J/MNRAS/458/56ivo://CDS.VizieR/J/MNRAS/458/56doi:10.26093/cds/vizier.74580056CDSWierzcholska A.Wagner S.J.2024-08-16T20:16:30Z2017-03-17T13:14:40ZCDS support team

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

cds-question@unistra.frbl-lacertae-objectsgamma-ray-astronomyx-ray-sourcesredshiftedThis work is a summary of the X-ray spectral studies of 29TeV (10^12^eV, tera-electron-volt) {gamma}-ray emitting blazars observed with Swift/XRT, especially focusing on sources for which the X-ray regime allows us to study the low- and the high-energy ends of the particle distribution function. Variability studies require simultaneous coverage, ideally sampling different flux states of each source. This is achieved using X-ray observations by disentangling the high-energy end of the synchrotron emission and the low-energy end of the Compton emission, which are produced by the same electron population. We focused on a sample of 29 TeV {gamma}-ray emitting blazars with the best signal-to-noise X-ray observations collected with Swift/XRT in the energy range 0.3-10keV during 10yr of Swift/XRT operations. We investigate the X-ray spectral shapes and the effects of different corrections for neutral hydrogen absorption and decompose the synchrotron and inverse Compton components. For five sources (3C 66A, S5 0716+714, W Comae, 4C +21.35 and BL Lacertae) a superposition of both components is observed in the X-ray band, permitting simultaneous, time-resolved studies of both ends of the electron distribution. The analysis of multi-epoch observations revealed that the break energy of the X-ray spectrum varies only by a small factor with flux changes. Flux variability is more pronounced in the synchrotron domain (high-energy end of the electron distribution) than in the Compton domain (low-energy end of the electron distribution). The spectral shape of the Compton domain is stable, while the flux of the synchrotron domain is variable. These changes cannot be described by simple variations of the cut-off energy, suggesting that the high-energy end of the electron distribution is not generally well described by cooling only.2016MNRAS.458...56Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/458/56CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/458/56https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/458/56http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/458/56https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/458/56https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/458/56http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/458/56GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/458/56/table1 (Summary of tera-electron-volt blazars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/458/56/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/458/56/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/458/56/table1?GETtext/xml+votable180.050000true3.466667-18.8913890.0055555555555555566/398 615 1700 2295 2414 3023 3431 4255 5423 6018 6647 7038 7518 7548 7570 7896 8374 8915 9003 9612 9711 10605 12973 13705 13820 13927 14751 15969 16447 16796 16806 17843 20141 20624 23134 23835 24027 24260 25132 26131 28083 28138-28139 28492 28517 31663 32261 32345 34209 36058 36342 38797 43603 44247 44908 47014 47375https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/458/56?format=asciiGamma-rayX-raydefaultJ/MNRAS/458/56/table1Summary of tera-electron-volt blazarsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameObject namemeta.id;meta.maincharprimaryr_NameTeV detection reference, in refs.dat filemeta.ref;pos.framecharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainTypeType of blazarsrc.classcharl_zLimit flag on zmeta.code.error;src.redshiftcharz? Redshiftsrc.redshiftfloatnullabler_zRedshift reference, in