Deprojected analysis of Abell 1835 observed with<i>Chandra</i>and compared with<i>XMM-Newton</i>

Li, Cheng-Kui; Jia, S.; Chen, Yong; Fang, Xiang; Wang, Y. S.; Zhao, Huabiao

doi:10.1051/0004-6361/201118578

Cited by 5 publications

(6 citation statements)

References 41 publications

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“…Figure 1 shows the fit to the projected temperature profile (blue line) assuming a deviation of the entropy from the profile k ∼ r a at r > r b ; this because a powerlaw increase is inconsistent with the Chandra data (see the green line). From the surface brightness distribution (see Figure 1), we derive the ICP density profile of Figure 2 in a slightly different way than the deprojected electron density profile obtained by Li et al (2012) from Chandra observations and in agreement with the profile derived at r 180 by the Suzaku observations (Ichikawa et al 2013). As shown in Figure 5, the gas density profile gives a central SZ effect value absolutely consistent with the observations (Reese et al 2002), at variance with the gas density profile derived by Li et al (2012).…”

Section: Supermodel Analysis Of A1835supporting

confidence: 72%

“…From the surface brightness distribution (see Figure 1), we derive the ICP density profile of Figure 2 in a slightly different way than the deprojected electron density profile obtained by Li et al (2012) from Chandra observations and in agreement with the profile derived at r 180 by the Suzaku observations (Ichikawa et al 2013). As shown in Figure 5, the gas density profile gives a central SZ effect value absolutely consistent with the observations (Reese et al 2002), at variance with the gas density profile derived by Li et al (2012). Moreover, our SZ effect profile reproduces fairly well the profile observed by Bolocam at r 30 (Sayers et al 2011).…”

Section: Supermodel Analysis Of A1835mentioning

confidence: 97%

“…ICP density profile. The solid line is the electron density profile obtained by the SM fit to the surface brightness profile observed by Chandra in A1835 (see Figure 1); the dashed line is the fit with a double-β model (Cavaliere & Fusco-Femiano 1976) of the deprojected density derived by Li et al (2012) from the Chandra results. The red points are the Suzaku results (Ichikawa et al 2013).…”

Section: Supermodel Analysis Of A1835mentioning

confidence: 99%

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Turbulence in the Supermodel: Mass Reconstruction With Nonthermal Pressure for A1835

Fusco-Femiano

Lapi

2013

ApJ

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The total mass derived from X-ray emission is biased low in a large number of clusters when compared with the mass estimated via strong and weak lensing. Suzaku and Chandra observations out to the virial radius report in several relaxed clusters' steep temperature gradients that on assuming pure thermal hydrostatic equilibrium (HE) imply an unphysically decreasing mass profile. Moreover, the gas mass fraction appears to be inconsistent with the cosmic value measured from the cosmic microwave background. Such findings can be interpreted as evidence for an additional nonthermal pressure in the outskirts of these clusters. This nonthermal component may be due to turbulence stirred by residual bulk motions of extragalactic gas infalling into the cluster. Here, we present a SuperModel analysis of A1835 observed by Chandra out to the virial radius. The SuperModel formalism can include in the equilibrium a nonthermal component whose level and distribution are derived imposing that the gas mass fraction (f gas ) equals the cosmic value at the virial radius. Including such a nonthermal component, we reconstruct from X-rays an increasing mass profile consistent with the HE also in the cluster outskirts and in agreement at the virial boundary with the weak-lensing value. The increasing f gas profile confirms that the baryons are not missing but located at the cluster outskirts.

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Section: Supermodel Analysis Of A1835supporting

confidence: 72%

Section: Supermodel Analysis Of A1835mentioning

confidence: 97%

Section: Supermodel Analysis Of A1835mentioning

confidence: 99%

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Turbulence in the Supermodel: Mass Reconstruction With Nonthermal Pressure for A1835

Fusco-Femiano

Lapi

2013

ApJ

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“…The Chandra data are performed by CIAO 4.3 and CALDB 4.4.0. We analyze the Chandra data following the method discussed in Li et al (2012). The tool LC CLEAN in CIAO is used to scan the light curve of data for flares, and the Good Time Intervals (GTIs) are selected.…”

