Temperature Map of the Virgo Cluster of Galaxies Observed with<i>ASCA</i>

Shibata, Ryo; Matsushita, Kyoko; Yamasaki, Noriko Y.; Ohashi, T.; Ishida, M.; Kikuchi, K.; Böhringer, H.; Matsumoto, Hironori

doi:10.1086/319075

Cited by 73 publications

(75 citation statements)

References 50 publications

(66 reference statements)

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“…In addition to the physically motivated model of the cosmic X-ray background (CXB) consisting of two unabsorbed MEKAL models plus a power law with fixed index γ = 1.4 (see Lumb et al 2002;De Luca & Molendi 2004), we considered a further thermal MEKAL component of the total background spectrum in order to account for the local foreground emission of Virgo at the position of XMMU J1230.3+1339. From this four-component model we obtained a best fitting local Virgo temperature of kT Virgo = 1.88 keV consistent with previous ASCA measurements of this region (Shibata et al 2001). This four-component model, with a renormalization appropriate to the ratio of the surface area of the extraction regions, was then added to the fit of the cluster spectrum, resulting in an X-ray temperature based on this external background model of 6.4 +1.7 −1.2 keV.…”

Section: Figsupporting

confidence: 87%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

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Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

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Section: Figsupporting

confidence: 87%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

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“…The latter is more likely to be the case: A1553 is directly behind the nearby Virgo Cluster of galaxies. The center of A1553 is %1: 8 to the south of M 87 and is clearly surrounded by X-ray emission from the foreground cluster (Böhringer et al 1994;Shibata et al 2001). Virgo has an average X-ray temperature of %2.5 keV (Shibata et al 2001), and therefore it is likely that A1553's true temperature is larger than previously derived.…”

Section: Cluster Propertiesmentioning

confidence: 81%

“…detected in X-rays numerous times (e.g., Böhringer et al 1994Böhringer et al , 2000Shibata et al 2001). White (2000) derived a temperature of 4:18 AE 0:15 keV for A1553 from ASCA data, but this temperature assumes a single thermal component model, and the temperature profile in the ASCA data is dropping significantly with radius, possibly because of poorer quality data or problems with background subtraction.…”

Section: Cluster Propertiesmentioning

confidence: 99%

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Feldmeier¹,

Mihos²,

Morrison³

et al. 2004

ApJ

132

150

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We report the search for intracluster light in four Abell type II-III (non-cD) galaxy clusters: A801, A1234, A1553, and A1914. We find that on average these clusters contain $10% of their detected stellar luminosity in a diffuse component. We show that for two of the clusters the intracluster light closely follows the galaxy distribution, but in the other two cases, there are noticeable differences between the spatial distribution of the galaxies and the intracluster light. We report the results of a search for intracluster tidal debris in each cluster and note that A1914 in particular has a number of strong tidal features likely due to its status as a recent cluster merger. One of the A1914 features appears to be spatially coincident with an extension seen in weak lensing maps, implying that the feature traces a large amount of mass. We compare these results with numerical simulations of hierarchically formed galaxy clusters and find good general agreement between the observed and simulated images, although we also find that our observations sample only the brightest features of the intracluster light. Together, these results suggest that intracluster light can be a valuable tool in determining the evolutionary state of galaxy clusters.

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“…The known X-ray tails have T ICM /T tail ratios of 3 − 8 (Sun & Vikhlinin 2005;Sun et al 2010;Weżgowiec et al 2011). If we simply take this range for the ratio, the expected tail temperature of IC3418 is 0.3 − 0.8 keV, for a surrounding ICM temperature of ∼ 2.5 keV (Shibata et al 2001). In this work, we assume a single APEC model with temperatures of 0.3 − 0.7 keV and abundances of 0.1 solar or 1 solar (see Table 5).…”

Section: Results -Chandramentioning

confidence: 99%

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Jáchym¹,

Kenney²,

Růžička³

et al. 2013

A&A

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We present IRAM 30m sensitive upper limits on CO emission in the ram pressure stripped dwarf Virgo galaxy IC3418 and in a few positions covering H ii regions in its prominent 17 kpc UV/Hα gas-stripped tail. In the central few arcseconds of the galaxy, we report a possible marginal detection of about 1 × 10 6 M ⊙ of molecular gas (assuming a Galactic CO-to-H 2 conversion factor) that could correspond to a surviving nuclear gas reservoir. We estimate that there is less molecular gas in the main body of IC3418, by at least a factor of 20, than would be expected from the pre-quenching UV-based star formation rate assuming the typical gas depletion timescale of 2 Gyr. Given the lack of star formation in the main body, we think the H 2 -deficiency is real, although some of it may also arise from a higher CO-to-H 2 factor typical in low-metallicity, low-mass galaxies. The presence of H ii regions in the tail of IC3418 suggests that there must be some dense gas; however, only upper limits of < 1 × 10 6 M ⊙ were found in the three observed points in the outer tail. This yields an upper limit on the molecular gas content of the whole tail < 1 × 10 7 M ⊙ , which is an amount similar to the estimates from the observed star formation rate over the tail. We also present strong upper limits on the X-ray emission of the stripped gas in IC3418 from a new Chandra observation. The measured X-ray luminosity of the IC3418 tail is about 280 times lower than that of ESO 137-001, a spiral galaxy in a more distant cluster with a prominent ram pressure stripped tail. Non-detection of any diffuse X-ray emission in the IC3418 tail may be due to a low gas content in the tail associated with its advanced evolutionary state and/or due to a rather low thermal pressure of the surrounding intra-cluster medium.

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Temperature Map of the Virgo Cluster of Galaxies Observed withASCA

Cited by 73 publications

References 50 publications

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

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