We present a consistent analysis of Chandra and XMM-Newton observations of an approximately mass-selected sample of 50 galaxy clusters at 0.15 < z < 0.3 -the 'LoCuSS high-L-X sample'. We apply the same analysis methods to data from both satellites, including newly developed analytic background models that predict the spatial variation of the Chandra and XMM-Newton backgrounds to < 2 and < 5 per cent precision, respectively. To verify the cross-calibration of Chandra-and XMM-Newton-based cluster mass measurements, we derive the mass profiles of the 21 clusters that have been observed with both satellites, extracting surface brightness and temperature profiles from identical regions of the respective data sets. We obtain consistent results for the gas and total hydrostatic cluster masses: the average ratio of Chandra-to XMM-Newton-based measurements of M-gas and M-X at r(500) are 0.99 +/- 0.02 and 1.02 +/- 0.05, respectively, with an intrinsic scatter of similar to 3 per cent for gas masses and similar to 8 per cent for hydrostatic masses. Comparison of our hydrostatic mass measurements at r(500) with the latest Local Cluster Substructure Survey (LoCuSS) weak-lensing results indicate that the data are consistent with non-thermal pressure support at this radius of similar to 7 per cent. We also investigate the scaling relation between our hydrostatic cluster masses and published integrated Compton parameter Y-sph measurements from the Sunyaev-Zel'dovich Array. We measure a scatter in mass at fixed Y-sph of similar to 16 per cent at Delta = 500, which is consistent with theoretical predictions of similar to 10-15 per cent scatter.

Martino, R., Mazzotta, P., Bourdin, H., Smith, G., Bartalucci, I., Marrone, D., et al. (2014). LoCuSS: hydrostatic mass measurements of the high-L-X cluster sample cross-calibration of Chandra and XMM-Newton. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 443(3), 2342-2360 [10.1093/mnras/stu1267].

LoCuSS: hydrostatic mass measurements of the high-L-X cluster sample cross-calibration of Chandra and XMM-Newton

MAZZOTTA, PASQUALE;Bourdin, H;
2014

Abstract

We present a consistent analysis of Chandra and XMM-Newton observations of an approximately mass-selected sample of 50 galaxy clusters at 0.15 < z < 0.3 -the 'LoCuSS high-L-X sample'. We apply the same analysis methods to data from both satellites, including newly developed analytic background models that predict the spatial variation of the Chandra and XMM-Newton backgrounds to < 2 and < 5 per cent precision, respectively. To verify the cross-calibration of Chandra-and XMM-Newton-based cluster mass measurements, we derive the mass profiles of the 21 clusters that have been observed with both satellites, extracting surface brightness and temperature profiles from identical regions of the respective data sets. We obtain consistent results for the gas and total hydrostatic cluster masses: the average ratio of Chandra-to XMM-Newton-based measurements of M-gas and M-X at r(500) are 0.99 +/- 0.02 and 1.02 +/- 0.05, respectively, with an intrinsic scatter of similar to 3 per cent for gas masses and similar to 8 per cent for hydrostatic masses. Comparison of our hydrostatic mass measurements at r(500) with the latest Local Cluster Substructure Survey (LoCuSS) weak-lensing results indicate that the data are consistent with non-thermal pressure support at this radius of similar to 7 per cent. We also investigate the scaling relation between our hydrostatic cluster masses and published integrated Compton parameter Y-sph measurements from the Sunyaev-Zel'dovich Array. We measure a scatter in mass at fixed Y-sph of similar to 16 per cent at Delta = 500, which is consistent with theoretical predictions of similar to 10-15 per cent scatter.
Pubblicato
Rilevanza internazionale
Articolo
Esperti anonimi
Settore FIS/05 - Astronomia e Astrofisica
English
Martino, R., Mazzotta, P., Bourdin, H., Smith, G., Bartalucci, I., Marrone, D., et al. (2014). LoCuSS: hydrostatic mass measurements of the high-L-X cluster sample cross-calibration of Chandra and XMM-Newton. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 443(3), 2342-2360 [10.1093/mnras/stu1267].
Martino, R; Mazzotta, P; Bourdin, H; Smith, G; Bartalucci, I; Marrone, D; Finoguenov, A; Okabe, N
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/2108/134697
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