J/A+A/709/A207ivo://CDS.VizieR/J/A+A/709/A207CDSZangrandi F.Sasaki M.Long K.S.Maggi P.Filipovic M.D.Haberl F.,Kavanagh P.Mayer M.Koribalski B.Maitra C.Points S.,Staveley-Smith L.Jurk K.Smeaton Z.J.Saeedi S.2026-08-19T07:39:06Z2026-04-06T13:53:44ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmagellanic-cloudssupernova-remnantschemical-abundancesx-ray-sourcesSupernova remnants (SNRs) are responsible for the injection of energy and chemical elements into the interstellar medium (ISM). The emission from SNRs can be studied to infer information about the supernova (SN) explosion itself as well as about the properties of the surrounding ISM. Studying a sample of SNRs in a galaxy provides an opportunity to better understand stellar feedback, and the best laboratory for such an investigation is the Large Magellanic Cloud (LMC). The LMC is the nearest star-forming galaxy, it lies outside the Galactic plane line of sight, and therefore its foreground absorption is low. The eROSITA telescopes are the best instruments currently available to perform a survey of the SNRs in the entire LMC due to their large field of view and their high sensitivity towards soft X-rays. We used the sample of SNRs reported in the previous paper and performed a spectral analysis on a part of the sample. We estimated the flux and the luminosity of the fainter sources using the energy conversion factor obtained assuming a non-equilibrium ionisation plasma model. The X-ray luminosity function (XLF) of SNRs in the LMC shows a relatively large number of SNRs at high luminosities. We fitted the distribution with two Gaussian components, which yielded best-fit maxima for the LX[0.3-8.0keV] distribution at m1=10^34.7+/-0.2^erg/s and m2=10^36.5+/-0.4^erg/s. We compared the XLF of the LMC with the XLFs of the Small Magellanic Cloud (SMC), M31, and M33 using a power-law fit and an Anderson-Darling (DA) test. The power indices of the XLFs of the LMC and SMC appear consistent with each other, while those of M33 and M31 are larger. Thus, the latter have steeper power laws, indicating a lower number of X-ray luminous SNRs with respect to the Magellanic Clouds. The DA test showed that the luminosity distributions of SNRs in the SMC and LMC are compatible with being extracted from the same underlying distribution. They are also compatible for different galaxies if we consider the same lower limit for LX [0.3-8.0 keV] for the entire distribution. Finally, we compared the luminosity and the X-ray sizes (diameter) of the SNRs in our sample. We observed a general trend of anti-correlation between size and X-ray luminosity that can be interpreted as a result of fading with time.2026A&A...709A.207Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A207CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/585/A162 : X-ray supernova remnants in LMC (Maggi+, 2016)J/A+A/692/A237 : eROSITA supernova remnant population in LMC (Zangrandi+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A207https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/709/A207http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/709/A207https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/709/A207https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/709/A207http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/709/A207GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/709/A207/tablea1 (Spectral fit parameters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/709/A207/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/709/A207/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/709/A207/tablea1?GETtext/xml+votable180.050000true76.425-67.87472220.005555555555555556Cone search capability for table J/A+A/709/A207/tableb1 (Spectral fit results assuming a single temperature model)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/709/A207/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/709/A207/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/709/A207/tableb1?GETtext/xml+votable180.050000true72.4535417-70.85244440.0055555555555555565/8274 6/33053-33054 33074 33079 33089-33092 33094-33095 33102 33104 33112-33113 33115-33116 33120-33121 33123-33124 33127 33136 37416https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/709/A207?format=asciiX-raydefaultJ/A+A/709/A207/tablea1Spectral fit parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCaCalcium abundance respect to solarphys.abundfloatSimbadSimbad column added by the CDSmeta.ref.urlcharMCSNRName of the SNR using the J2000 coordinatesmeta.id;meta.maincharCompComponent of the model name, compNmeta.code.multipcharNHcolumn density of the LMC in 10^22^cm^-2^1e+22cm**-2phys.columnDensityfloatE_NHUpper error on the column density of the LMC in 10^22^cm^-2^1e+22cm**-2stat.error;stat.maxfloate_NHLower error on the column density of the LMC in 10^22^cm^-2^1e+22cm**-2stat.errorfloatkTTemperature of the plasma in keVkeVphys.temperaturefloatE_kT? Upper error on the temperature of the plasma in keVkeVstat.error;stat.maxfloatnullablee_kT? Lower error on the temperature of the plasma in keVkeVstat.error;phys.energyfloatnullableO? Oxygen abundance respect to solarphys.abundfloatnullablen_OP for Puremeta.notecharE_O? Upper error on the oxygen abundancestat.error;stat.maxfloatnullablen_E_O[e] e for ePOmeta.notechare_O? lower error on the oxygen abundancestat.errorfloatnullablen_e_O[e] e for eMOmeta.notecharNeNeon abundance respect to solarphys.abundfloatE_Ne? Upper error on the neon abundancestat.error;stat.maxfloatnullablee_Ne? Lower error on the neon abundancestat.errorfloatnullableMgMagnesium abundance respect to solarphys.abundfloatSi? Silicium abundance respect to solarphys.abundfloatnullablen_Si[Si ]meta.notecharE_Si? Upper error on the silicium abundancestat.error;stat.maxfloatnullablee_Si? Lower error on the silicium abundancestat.errorfloatnullableSSolfur abundance respect to solarphys.abundfloatE_S? Upper error on the sulfur abundancestat.error;stat.maxfloatnullablen_E_S[e] e for ePSmeta.notechare_S? Lower error on the sulfur abundancestat.errorfloatnullableArArgon abundance respect to solarphys.abundfloatFe? Iron abundance respect to solarphys.abund.Fefloatnullablen_Fe[P] P for Puremeta.notecharE_Fe? Upper error on the iron abundancestat.error;stat.maxfloatnullablee_Fe? Lower error on the iron abundancestat.error;phys.abund.Fefloatnullablel_tauLimit flag on taumeta.code.errorchartauIonization time scale in 10^11^s/cm^3^1e+11s.cm**-3time.scale;phys.atmol.ionizationfloatE_tau? Upper error on the ionization time scale in 10^11^s/cm^3^1e+11s.cm**-3stat.error;stat.maxfloatnullablee_tau? Lower^error on the ionization time scale in 10^11^s/cm^3^1e+11s.cm**-3stat.errorfloatnullableFXUnabsorbed flux of the single component in erg/s/cm^2^ (1)mW.m**-2phot.flux;em.X-rayfloate_FXError on the unabsorbed flux of the single component in erg/s/cm^2^mW.m**-2stat.errorfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainSpDisplay the list of spectrameta.ref.urlcharJ/A+A/709/A207/tableb1Spectral fit results assuming a single temperature modelSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpDisplay the list of spectrameta.ref.urlcharMCSNRName of the SNR using the J2000 coordinatesmeta.id;meta.maincharl_NHLimit flag on NHmeta.code.errorcharNHColumn density of the LMC in 10^22^cm^2^1e+22cm**-2phys.columnDensityfloatE_NH? Upper error on the column density of the LMC in 10^22^cm^2^1e+22cm**-2stat.error;stat.maxfloatnullablee_NH? Lower error on the column density of the LMC in 10^22^cm^2^1e+22cm**-2stat.errorfloatnullablekTTemperature of the plasma in keVkeVphys.temperaturefloatE_kTUpper error on the temperature of the plasma in keVkeVstat.error;stat.maxfloate_kTLower error on the temperature of the plasma in keVkeVstat.error;phys.energyfloatl_tauLimit flag on taumeta.code.errorchartauIonization time scale in 10^11^s/cm^3^1e+11s.cm**3time.scale;phys.atmol.ionizationfloatE_tau? Upper error on the ionization time scale in 10^11^s/cm^3^1e+11s.cm**3stat.error;stat.maxfloatnullablee_tau? Lower error on the ionization time scale in 10^11^s/cm^3^1e+11s.cm**3stat.errorfloatnullableFXAbsorbed flux in erg/s/cm^2^ (1)mW.m**-2phot.flux;em.X-rayfloate_FXError on absorbed flux in erg/s/cm^2^mW.m**-2stat.errorfloatCstatCstat valuestat.fit.paramfloatdofDegree of freedomstat.fit.dofint_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/709/A207/listList of spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMCSNRName of the SNR using the J2000 coordinatesmeta.id;meta.maincharModuleMolule (SNR120, SNR220, SNR320, SNR420 or SNR620)meta.codecharTypeType (ARF, RMF or SourceSpec)meta.codecharFileNameName of the spectrum file in subdirectory spmeta.id;meta.filechar