A mosaic of the Coma cluster of galaxies with XMM-Newton

Briel, U. G.; Henry, J. P.; Lumb, D.; Arnaud, M.; Neumann, D. M.; Aghanim, N.; Gastaud, R.; Mittaz, Jonathan P. D.; Sasseen, T.; Vestrand, W. T.

doi:10.1051/0004-6361:20000024

Cited by 74 publications

(89 citation statements)

References 15 publications

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“…These regions are masked out of the image used to fit the models and they certainly do not account for the extended regions of enhanced X-ray emission associated with the subhalos. There are no other signs of cooler gas in the images of Figure 7, consistent with previous investigations (Arnaud et al 2001;Briel et al 2001;Neumann et al 2003). In particular, there is no sign of a radial temperature increase in any of these regions.…”

Section: Temperature Perturbationssupporting

confidence: 91%

“…In either case, it is transient on the dynamical timescale and so must be due to recent infall. In the radio, Brown & Rudnick (2011) have argued that a ∼2 Mpc radio relic on the western side of the cluster is one signature of an infall shock, caused by a new, ongoing merger. If so, this merger is distinct from the one responsible for the formation of the X-ray filament.…”

Section: The Coma Clustermentioning

confidence: 99%

“…The temperature plays a secondary role in our models, only entering through the unperturbed enthalpy in Equation (3). Thus, the temperature in the unperturbed cluster is assumed to be constant, an adequate approximation for the core region of the Coma Cluster (see Arnaud et al 2001;Briel et al 2001).…”

Section: Unperturbed Cluster Modelmentioning

confidence: 99%

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Dark Matter Subhalos and the X-Ray Morphology of the Coma Cluster

Andrade-Santos

Nulsen

Kraft

et al. 2013

ApJ

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Structure formation models predict that clusters of galaxies contain numerous massive subhalos. The gravity of a subhalo in a cluster compresses the surrounding intracluster gas and enhances its X-ray emission. We present a simple model, which treats subhalos as slow moving and gasless, for computing this effect. Recent weak lensing measurements by Okabe et al. have determined masses of ∼10 13 M for three mass concentrations projected within 300 kpc of the center of the Coma Cluster, two of which are centered on the giant elliptical galaxies NGC 4889 and NGC 4874. Adopting a smooth spheroidal β-model for the gas distribution in the unperturbed cluster, we model the effect of these subhalos on the X-ray morphology of the Coma Cluster, comparing our results to Chandra and XMM-Newton X-ray data. The agreement between the models and the X-ray morphology of the central Coma Cluster is striking. With subhalo parameters from the lensing measurements, the distances of the three subhalos from the Coma Cluster midplane along our line of sight are all tightly constrained. Using the model to fit the subhalo masses for NGC 4889 and NGC 4874 gives 9.1 × 10 12 M and 7.6 × 10 12 M , respectively, in good agreement with the lensing masses. These results lend strong support to the argument that NGC 4889 and NGC 4874 are each associated with a subhalo that resides near the center of the Coma Cluster. In addition to constraining the masses and 3-d location of subhalos, the X-ray data show promise as a means of probing the structure of central subhalos.

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Section: Temperature Perturbationssupporting

confidence: 91%

Section: The Coma Clustermentioning

confidence: 99%

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Dark Matter Subhalos and the X-Ray Morphology of the Coma Cluster

Andrade-Santos

Nulsen

Kraft

et al. 2013

ApJ

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“…Advantages of mosaicing for cluster outskirts are many, in particular better control over the instrumental background that could be achieved; larger radii of the cluster that could be covered. Coma cluster takes a special place in cluster mosaics as the best-covered nearby cluster, yielding a rich collection of publications (Briel et al 2001;Arnaud et al 2001;Neumann et al 2001;Neumann et al 2003;Finoguenov et al 2003b;Finoguenov et al 2004a;Schuecker et al 2004).…”

Section: Xmm Cluster Mosaicsmentioning

confidence: 99%

XMM-Newton view on cluster outskirts

Finoguenov

2004

IAU

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Abstract. We present an overview on the state of the gas in cluster outskirts. We show that the entropy of the gas in the outskirts often exhibit strong deviations from predictions based on the cluster scaling. We identify the cause of these deviations with incomplete shock propagation observed in clusters with ongoing major merging, survival of substructure and incomplete thermalization, and emission from the surrounding large-scale structure seen in projection.

