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tokens: uncertain by an order of magnitude. Zane et al. ( 2011 ) performed the first detailed analysis of its spectrum. Among numerous fits tried by the authors, only those with the interstellar hydrogen column density N H fixed to the Galactic value 2.7 × 10 20 cm −2 gave an acceptable reduced chi-square statistic and a reasonable distance (other fits gave distances down to 175 pc, too large N H and tiny emitting area). A fit with a two-temperature atmosphere model (2NSA) gave eV/ eV, with radius of the cold component fixed at the realistic value R = 12 km. This fit gave L ∞ ∼ 6 × 10 32 erg s −1 at d ≈ 1.55 kpc. Other acceptable fits indicated d in the range from ∼1 kpc to ≈2.25 kpc. The values of the unabsorbed flux for various statistically acceptable fits implied L ∞ ranging from 5.5 × 10 32 to 9.2 × 10 32 erg s −1 , assuming d = 2 kpc. Shibanov et al. ( 2016 ) fitted the XMM–Newton and Chandra data using nsmax models of magnetized hydrogen atmospheres covering the entire surface, assuming a centred dipole field and the ensuing temperature distribution. They found that an additional absorption feature at energy E abs = 740 ± 30 eV improved the fit. In this case, the best-fitting model yields T ∞ = 1.18 ± 0.05 MK. The resulting normalization (the effective emitting radius) can be reconciled with R = 12 km (assumed in the nsmax model) at d ∼ 4 kpc. The corresponding luminosity is L ∞ = (3.0 ± 0.5) × 10 33 erg s −1 . Other fits, performed for different data sets with or without involving the absorption, are only slightly worse statistically. They yield T ∞ from 0.79 ± 0.03 MK to MK, corresponding to L ∞ ∼ 5 × (10 32 − 10 33 ) erg s −1 . Bogdanov et al. ( 2019 ) have performed an analysis of the spectrum obtained with NICER . They fixed d = 2 kpc and obtained k B T ∞ = 205 ± 3 eV, km ( erg s −1 ) for a BB plus power-law (BB+PL) fit with an absorption at E abs = 780 ± 20 eV. An alternative fit including a Gaussian absorption at E abs = 760 ± 10 eV and two BB components (the G2BB fit) gives eV, km, totalling to L ∞ = (5.4 ± 0.6) × 10 32 erg s −1 . The ranges of L ∞ and T ∞ in Table 2 cover the results obtained by Bogdanov et al. ( 2019 ) and by Shibanov et al. ( 2016 ) for the different instruments. 7. CXOU J160103.1–513353 is a CCO in the SNR G330.2+1.0. Proper motion of the SNR fragments indicates an age of 0.8–1 kyr, if one neglects deceleration; because of deceleration the actual age should be smaller (Borkowski et al. 2018 ; Williams et al. 2018 ). McClure-Griffiths et al. ( 2001 ) derived the minimum distance to this SNR of d = 4.9 ± 0.3 kpc from the observed velocities in the absorption spectrum; a hypothetical maximum distance is d 9.9 kpc. The X-ray spectrum of the CCO is well described with either single-component carbon or two-component hydrogen atmosphere models (Doroshenko, Suleimanov Santangelo 2018 ). In the latter case, the observed spectrum is dominated by the emission from a hot component with a temperature ∼3.9 MK, corresponding to