2017A&A...608A..88B


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.14CET22:58:04

2017A&A...608A..88B - Astronomy and Astrophysics, volume 608A, 88-88 (2017/12-1)

Recovering galaxy cluster gas density profiles with XMM-Newton and Chandra.

BARTALUCCI I., ARNAUD M., PRATT G.W., VIKHLININ A., POINTECOUTEAU E., FORMAN W.R., JONES C., MAZZOTTA P. and ANDRADE-SANTOS F.

Abstract (from CDS):

We examined the reconstruction of galaxy cluster radial density profiles obtained from Chandra and XMM-Newton X-ray observations, using high quality data for a sample of twelve objects covering a range of morphologies and redshifts. By comparing the results obtained from the two observatories and by varying key aspects of the analysis procedure, we examined the impact of instrumental effects and of differences in the methodology used in the recovery of the density profiles. We find that the final density profile shape is particularly robust. We adapted the photon weighting vignetting correction method developed for XMM-Newton for use with Chandra data, and confirm that the resulting Chandra profiles are consistent with those corrected a posteriori for vignetting effects. Profiles obtained from direct deprojection and those derived using parametric models are consistent at the 1% level. At radii larger than ∼6'', the agreement between Chandra and XMM-Newton is better than 1%, confirming an excellent understanding of the XMM-Newton PSF. Furthermore, we find no significant energy dependence. The impact of the well-known offset between Chandra and XMM-Newton gas temperature determinations on the density profiles is found to be negligible. However, we find an overall normalisation offset in density profiles of the order of ∼2.5%, which is linked to absolute flux cross-calibration issues. As a final result, the weighted ratios of Chandra to XMM-Newton gas masses computed at R2500 and R500 are r=1.03±0.01 and r=1.03±0.03, respectively. Our study confirms that the radial density profiles are robustly recovered, and that any differences between Chandra and XMM-Newton can be constrained to the ∼2.5% level, regardless of the exact data analysis details. These encouraging results open the way for the true combination of X-ray observations of galaxy clusters, fully leveraging the high resolution of Chandra and the high throughput of XMM-Newton.

Abstract Copyright: © ESO, 2017

Journal keyword(s): methods: data analysis - galaxies: clusters: intracluster medium - X-rays: galaxies: clusters - X-rays: galaxies: clusters

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 1RXS J054638.7-534434 ClG 05 46 35.0 -53 46 04           ~ 64 0
2 ClG J0717+3745 ClG 07 17 36.50 +37 45 23.0           ~ 334 0
3 ClG J0744+3927 ClG 07 44 52.5 +39 27 30           ~ 152 0
4 ACO 1413 ClG 11 55 18.0 +23 24 19           ~ 374 0
5 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 264 0
6 ACO 1651 ClG 12 59 22.43 -04 11 47.1           ~ 269 0
7 ClG J1423+2404 ClG 14 23 47.7 +24 04 40           ~ 167 0
8 ACO 2163 ClG 16 15 34.1 -06 07 26           ~ 514 0
9 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 390 0
10 SPT-CL J2146-4633 ClG 21 46 35 -46 32.9           ~ 22 0
11 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 615 2
12 SPT-CL J2341-5119 ClG 23 41 12.3 -51 19 43           ~ 34 0

    Equat.    Gal    SGal    Ecl

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2019.12.14-22:58:04

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