Properties of nearby clusters of galaxies

Trèvese, D.; Cirimele, G.; Cenci, A.; Appodia, B.; Флин, П.; Hickson, Paul

doi:10.1051/aas:1997379

Cited by 11 publications

(13 citation statements)

References 11 publications

(12 reference statements)

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“…Abell 2028 in the optical band is an elongated structure as shown by galaxy iso-density images (see Fig. 8 of Trevese et al 1997) or by wavelet analysis (see the panels on scales of 750 kpc and 527 kpc of Fig. 13 in Flin & Krywult 2006).…”

Section: The Dynamical State Of Abell 2028mentioning

confidence: 91%

Apparent high metallicity in 3–4 keV galaxy clusters: the inverse iron-bias in action in the case of the merging cluster Abell 2028

Gastaldello¹,

Ettori²,

Balestra³

et al. 2010

A&A

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Context. Recent work based on a global measurement of the ICM properties finds evidence for an increase in the iron abundance in galaxy clusters with temperatures around 2−4 keV up to a value about 3 times higher than is typical of very hot clusters Z Fe 0.25 Z . Aims. We have started a study of the metal distribution in nearby X-ray luminous poor galaxy clusters in the temperature range 3−4 keV with measured high abundances. Our study aims at spatially resolving the metal content of the central regions of the ICM, in particular characterizing how our measurements are biased by the diagnostics adopted and by the possible multi-temperature nature of the projected observed spectra. We report here on a 42 ks XMM-Newton observation of the first object in the sample, the cluster Abell 2028. Methods. We selected interesting regions of the ICM to analyze the spatially resolved structure of projected temperature and abundance, thereby producing two-dimensional maps. Results. The XMM-Newton observation of the first object of the sample, the cluster Abell 2028, reveals the complex structure of the cluster over a scale of ∼300 kpc, showing an interaction between two subclusters in cometary-like configurations. Cold fronts have been detected at the leading edges of the two substructures. The core of the main subcluster is likely hosting a cool corona. We show that a one-component fit for this region returns a biased high metallicity. The inverse iron bias is caused by the behavior of the fitting code in shaping the Fe-L complex. In the presence of a multi-temperature structure of the ICM, the best-fit metallicity turns out to be artificially higher when the projected spectrum is modeled with a single temperature component, while it is not related to the presence of both Fe-L and Fe-K emission lines in the spectrum. After accounting for the inverse iron bias, the overall abundance of the cluster is consistent with the one typical of hotter, more massive clusters. Conclusions. We caution against interpreting high abundances inferred when fitting a single thermal component to spectra derived from relatively large apertures in 3−4 keV clusters, because the inverse iron bias can be present. Most of the inferences trying to relate high abundances in 3−4 keV clusters to fundamental physical processes will probably have to be revised.

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Section: The Dynamical State Of Abell 2028mentioning

confidence: 91%

Apparent high metallicity in 3–4 keV galaxy clusters: the inverse iron-bias in action in the case of the merging cluster Abell 2028

Gastaldello¹,

Ettori²,

Balestra³

et al. 2010

A&A

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“…E.g. Trèvese et al (1996) find M * = −22.66 ± 0.52 from a study of 36 Abell clusters for a fixed α = −1.25. For this value of α the M * value for A 222 increases to −22.4, but the fit then has a reduced χ 2 of 2.2.…”

Section: Mass-to-light Ratiomentioning

confidence: 99%

Spectroscopy of the neighboring massive clusters Abell 222 and Abell 223

Clowe

Soucail

2002

A&A

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Abstract. We present a spectroscopic catalog of the neighboring massive clusters Abell 222 and Abell 223. The catalog contains the positions, redshifts, R magnitudes, V − R color, as well as the equivalent widths for a number of lines for 183 galaxies, 153 of them belonging to the A 222 and A 223 system. We determine the heliocentric redshifts to be z = 0.2126 ± 0.0008 for A 222 and z = 0.2079 ± 0.0008 for A 223. The velocity dispersions of both clusters in the cluster restframe are about the same: σ = 1014

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“…For clusters of the Z sample we consider only galaxies Metcalfe et al 1994 ;(11) Willmer et al 1991 ;(12) et al 1992 ; (13) Beers et al Sodre 1984 ;(14) (15) Richter 1989 ;(16) Fabricant et al 1993 ;(17) Mohr et al 1996 ;(18) Flin et al 1995 ;(19) Trevese et al 1997 ;(20) Barmby & Huchra 1998 ;(21) Fabricant, Kent, & Kurtz 1989 ;(22) Malumuth & Kriss 1986 ;(23) Bardelli et al 1998 ; (24) COSMOS catalog ; (25) Tully et al 1996. identiÐed as cluster members : for cluster data in common with G98 we use their member identiÐcation after the peak selection in velocity distribution via the adaptive kernel method and the shifting gapper (see also Fadda et al 1996). For new cluster data we apply this same procedure for cluster member identiÐcation.…”

Section: Other Samplesmentioning

confidence: 99%

Optical Luminosities and Mass‐to‐Light Ratios of Nearby Galaxy Clusters

Girardi

Borgani

Giuricin

et al. 2000

ApJ

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We analyze a sample of 105 clusters having virial mass homogeneously estimated and for which galaxy magnitudes are available with a well-deÐned high degree of completeness. In particular, we consider a subsample of 89 clusters with galaxy magnitudes taken from the COSMOS/UKST B j -band Southern Sky Object Catalog. After suitable magnitude corrections and uniform conversions to band, B j we compute cluster luminosities within several clustercentric distances, 0.5, 1.0, 1.5 h~1 Mpc and L Bj within the virialization radiusIn particular, we use the luminosity function and background counts R vir . estimated by Lumsden et al. on the Edinburgh/Durham Southern Galaxy Catalog, which is the wellcalibrated part of the COSMOS catalog. We analyze the e †ect of several uncertainties connected to photometric data, fore/background removal, and extrapolation below the completeness limit of the photometry, in order to assess the robustness of our cluster luminosity estimates. We draw our results on the relations between luminosity and dynamical quantities from the COSMOS sample by considering mass and luminosities determined within the virialization radius. We Ðnd a very good correlation between cluster luminosity, and galaxy velocity dispersion, with Our estimate of . the typical value for the mass-to-light ratio isWe do not Ðnd any correlation ofwith cluster morphologies, i.e., Rood-Sastry and Bautz-Morgan types, and only a weak signiÐcant M/L Bj correlation with cluster richness. We Ðnd that mass has a slight, but signiÐcant, tendency to increase faster than the luminosity does,We verify the robustness of this relation against a number M P L Bj 1.2h1.3. of possible systematics. We verify that this increasing trend of M/L with cluster mass cannot be entirely due to a higher spiral fraction in poorer clusters, thus suggesting that a similar result would also be found by using R-band galaxy magnitudes.

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Properties of nearby clusters of galaxies

Cited by 11 publications

References 11 publications

Apparent high metallicity in 3–4 keV galaxy clusters: the inverse iron-bias in action in the case of the merging cluster Abell 2028

Apparent high metallicity in 3–4 keV galaxy clusters: the inverse iron-bias in action in the case of the merging cluster Abell 2028

Spectroscopy of the neighboring massive clusters Abell 222 and Abell 223

Optical Luminosities and Mass‐to‐Light Ratios of Nearby Galaxy Clusters

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