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tokens: in the Bar regions are primarily on the near side (low fraction), lending support to the foreground location of the Bar. Finally, we compared the populations of SNRs in Local Group galaxies via their X-ray luminosity function. The XLF of SNRs in the SMC, M31, and M33 are relatively homogeneous over all the observed luminosity range, although that of the SMC is flatter. The LMC XLF is remarkable by its prominent bright end. The largest population of SNRs brighter than erg s is found in the LMC (13 SNRs vs. 8 and 7 in M31 and M33, respectively). This is possibly an effect of the lower metallicity in the LMC: massive stars have smaller mass loss rates (less heavy elements to drive stellar winds) and the interaction of SN ejecta with less massive CSM shells produce brighter remnants. The number of SNRs brighter than erg s in the LMC is comparable to that in M31 and M33, likely owing to its high recent SFR and high current type Ia SN rate. The LMC XLF flattens significantly because of incompleteness: many X-ray-faint SNRs have been missed so far, due to the incomplete coverage of the LMC with sensitive X-ray instruments (i.e. Chandra or XMM-Newton ). This work presents the state of the art on X-ray emission of SNRs in the LMC. However, it is clear that the current sample is incomplete, as evidenced by the flattening of the X-ray luminosity function of LMC SNRs (Sect. 7 ). In the last 15 years, new SNRs were confirmed or discovered in the LMC at an almost constant rate (one or few per year), principally using X-ray observations. There is no indication that this trend will stop in the near future, so that more observations of the LMC will increase the sample of SNRs. Nevertheless, the observing time of major observatories is limited and expensive. We conclude this work by offering several strategies to maximise the chance of finding “missing” SNRs: As shown in Sect. 8 , star formation is intensearound the SGS LMC 4, and the edges of the shellabound in SNRs. Many LMC SGS have not been (fully) surveyedby XMM-Newton , for instance (in the notationof Kim et al. 1999 )SGS 3 and 6 in the north, SGS 2 and5 in the west, and SGS 4 in the south. Targeting inparticular SGSs associated to star formation (e.g. withH ii region along the rims) warrants successfulSNR searches. The follow-up observations of X-ray-selected candidates (usually ROSAT sources) with XMM-Newton have been extremely successful. Such programmes should be continued until completion of the list of candidates. Even the ROSAT (targeted) survey of the LMC was not covering the LMC up to its outskirts. To find SNRs in these regions, the future eROSITA survey ( Merloni et al. 2012 ) will be most useful, covering the full sky in the 0.58 keV band. The LMC is located close to the South Ecliptic Pole and will be observed with a deeper exposure than the rest of the sky. Looking for new SNR candidates, especially evolved X-ray-only SNRs, will be of special interest. Even in existing data, some SNRs