooling flow clusters. These observations thereby represent a further unsuccessful attempt in detecting the presumed final stage of the cooling flow material, in accord with quite a number of previous studies in other wavelengths regions. Finally, the observed dimming of the high-redshift supernovae is unlikely be attributable to extinction caused by dust in the intracluster or even a presumed intercluster medium.

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“…Previously, since the stellar iron abundance of ellipticals was believed as high as f'J 2Z 0 , the iron yield was regarded to be enough high to enrich the ICM mainly by SNII. Moreover, it was reported that ASCA observations gave high values of [a/Fe] to ICM (Mushotzky et al 1996). These estimates seemed to support SNII enriched ICM.…”

Section: Introductionmentioning

confidence: 68%

“…2, the observed range of FeML cannot be explained only by galactic winds, unless IMF slope is as flat as x rv 0.9, which causes too high stellar abundances. But if the ICM was enriched by SNla as well as SNII, the FeML and the mass-metallicity relation can be explained consistently with the combinations of (Mushotzky et al 1996). However, this discussion is based on comparison with the solar-photospheric abundances.…”

Section: Mass-metallicity Relation Of Ellipticalsmentioning

confidence: 98%

Enrichment of Heavy Elements in Clusters of Galaxies

Ishimaru¹

2002

Symp. - Int. Astron. Union

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Abstract. We study the roles of type Ia (SNla) and type II supernovae (SNII) in enrichment of the intra-cluster medium (ICM). Considering stellar [Fe/H] of ellipticals, iron mass in ICM to luminosity ratios, and [a/Fe] of ICM, we show that f'J 53% of iron in ICM comes from SNla. While clusters keep all of ejecta from ellipticals, we obtain the observational evidence for that groups of galaxies lose parts of the gas by supernovae-driven winds. This 'group wind' scenario is confirmed by an 1D hydrodynamical model.

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Measurement of the Elemental Abundances in Four Rich Clusters of Galaxies. I. Observations

Cited by 187 publications

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BeppoSAX observation of the rich cluster of galaxies Abell 85

BeppoSAX observation of the rich cluster of galaxies Abell 85

Far-infrared emission from intracluster dust in Abell clusters

Enrichment of Heavy Elements in Clusters of Galaxies

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