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tokens: Sky Survey (RASS). For A478 and Ophiuchus, we corrected the MCXC luminosities by factors of 1.34 and 1.25, respectively, to account for the different N H derived from our Chandra fits, which were factors of 2.0 and 1.8 higher than the database values adopted for the RASS catalogs. This makes the luminosities internally consistent with those for the central regions that were derived directly from Chandra observations. For Perseus, even the 0.15 R 500 radius is not fully covered by one Chandra ACIS-I observation, so we used the Chandra mosaic from Aharonian et al. ( 2017 ) to derive the luminosity within 0.15 R 500 . To convert the 0.1–2.4 keV luminosities to the more physically meaningful bolometric ones, we need gas temperatures, which we have derived from Chandra spectral fits in the same regions for most clusters. The temperature fits are summarized in Table 6 ; their errors include the statistical uncertainty and a 10% uncertainty on the value of N H . For Perseus, Ophiuchus, and 2A 0335+096, Chandra coverage is too small to probe an average temperature within R 500 , so we used average cluster temperatures from the literature instead, which come from instruments with a larger field of view (see Table 6 ). For Perseus and Ophiuchus, whose total mass is estimated from the M 500 − T X relation (the 2A 0335+096 mass comes from Planck ), this should result in slightly underestimated masses and R 500 , because the cool core biases the average temperature low. This will not affect our conclusions in any significant way. For a further eight clusters, marked with a in Table 6 , the Chandra field of view is smaller than R 500 but covers enough of it to derive a reliable temperature for the region, considering the steeply declining radial brightness profiles and the relatively small contribution of the missing emission to the spectrum. For these clusters, we use Chandra temperatures fitted in smaller regions given in the notes for Table 6 . For Perseus, for simplicity, we used one ACIS-I pointing (Table 5 ) out of many available to derive a temperature for r 0.15 R 500 , as it almost covers the whole region. The statistics of that data subset are more than sufficient. The above simplifications are adequate because we are using the temperatures only for the luminosity conversion. For each cluster region, we converted the 0.1–2.4 keV luminosities to the bolometric luminosities (Table 6 ) using a conversion factor appropriate for the corresponding temperature (Böhringer et al. 2004 ). The luminosity errors in Table 6 include the uncertainty on the temperature and a 10% ROSAT – Chandra flux cross-calibration uncertainty, added in quadrature. The latter was evaluated by comparing the R 500 0.1–2.4 keV luminosities derived from Chandra and those determined from ROSAT for the 10 clusters in our sample with both the Chandra and the MCXC measurements. We found that our Chandra luminosities are, on average, 6% higher than the RASS ones, with a scatter of ∼10%.