Statistical properties of metal abundances of the intracluster medium in the central region of clusters

Fukazawa, Yasushi; Makishima, Kazuo; Tamura, Takayuki; Nakazawa, K.; Ezawa, H.; Ikebe, Y.; Kikuchi, K.; Ohashi, T.

doi:10.1046/j.1365-8711.2000.03204.x

Cited by 71 publications

(82 citation statements)

References 41 publications

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“…It shows high values between 0.6 and 0.8 (in solar units) in the innermost 100 kpc, then varies between 0.2 and 0.5 at larger radii. The mean emission-weighted metallicity within 200 arcsec is about 0.4 Z , a value usually found in nearby rich clusters (e.g., Fukazawa et al 2000). The extent to which the hydrogen column density is fixed or not only has a very small effect; therefore, the results related to the metallicity presented below are always obtained by letting N H remain free.…”

Section: X-ray Spectral Analysis and Temperature Mapmentioning

confidence: 76%

Diffuse light and building history of the galaxy cluster Abell 2667

Covone

Adami²,

Durret

et al. 2006

A&A

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Aims. We searched for diffuse intracluster light in the galaxy cluster Abell 2667 (z = 0.233) from HST images in three broad bandfilters.Methods. We applied an iterative multi-scale wavelet analysis and reconstruction technique to these images, which allows to subtract stars and galaxies from the original images. Results. We detect a zone of diffuse emission southwest of the cluster center (DS1) and a second faint object (ComDif) within DS1. Another diffuse source (DS2) may be detected at lower confidence level northeast of the center. These sources of diffuse light contribute to 10−15% of the total visible light in the cluster. Whether they are independent entities or part of the very elliptical external envelope of the central galaxy remains unclear. Deep VLT VIMOS integral field spectroscopy reveals a faint continuum at the positions of DS1 and ComDif but do not allow a redshift to be computed, so we conclude if these sources are part of the central galaxy or not. A hierarchical substructure detection method reveals the presence of several galaxy pairs and groups defining a similar direction to the one drawn by the DS1 -central galaxy -DS2 axis. The analysis of archive XMM-Newton and Chandra observations shows X-ray emission elongated in the same direction. The X-ray temperature map shows the presence of a cool core, a broad cool zone stretching from north to south, and hotter regions towards the northeast, southwest, and northwest. This might suggest shock fronts along these directions produced by infalling material, even if uncertainties remain quite large on the temperature determination far from the center. Conclusions. These various data are consistent with a picture in which diffuse sources are concentrations of tidal debris and harassed matter expelled from infalling galaxies by tidal stripping and undergoing an accretion process onto the central cluster galaxy; as such, they are expected to be found along the main infall directions. Note, however, that the limited signal to noise of the various data and the apparent lack of large numbers of well-defined independent tidal tails, besides the one named ComDif, preclude definitive conclusions on this scenario.

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Section: X-ray Spectral Analysis and Temperature Mapmentioning

confidence: 76%

Diffuse light and building history of the galaxy cluster Abell 2667

Covone

Adami²,

Durret

et al. 2006

A&A

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“…Within cool core regions, clusters have negative abundance gradients (e.g. Fukazawa et al 2000;De Grandi et al 2004). and Leccardi et al (2010) also found central metal abundance excess in low-entropy core systems.…”

Section: Fe Profiles Within the Cool Core Regionsmentioning

confidence: 99%

“…The ASCA satellite (Tanaka et al 1994) first enabled us to measure the distribution of Fe in the ICM (e.g., Fukazawa et al 2000;Finoguenov et al 2000Finoguenov et al , 2001. The Fe abundances of these clusters are 0.2−0.3 solar, adopting the solar abundance from the "photospheric" values given by Anders & Grevesse (1989).…”

Section: Introductionmentioning

confidence: 99%

Radial profiles of Fe abundance in the intracluster medium of nearby clusters observed withXMM-Newton

Matsushita

2011

A&A

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Aims. The abundances of Fe in the intracluster medium of nearby (z < 0.08) clusters were measured up to 0.3 ∼ 0.5r 180 . Methods. We analyzed 28 clusters of galaxies observed with XMM-Newton. We derived Fe abundances from the flux ratios of Fe lines to the continuum within an energy range of 3.5−6 keV to minimize and evaluate systematic uncertainties. Results. The radial profiles of the Fe abundances of relaxed clusters with a cD galaxy at their X-ray peak have similar slopes. These clusters show similar enhancements in the Fe abundance within 0.1r 180 , and at 0.1−0.3r 180 , they have flatter Fe abundance profiles at 0.4 ∼ 0.5 solar, with a small scatter. Most other clusters, including merging clusters, also have similar Fe abundance profiles beyond 0.1r 180 . These clusters may have universal metal enrichment histories, and a significant amount of Fe was synthesized at a very early stage in cluster formation. Mergers of clusters can destroy the central Fe peak.

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“…We leave the abundances of Ar, Ca, Fe, and Ni (the only elements that have emission lines in the range 3-10 keV) free and keep all the other abundances fixed to half the solar values [Fukazawa et al 2000; this corresponds for example to the 1T (3-10 keV) model in Tables 1 and 2].…”

Section: Observation and Data Preparationmentioning

confidence: 99%

Ni Abundance in the Core of the Perseus Cluster: An Answer to the Significance of Resonant Scattering

Gastaldello

Molendi²

2004

ApJ

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Using an XMM-Newton observation of the Perseus cluster we show that the excess in the flux of the 7-8 keV line complex previously detected by ASCA and BeppoSAX is due to an overabundance of nickel rather than to an anomalously high Fe He /Fe He ratio. This observational fact leads to the main result that resonant scattering, which was assumed to be responsible for the supposed anomalous Fe He /Fe He ratio, is no longer required. The absence of resonant scattering points toward the presence of significant gas motions (either turbulent or laminar) in the core of the Perseus Cluster.

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Statistical properties of metal abundances of the intracluster medium in the central region of clusters

Cited by 71 publications

References 41 publications

Diffuse light and building history of the galaxy cluster Abell 2667

Diffuse light and building history of the galaxy cluster Abell 2667

Radial profiles of Fe abundance in the intracluster medium of nearby clusters observed withXMM-Newton

Ni Abundance in the Core of the Perseus Cluster: An Answer to the Significance of Resonant Scattering

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