refs.dat filemeta.ref;pos.framecharFPC? Integrated flux for Swift/XRT observations in PC mode in the energy range 0.3-10keV1e-15W.m**-2phot.flux;em.X-rayfloatnullableExpPC? Exposure for Swift/XRT observations in PC mode in the energy range 0.3-10keVkstime.expofloatnullableSimbadSimbad column added by the CDSmeta.ref.urlcharFPCxExpPC? Product FPC and ExpPC (in 10^-11^erg/cm2)1e-18W.cm**-2phot.flux;em.X-rayfloatnullableFlag[+] + for blazars selected for further detailed studiesmeta.code.errorcharNoteNotemeta.notecharJ/MNRAS/458/56/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.notecharBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notecharJ/MNRAS/458/56/table2Comparison of Galactic column density valuesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameObject Namemeta.id;meta.maincharNHLABNH value provided by Kalberla et al. (2005A&A...440..775K, Cat. VIII/76)1e+20cm**-2phys.columnDensityfloatNHDLNH value provided by Dickey & Lockman (1990ARA&A..28..215D)1e+20cm**-2phys.columnDensityfloatNHH2NH_2_ value provided by Willingale et al. (2013MNRAS.431..394W)1e+20cm**-2phys.columnDensityfloatNHWillNH value provided by Willingale131e+20cm**-2phys.columnDensityfloatNHLPFree? Free NH value obtained with log-parabola model fitted1e+20cm**-2phys.columnDensityfloatnullablee_NHLPFree? rms uncertainty on NHLPFree1e+20cm**-2stat.errorfloatnullableNHPLFree? Free NH value obtained with power-law model fitted1e+20cm**-2phys.columnDensityfloatnullablee_NHPLFree? rms uncertainty on NHPLFree1e+20cm**-2stat.errorfloatnullableNHBPFree? Free NH value obtained with broken power-law model fitted1e+20cm**-2phys.columnDensityfloatnullablee_NHBPFree? rms uncertainty on NHBPFree1e+20cm**-2stat.errorfloatnullableJ/MNRAS/458/56/table3Fit parameters for the log-parabola fits for 29 sourcesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameObject namemeta.id;meta.maincharRefSource of NH value (G1)meta.id;stat.fitcharalpha{alpha} parameterstat.fit.paramfloate_alpharms uncertainty on alphastat.error;pos.eq.rafloatbeta{beta} parameterstat.fit.paramfloate_betarms uncertainty on betastat.errorfloatNlNormalization for the log-parabola fit defined in Section 30.01cm**-2.s**-1.keV**-1stat.fit.paramfloate_Nlrms uncertainty on Nl0.01cm**-2.s**-1.keV**-1stat.errorfloatrchi2Reduced {chi}^2^ valuestat.fit.chi2floatDOFNumber of degrees of freedommeta.numberintJ/MNRAS/458/56/table4Fit parameters for power-law fits for 29 sourcesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameObject namemeta.id;meta.maincharRefSource of NH value (G1)meta.id;stat.fitcharGAMMASpectral indexspect.indexfloate_GAMMArms uncertainty on GAMMAstat.errorfloatNpNormalization for the power-law fit defined in Sect.30.01cm**-2.s**-1.keV**-1stat.fit.paramfloate_Nprms uncertainty on Np0.01cm**-2.s**-1.keV**-1stat.errorfloatrchi2Reduced {chi}^2^ valuestat.fit.chi2floatDOFNumber of degrees of freedommeta.numberintFTest statistics value for F-teststat.fit.goodnessfloatpvalueProbabilitystat.fit.goodnessdoubleModelPreferable model (1)stat.param;meta.modelledcharJ/MNRAS/458/56/table5Fit parameters for broken power-law fits for 5 sourcesDOFNumber of degrees of freedommeta.numberintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameObject namemeta.id;meta.maincharRefSource of NH value (G1)meta.id;stat.fitcharGAMMA1First spectral indexspect.indexfloate_GAMMA1rms uncertainty on GAMMA1stat.errorfloatGAMMA2Second spectral indexspect.indexfloate_GAMMA2rms uncertainty on GAMMA2stat.errorfloatNbNormalization for the power-law fit defined in Sect.30.01cm**-2.s**-1.keV**-1stat.fit.paramfloate_Nbrms uncertainty on Nb0.01cm**-2.s**-1.keV**-1stat.errorfloatEbBreak energy for the broken power-law fit defined in Sect. 3keVem.energyfloate_Ebrms uncertainty on EbkeVstat.errorfloatrchi2Reduced {chi}^2^ valuestat.fit.chi2float