tokens: resolved temperature profiles up to . The fifth cluster, PLCK G266.627.3, had already been observed to similar depth with Chandra ( ks, proposal , PI P. Mazzotta). In addition to our deep XMM-Newton data, the four SPT clusters had previously been observed as part of the Chandra X-Ray Visionary Project proposal (P.I. B. Benson). Exposure times for these observations (typically 80 ks), were tuned so as to obtain counts per cluster to allow for global properties to be measured ( McDonald et al. 2014 ). The original ks snapshot observation of PLCK G266.627.3, obtained as part of the Planck - XMM-Newton validation programme, is described in Planck Collaboration XXVI (2011) . Observation details are given in Table 1 . All the XMM-Newton observations were taken using the European Photon Imaging Camera (EPIC), combining the data taken with the MOS, MOS, and PN cameras. Chandra observations were taken using the Advanced CCD imaging spectrometer (ACIS, Garmire et al. 2003 ). XMM-Newton and Chandra images of all five objects are shown in Appendix A . Table 2 Global properties. Notes. (a) Spectroscopic temperature measured in the region. (b) is the product of and ( Kravtsov et al. 2006 ). (d) The gas mass within , derived using the combined density profiles. (c,e) and are determined iteratively using the relation of Arnaud et al. (2010) , assuming self-similar evolution. 2.2. Data preparation We processed Chandra observations using the Chandra Interactive Analysis of Observations (CIAO, Fruscione et al. 2006 ) ver. 4.7 and the calibration database 3 ver. 4.6.5. The latest version of calibration files were applied following the prescriptions detailed in cxc.harvard.edu/ciao/ guides/acis_data.html? using the chandra_repro tool. To process the XMM-Newton datasets, we used the Science Analysis System 4 pipeline ver. and calibration files as available in December . New event files with the latest calibration applied were produced using the emchain and epchain tools. 2.3. Data filtering We reduced the contamination from high-energy particles using the Very Faint Mode status bit 5 and the keyword PATTERN for the Chandra and XMM-Newton datasets, respectively. In particular, we removed from the analysis all the events for which the keyword PATTERN is and for MOS, and PN cameras. To remove periods of anomalous count rate, i.e. flares, we followed the prescriptions described in Markevitch’s COOKBOOK 6 and Pratt et al. (2007) for Chandra and XMM-Newton , respectively. For both datasets, we extracted a light curve for each observation and removed from the analysis the time intervals where the count rate exceeds times the mean value. If there were multiple observations of the same objects, these were merged after the processing and cleaning procedures. We list in Table 1 the effective exposure times, after cleaning, for each instrument. Point sources were identified using the CIAO wavdetect tool ( Freeman et al. 2002 ) on and exposure-corrected images. For
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