Section: Sample Selection and Data Analysismentioning

confidence: 99%

“…By multiplying the effective area of Chandra/ACIS with the corresponding splines of the stacked residuals, Schellenberger et al (2014) changed the energy dependence of effective area and found that the temperatures between Chandra/ACIS and XMM-Newton/pn were consistent. Li et al (2012) tried to fit Chandra spectra with XMM-Newton temperatures and presented that the modified Chandra mass of Abell 1835 was consistent with the XMM-Newton mass. These works focused on looking for the reasons of discrepancy in temperature or mass, but they didn't give an correction relation which can be used directly in combining Chandra and XMM-Newton data to build a large sample.…”

Section: Introductionmentioning

confidence: 99%

UNBIASED CORRECTION RELATIONS FOR GALAXY CLUSTER PROPERTIES DERIVED FROMCHANDRAANDXMM-NEWTON

Zhao

Chen

et al. 2015

ApJ

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We use a sample of 62 clusters of galaxies to investigate the discrepancies of gas temperature and total mass within r 500 between XMM-Newton and Chandra data. Comparisons of the properties show that (1) Both the de-projected and projected temperatures determined by Chandra are higher than those of XMM-Newton and there is a good linear relation for the de-projected temperature: T Chandra =1.25×T XM M -0.13.(2) The Chandra mass is much higher than XMM-Newton mass with a bias of 0.15 and our mass relation is: log 10 M Chandra =1.02 × log 10 M XM M +0.15. To explore the reasons for the discrepancy in mass, we recalculate the Chandra mass (expressed as M mo/d Ch ) by modifying its temperature with the de-projected temperature relation. The results show that M mo/d Ch is more close to the XMM-Newton mass with the bias reducing to 0.02. Moreover, M mo/d Ch are corrected with the r 500 measured by XMM-Newton and the intrinsic scatter is significantly improved with the value reducing from 0.20 to 0.12. These mean that the temperature bias may be the main factor causing the mass bias. At last, we find that M mo/d Ch is consistent with the corresponding XMM-Newton mass derived directly from our mass relation at a given Chandra mass. Thus, the deprojected temperature and mass relations can provide unbiased corrections for galaxy cluster properties derived from Chandra and XMM-Newton.

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SUZAKUOBSERVATIONS OF THE OUTSKIRTS OF A1835: DEVIATION FROM HYDROSTATIC EQUILIBRIUM

Ichikawa¹,

Matsushita²,

Okabe³

et al. 2013

ApJ

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We present results of four-pointing Suzaku X-ray observations (total ∼200 ks) of the intracluster medium (ICM) in the Abell 1835 galaxy cluster (kT ∼ 8 keV, z = 0.253) out to the virial radius (r vir ∼ 2.9 Mpc) and beyond. Faint X-ray emission from the ICM out to r vir is detected. The temperature gradually decreases with radius from ∼8 keV in the inner region to ∼2 keV at r vir . The entropy profile is shown to flatten beyond r 500 , in disagreement with the r 1.1 dependence predicted from the accretion shock heating model. The thermal pressure profile in the range 0.3r 500 < ∼ r < ∼ r vir agrees well with that obtained from the stacked Sunyaev-Zel'dovich effect observations with the Planck satellite. The hydrostatic mass profile in the cluster outskirts (r 500 < ∼ r < ∼ r vir ) falls well short of the weak lensing one derived from Subaru/Suprime-Cam observations, showing an unphysical decrease with radius. The gas mass fraction at r vir defined with the lensing total mass agrees with the cosmic baryon fraction from the WMAP 7-year data. All these results indicate, rather than the gas-clumping effect, that the bulk of the ICM in the cluster outskirts is far from hydrostatic equilibrium and infalling matter retained some of its kinetic energy. Finally, combining with our recent Suzaku and lensing analysis of Abell 1689, a cluster of similar mass, temperature, and redshift, we show that the cluster temperature distribution in the outskirts is significantly correlated with the galaxy density field in the surrounding large-scale environment at (1-2)r vir .

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Deprojected analysis of Abell 1835 observed withChandraand compared withXMM-Newton

Cited by 5 publications

References 41 publications

Turbulence in the Supermodel: Mass Reconstruction With Nonthermal Pressure for A1835

Turbulence in the Supermodel: Mass Reconstruction With Nonthermal Pressure for A1835

UNBIASED CORRECTION RELATIONS FOR GALAXY CLUSTER PROPERTIES DERIVED FROMCHANDRAANDXMM-NEWTON

SUZAKUOBSERVATIONS OF THE OUTSKIRTS OF A1835: DEVIATION FROM HYDROSTATIC EQUILIBRIUM

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