SZ and X-ray combined analysis of a distant galaxy cluster, RX J2228+2037

Pointecouteau, É.; Hattori, Makoto; Neumann, D. M.; Komatsu, Eiichiro; Matsuo, Hiroshi; Kuno, Nario; Böhringer, H.

doi:10.1051/0004-6361:20020394

Cited by 16 publications

(22 citation statements)

References 20 publications

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“…In our analysis, the extrapolated value of r vir = 2.48 ± 0.38 Mpc = 7.5 ± 1.1 , and M vir = (1.55 ± 0.72) × 10 15 M , which both agree with the measurements derived by Pointecouteau et al (2002). …”

Section: Total Masssupporting

confidence: 90%

“…+2.39 −1.56 keV, which is consistent with the results of Pointecouteau et al (2002) and LaRoque et al (2006) within the margins of error and a little higher than that of Morandi et al (2007). The diamonds in the bottom panel of Fig.…”

Section: Radial Deprojected Temperature Profilesupporting

confidence: 89%

“…8. The integrated X-ray pressure profile of RXC J2228.6 +2036 convolved with the PSF of the SZ telescope (the solid line) and compared with the SZ radial profile (the diamonds) derived by Pointecouteau et al (2002). All errors shown correspond to the 68% confidence level.…”

Section: Gas Pressure and Comparison With The Sz Datamentioning

confidence: 99%

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XMM-Newton studies of a massive cluster of galaxies: RXC J2228.6+2036

Jia

Böhringer

Pointecouteau

et al. 2008

A&A

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We present the X-ray properties of a massive cluster of galaxies (RXC J2228.6+2036 at z = 0.421) using XMM-Newton data. The X-ray mass modeling is based on the temperature and density distributions of the intracluster medium derived using a deprojection method. We find that RXC J2228.6+2036 is a hot cluster (T 500 = 8.92 based on spectral fitting within the cooling flow radius (r cool = 147 ± 10 kpc). The total cluster mass is M 500 = (1.19 ± 0.35) × 10 15 M and the mean gas mass fraction is f gas = 0.165 ± 0.045 at r 500 = 1.61 ± 0.16 Mpc. We discuss the PSF-correction effect on the spectral analysis and find that, for the selected annular width, the PSF-corrected temperatures are consistent with those without PSF-correction. We observe remarkable agreement between X-ray and SZ results, which is of prime importance for future SZ surveys. RXC J2228.6+2036 obeys the empirical scaling relations found in general massive galaxy clusters (e.g. S -T , M-T , L-T and M-Y), after accounting for self-similar evolution.

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Section: Total Masssupporting

confidence: 90%

Section: Radial Deprojected Temperature Profilesupporting

confidence: 89%

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XMM-Newton studies of a massive cluster of galaxies: RXC J2228.6+2036

Jia

Böhringer

Pointecouteau

et al. 2008

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“…Early single target SZ studies were limited to the clusters' inner regions (i.e., within R 500 ), and were not really competitive with the X-ray measurements in terms of resolution and sensitivity (see e.g., Pointecouteau et al 2001;Halverson et al 2009;Korngut et al 2011). However, the combination of SZ and X-ray tracers has already shown its potential in terms of structural studies of clusters (Pointecouteau et al 2002;Kitayama et al 2004;Jia et al 2008;Basu et al 2010). The first studies working on SZ cluster samples were presented by the SPT and ACT collaborations (Plagge et al 2010;Sehgal et al 2011), with 15 and 9 high significance clusters, respectively.…”

Section: The Inner Profilementioning

confidence: 99%

Planckintermediate results

Ade

Aghanim

Arnaud

et al. 2013

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Taking advantage of the all-sky coverage and broad frequency range of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and pressure profiles of 62 nearby massive clusters detected at high significance in the 14-month nominal survey. Careful reconstruction of the SZ signal indicates that most clusters are individually detected at least out to R 500 . By stacking the radial profiles, we have statistically detected the radial SZ signal out to 3 × R 500 , i.e., at a density contrast of about 50-100, though the dispersion about the mean profile dominates the statistical errors across the whole radial range. Our measurement is fully consistent with previous Planck results on integrated SZ fluxes, further strengthening the agreement between SZ and X-ray measurements inside R 500 . Correcting for the effects of the Planck beam, we have calculated the corresponding pressure profiles. This new constraint from SZ measurements is consistent with the X-ray constraints from XMM-Newton in the region in which the profiles overlap (i.e., [0.1-1] R 500 ), and is in fairly good agreement with theoretical predictions within the expected dispersion. At larger radii the average pressure profile is slightly flatter than most predictions from numerical simulations. Combining the SZ and X-ray observed profiles into a joint fit to a generalised pressure profile gives best-fit parameters [P 0 , c 500 , γ, α, β] = [6.41, 1.81, 0.31, 1.33, 4.13]. Using a reasonable hypothesis for the gas temperature in the cluster outskirts we reconstruct from our stacked pressure profile the gas mass fraction profile out to 3 R 500 . Within the temperature driven uncertainties, our Planck constraints are compatible with the cosmic baryon fraction and expected gas fraction in halos. Key words. cosmology: observations -galaxies: clusters: general -galaxies: clusters: intracluster medium -submillimeter: general -X-rays: general Appendices are available in electronic form at

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“…Such a method has previously been used to extract 1D gas temperature profiles, complementing X-ray spectroscopic measurements (e.g. Pointecouteau et al 2002;Kitayama et al 2004;Nord et al 2009;Basu et al 2010;Eckert et al 2013;Ruppin et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel’dovich imaging

Adam

Arnaud

Bartalucci

et al. 2017

A&A

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We propose a method to map the temperature distribution of the hot gas in galaxy clusters that uses resolved images of the thermal Sunyaev-Zel'dovich (tSZ) effect in combination with X-ray data. Application to images from the New IRAM KIDs Array (NIKA) and XMM-Newton allows us to measure and determine the spatial distribution of the gas temperature in the merging cluster MACS J0717.5+3745, at z = 0.55. Despite the complexity of the target object, we find a good morphological agreement between the temperature maps derived from X-ray spectroscopy only -using XMM-Newton (T XMM ) and Chandra (T CXO ) -and the new gas-mass-weighted tSZ+X-ray imaging method (T SZX ). We correlate the temperatures from tSZ+X-ray imaging and those from X-ray spectroscopy alone and find that T SZX is higher than T XMM and lower than T CXO by ∼10% in both cases. Our results are limited by uncertainties in the geometry of the cluster gas, contamination from kinetic SZ (∼10%), and the absolute calibration of the tSZ map (7%). Investigation using a larger sample of clusters would help minimise these effects.

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SZ and X-ray combined analysis of a distant galaxy cluster, RX J2228+2037

Cited by 16 publications

References 20 publications

XMM-Newton studies of a massive cluster of galaxies: RXC J2228.6+2036

XMM-Newton studies of a massive cluster of galaxies: RXC J2228.6+2036

Planckintermediate results

Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel’dovich imaging

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