Notes. Sample of SNRs in the LMC. The columns are the following: (1) MCSNR identifier, in the form “JHHMM−DDMM”. (2) Right ascension of the remnant, in J2000 equinox. (3) Declination in J2000 equinox. (4) Old “common” name used in the literature. (5) Flag coding the type of X-ray data available and used in this work. “X” indicates that XMM-Newton data are present, and “MX” that multiple XMM-Newton observation of the remnant exist. “C” or “R” are used when no XMM-Newton observations are available but Chandra or ROSAT observations were used, respectively. “N” means that no X-ray information was found. (6) L_X, the X-ray luminosity in the 0.3 keV−8 keV band, in units of 10³⁵ erg s^-1, obtained as described in Sect. 7. (7) X-ray size in arcsec. Only the maximal extent is given (corresponding to the diametre in a circularly symmetric case). The number in brackets gives the position angle (PA) of the maximal extent in the non-symmetric case. The PA is measured in degrees, eastwards of north. Size was measured from XMM-Newton images whenever applicable (“X” and “MX” flags). For “C” SNRs, the quoted value is taken from the entry in the Chandra SNR catalogue. For the ROSAT-only SNRs (J0448−6700 and J0455−6839), we used the value quoted in Badenes et al. (2010) and Williams et al. (1999a), respectively. (8) N_H fraction, as defined in Sect. 8. Uncertainties are given at the 90 % C.L. (9) N_OB, the number of blue early-type stars within 100 pc of the remnant (see Sect. 6.2). (10) r, the ratio of CC SNe to thermonuclear SNe expected from the observed distribution of stellar ages in the neighbourhood of the remnant, as obtained by Eq. (2) (see Sect. 6 for details). (11) “Hint-spec”, the number attributed to SNRs as function of spectral results, as described in Sect. 6.3 and Table 7.

Reference. In which the SNR was first published: WM66: Westerlund & Mathewson (1966); MC73: Mathewson & Clarke (1973); LHG81: Long et al. (1981); MFD83: Mathewson et al. (1983); TM84: Turtle & Mills (1984); MFD84: Mathewson et al. (1984); MFT85: Mathewson et al. (1985); CMG83: Chu et al. (1993); SCM94: Smith et al. (1994); CDS95: Chu et al. (1995); CKS97: Chu et al. (1997); BGS06: Blair et al. (2006); KPS10: Klimek et al. (2010); GSH12: Grondin et al. (2012); BFC12a: Bozzetto et al. (2012a); BFC12b: Bozzetto et al. (2012b); DFB12: de Horta et al. (2012); MHB12: Maggi et al. (2012a); KSP13: Kavanagh et al. (2013); BFC13: Bozzetto et al. (2013); MHK14: Maggi et al. (2014); BKM14: Bozzetto et al. (2014); KSB15a: Kavanagh et al. (2015a); KSB15b: Kavanagh et al. (2015c).