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We re-analysed numerous archival Chandra X-ray observations of the brightsupernova remnant (SNR) 1E 0102.2-7219 in the Small Magellanic Cloud, tovalidate the detection of a neutron star (NS) in the SNR by Vogt et al. (2018).Careful attention to the background is necessary for this spectral analysis. Wefind that a blackbody + power-law model is a decent fit, suggestive of arelatively strong B field and synchrotron radiation, as in a normal youngpulsar, though the thermal luminosity would be unusually high for youngpulsars. Among realistic NS atmosphere models, a carbon atmosphere with B =10^12 G best fits the observed X-ray spectra. Comparing its unusually highthermal luminosity (L_{bol} = 1.1^{+1.6}_{-0.5}*10^34 ergs/s) to other NSs, wefind that its luminosity can be explained by the decay of an initially strongmagnetic field (as in magnetars or high B-field pulsars) or by slower coolingafter the supernova explosion. The nature of the NS in this SNR (and of othersin the Magellanic Clouds) could be nicely confirmed by an X-ray telescope withan angular resolution like Chandra, but superior spectral resolution andeffective area, such as the Lynx concept.

X-ray spectral analysis of the neutron star in SNR 1E 0102.2-7219