XMM-Newton observation of the Coma Galaxy
 cluster

Arnaud, M.; Aghanim, N.; Gastaud, R.; Neumann, D. M.; Lumb, D.; Briel, U. G.; Altiéri, B.; Ghizzardi, S.; Mittaz, Jonathan P. D.; Sasseen, T.; Vestrand, W. T.

doi:10.1051/0004-6361:20000195

Cited by 121 publications

(129 citation statements)

References 22 publications

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“…Indeed, we find that a satisfactory fit (χ 2 /dof = 846.5/856) is achieved using two APEC models. The most intense component has a temperature of 8.40 +0.25 −0.24 keV and an abundance of 0.21 +0.03 −0.03 , consistent with what was found by Arnaud et al (2001) and Lutovinov et al (2008). The low-temperature component (T = 1.45 +0.21 −0.11 keV and Z = 0.05(±0.02)Z ) very likely accounts for one or more of the X-ray sources in the field of Coma.…”

Section: Comasupporting

confidence: 89%

GALAXY CLUSTERS IN THESWIFT/BURST ALERT TELESCOPE ERA: HARD X-RAYS IN THE INTRACLUSTER MEDIUM

Ajello

Rebusco

Cappelluti

et al. 2008

ApJ

101

126

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We report the detection of 10 clusters of galaxies in the ongoing Swift/Burst Alert Telescope (BAT) all-sky survey. This sample, which mostly comprises merging clusters, was serendipitously detected in the 15-55 keV band. We use the BAT sample to investigate the presence of excess hard X-rays above the thermal emission. The BAT clusters do not show significant (e.g., 2σ ) nonthermal hard X-ray emission. The only exception is represented by Perseus whose high-energy emission is likely due to NGC 1275. Using XMM-Newton, Swift/XRT, Chandra and BAT data, we are able to produce upper limits of the inverse Compton (IC) emission mechanism which are in disagreement with most of the previously-claimed hard X-ray excesses. The coupling of the X-ray upper limits of the IC mechanism to radio data shows that, in some clusters, the magnetic field might be larger than 0.5 μG. We also derive the first log N-log S and luminosity function distributions of galaxy clusters above 15 keV.

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Section: Comasupporting

confidence: 89%

GALAXY CLUSTERS IN THESWIFT/BURST ALERT TELESCOPE ERA: HARD X-RAYS IN THE INTRACLUSTER MEDIUM

Ajello

Rebusco

Cappelluti

et al. 2008

ApJ

101

126

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“…This is consistent with our observations 3 , especially since n e (r) varies much more than T (r) in the Coma cluster (see e.g. Arnaud et al 2001;Snowden et al 2008). Jeltema & Profumo (2011) derive a lower limit for the average field in Coma of 1.7 μG, from limits on the Fermi γ-ray 3 In the case that α = 1 + δ, the relationship would be r ∝ (y/T ) 1+δ/2 , if we assume B ∝ √ n e .…”

Section: Quasi-linear Sz-radio Relationsupporting

confidence: 93%

Planckintermediate results

Collaboration¹,

Ade

Aghanim

et al. 2013

A&A

Self Cite

104

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We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r ≈ 3 × R 500 . We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) "universal" pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R 500 ; by r = 2 × R 500 it underestimates the observed y profile by a factor of 2. This may indicate that at these larger radii either: i) the cluster SZ emission is contaminated by unresolved SZ sources along the line of sight; or ii) the pressure profile of Coma is higher at r > R 500 than the mean pressure profile predicted by the simulations used to constrain the models. The Planck image shows significant local steepening of the y profile in two regions about half a degree to the west and to the south-east of the cluster centre. These features are consistent with the presence of shock fronts at these radii, and indeed the western feature was previously noticed in the ROSAT PSPC mosaic as well as in the radio. Using Planck y profiles extracted from corresponding sectors we find pressure jumps of 4.9 +0.4 −0.2 and 5.0 +1.3 −0.1 in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number M w = 2.03 +0.09 −0.04 and M se = 2.05 +0.25 −0.02 in the west and south-east, respectively. Finally, we find that the y and radio-synchrotron signals are quasi-linearly correlated on Mpc scales, with small intrinsic scatter. This implies either that the energy density of cosmic-ray electrons is relatively constant throughout the cluster, or that the magnetic fields fall off much more slowly with radius than previously thought.

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“…In comparison, the first cluster temperature measurement using purely the SZ observations gave T e = 26 +34 −19 keV for A2163 (Hansen, Pastor & Semikoz 2002), where only observations at 4 frequencies were available. Similarly, using the observed temperature, T e = 8.25 ± 0.10 keV (Arnaud et al 2001), one finds the peculiar velocity v p = −300 ± 500 km/sec, as seen on figure 1b, which is in good agreement with the findings of Colless et al (2001).…”

Section: An Example: Comasupporting

confidence: 84%

Extraction of cluster parameters from Sunyaev–Zeldovich effect observations with simulated annealing optimization

Hansen

2004

New Astronomy

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XMM-Newton observation of the Coma Galaxy cluster

Cited by 121 publications

References 22 publications

GALAXY CLUSTERS IN THESWIFT/BURST ALERT TELESCOPE ERA: HARD X-RAYS IN THE INTRACLUSTER MEDIUM

GALAXY CLUSTERS IN THESWIFT/BURST ALERT TELESCOPE ERA: HARD X-RAYS IN THE INTRACLUSTER MEDIUM

Planckintermediate results

Extraction of cluster parameters from Sunyaev–Zeldovich effect observations with simulated annealing optimization

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