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“…Direct ROSAT images (Dow & White 1995) and the wavelet analysis of X-ray data by Biviano et al (1996) clearly show that the center of Coma consists of two subclusters, each centered on the bright cD elliptical galaxies NGC 4489 and NGC 4874, separated in projection by Recent XMM data conÐrm the existence 7@ .1. of enhanced, D100 kpc X-ray emission around these two galaxies Briel et al 2001) and so do the Chandra images of Vikhlinin et al (2001). We assume here that the two bright E galaxies are each centers of merging subclusters so the ambient dark matter and gas peaked around each galaxy is locally comoving with the galaxies as they orbit in Coma ; i.e., there is no local ram pressure e †ect near the cD galaxies.…”

Section: W Here Is the Cooled Gas ?mentioning

confidence: 99%

Confrontation of Intracluster and Interstellar Gas in Cluster‐centered Elliptical Galaxies: M87 in Virgo and NGC 4874 in Coma

Brighenti

Mathews

2002

ApJ

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The evolution of hot interstellar gas in cluster-centered cD galaxies and the inÑow of gas from the surrounding galaxy clusters are strongly coupled. Cooling Ñows arise inside the cD galaxy because the deep stellar potential and stellar mass loss increase the gas density and decrease the radiative cooling time within the galaxy. Recent X-ray observations of M87 in the Virgo Cluster and NGC 4874 in Coma reveal that the gas temperature beyond about 50 kpc from these cD galaxies is comparable to the virial temperature of the cluster, 3 or 9 keV, respectively, but within the optical galaxy the temperature drops to the galactic virial temperature D1 keV. We show that these steep thermal gradients on galactic scales follow naturally from the usual cooling inÑow assumptions without recourse to thermal conductivity. However, most of the gas must radiatively cool ("" dropout ÏÏ) before it Ñows to the galactic core ; i.e., the gas must be multiphase. The temperature and density proÐles observed in M87 and NGC 4874 can be matched with approximate gasdynamical models calculated over several gigayears with either globally uniform or centrally concentrated multiphase mass dropout. Recent XMM observations of M87 indicate single-phase Ñow at every radius with no apparent radiative cooling to low temperatures. Gasdynamical models can be made consistent with single-phase Ñow for kpc, but to avoid huge central masses r Z 10 of cooled gas, we assume that some distributed cooling dropout occurs near the center of the Ñow, where the gas temperature is T D 1 keV. The evidence in X-ray spectra for multiphase cooling beginning at lower temperatures D1 keV may be less apparent than for higher temperatures and may have escaped detection. However, even if the mass of cooled gas is distributed within kpc, it is necessary that r [ 10 the mass of cooled gas not conÑict with dynamical mass-to-light determinations. Because of small deviations from true steady-state Ñow, we Ðnd that the standard decomposition methods used by X-ray observers to determine the mass Ñow may fail rather badly, particularly when the mass dropout M 0 (r) decreases with radius in the Ñow. For this case the decomposition procedure gives the usual cooling Ñow result, which is quite unlike the true variation of in our computed models. M 0 P r, M 0 (r)

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A mosaic of the Coma cluster of galaxies with XMM-Newton

Cited by 74 publications

References 15 publications

Dark Matter Subhalos and the X-Ray Morphology of the Coma Cluster

Dark Matter Subhalos and the X-Ray Morphology of the Coma Cluster

XMM-Newton view on cluster outskirts

Confrontation of Intracluster and Interstellar Gas in Cluster‐centered Elliptical Galaxies: M87 in Virgo and NGC 4874 in Coma

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