  We re-analysed numerous archival Chandra X-ray observations of the bright
supernova remnant (SNR) 1E 0102.2-7219 in the Small Magellanic Cloud, to
validate 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. We
find that a blackbody + power-law model is a decent fit, suggestive of a
relatively strong B field and synchrotron radiation, as in a normal young
pulsar, though the thermal luminosity would be unusually high for young
pulsars. Among realistic NS atmosphere models, a carbon atmosphere with B =
10^12 G best fits the observed X-ray spectra. Comparing its unusually high
thermal luminosity (L_{bol} = 1.1^{+1.6}_{-0.5}*10^34 ergs/s) to other NSs, we
find that its luminosity can be explained by the decay of an initially strong
magnetic field (as in magnetars or high B-field pulsars) or by slower cooling
after the supernova explosion. The nature of the NS in this SNR (and of others
in the Magellanic Clouds) could be nicely confirmed by an X-ray telescope with
an angular resolution like Chandra, but superior spectral resolution and
effective area, such as the Lynx concept.
