J/A+A/640/A132ivo://CDS.VizieR/J/A+A/640/A132doi:10.26093/cds/vizier.36400132CDSMAGIC CollaborationAcciari V.A.Ansoldi S.Antonelli L.A.,Arbet Engels A.Baack D.Babic A.Banerjee B.Barres de Almeida U.,Barrio J.A.Becerra Gonzalez J.Bednarek W.Bellizzi L.Bernardini E.,Berti A.Besenrieder J.Bhattacharyya W.Bigongiari C.Biland A.,Blanch O.Bonnoli G.Bosnjak Z.Busetto G.Carosi R.Ceribella G.,Cerruti M.Chai Y.Chilingarian A.Cikota S.Colak S.M.Colin U.,Colombo E.Contreras J.L.Cortina J.Covino S.D'Amico G.D'Elia V.,Da Vela P.Dazzi F.De Angelis A.De Lotto B.Delfino M.Delgado J.,Depaoli D.Di Pierro F.Di Venere L.Do Souto Espineira E.,Dominis Prester D.Donini A.Dorner D.Doro M.Elsaesser D.,Fallah Ramazani V.Fattorini A.Ferrara G.Foano L.Fonseca M.V.,Font L.Fruck C.Fukami S.Garcia Lopez R.J.Garczarczyk M.,Gasparyan S.Gaug M.Giglietto N.Giordano F.Gliwny P.Godinovic N.,Green D.Hadasch D.Hahn A.Herrera J.Hoang J.Hrupec D.Huetten M.,Inada T.Inoue S.Ishio K.Iwamura Y.Jouvin L.Kajiwara Y.,Karjalainen M.Kerszberg D.Kobayashi Y.Kubo H.Kushida J.,Lamastra A.Lelas D.Leone F.Lindfors E.Lombardi S.Longo F.,Lopez M.Lopez-Coto R.Lopez-Oramas A.Loporchio S.,Machado de Oliveira Fraga B.Maggio C.Majumdar P.Makariev M.,Mallamaci M.Maneva G.Manganaro M.Mannheim K.Maraschi L.,Mariotti M.Martinez M.Mazin D.Mender S.Micanovic S.Miceli D.,Miener T.Minev M.Miranda J.M.Mirzoyan R.Molina E.Moralejo A.,Morcuende D.Moreno V.Moretti E.Munar-Adrover P.Neustroev V.,Nigro C.Nilsson K.Ninci D.Nishijima K.Noda K.Nogues L.,Nozaki S.Ohtani Y.Oka T.Otero-Santos J.Palatiello M.Paneque D.,Paoletti R.Paredes J.M.Pavletic L.Penil P.Peresano M.Persic M.,Prada Moroni P.G.Prandini E.Puljak I.Rhode W.Ribo M.Rico J.,Righi C.Rugliancich A.Saha L.Sahakyan N.Saito T.Sakurai S.,Satalecka K.Schleicher B.Schmidt K.Schweizer T.Sitarek J.,Snidaric I.Sobczynska D.Spolon A.Stamerra A.Strom D.Strzys M.,Suda Y.Suric T.Takahashi M.Tavecchio F.Temnikov P.Terzic T.,Teshima M.Torres-Alba N.Tosti L.van Scherpenberg J.Vanzo G.,Vazquez Acosta M.Ventura S.Verguilov V.Vigorito C.F.Vitale V.,Vovk I.Will M.Zaric D.Nievas-Rosillo M.Arcaro C.D'Ammando F.,de Palma F.Hodges M.Hovatta T.Kiehlmann S.Max-Moerbeck W.,Readhead A.C.S.Reeves R.Takalo L.Reinthal R.Jormanainen J.,Wierda F.Wagner S.M.Berdyugin A.Nabizadeh A.Talebpour Sheshvan N.,Oksanen A.Bachev R.Strigachev A.Kehusmaa P.2020-11-26T11:37:12Z2020-08-28T08:01:15ZCDS support team

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

cds-question@unistra.frbl-lacertae-objectsphotometryx-ray-sourcesIt has become evident that one-zone synchrotron self-Compton models are not always adequate for very high-energy (VHE) gamma-ray-emitting blazars. While two-component models perform better, they are difficult to constrain due to the large number of free parameters. In this work, we make a first attempt at taking into account the observational constraints from very long baseline interferometry (VLBI) data, long-term light curves (radio, optical, and X-rays), and optical polarisation to limit the parameter space for a two-component model and test whether or not it can still reproduce the observed spectral energy distribution (SED) of the blazars. We selected five TeV BL Lac objects based on the availability of VHE gamma-ray and optical polarisation data. We collected constraints for the jet parameters from VLBI observations. We evaluated the contributions of the two components to the optical flux by means of decomposition of long-term radio and optical light curves as well as modelling of the optical polarisation variability of the objects. We selected eight epochs for these five objects based on the variability observed at VHE gamma rays, for which we constructed the SEDs that we then modelled with a two-component model. We found parameter sets which can reproduce the broadband SED of the sources in the framework of two-component models considering all available observational constraints from VLBI observations. Moreover, the constraints obtained from the long-term behaviour of the sources in the lower energy bands could be used to determine the region where the emission in each band originates. Finally, we attempt to use optical polarisation data to shed new light on the behaviour of the two components in the optical band. Our observationally constrained two-component model allows explanation of the entire SED from radio to VHE with two co-located emission regions.2020A&A...640A.132Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/640/A132CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/640/A132https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/640/A132http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/640/A132https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/640/A132https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/640/A132http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/640/A132GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/640/A132/table1 (General properties of the selected TeV BL Lacs and the correction coefficients used in optical, UV, and X-ray data analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/640/A132/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/640/A132/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/640/A132/table1?GETtext/xml+votable180.050000true80.4412521.2141670.0055555555555555566/8915 9711 13820 15969 24260https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/640/A132?format=asciiX-raydefaultJ/A+A/640/A132/table1General properties of the selected TeV BL Lacs and the correction coefficients used in optical, UV, and X-ray data analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource namemeta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainl_zLower limit on z based on spectroscopy (Paiano et al., 2017ApJ...837..144P)meta.code.error;src.redshiftcharzRedshiftsrc.redshiftfloatARR-band Galactic extinction (1)magphys.absorption.galfloatNHEquivalent Galactic hydrogen column density (2)1e+21cm**-2phys.columnDensity;pos.galacticfloatrap(ph)Aperture radius for optical photometryarcsecphys.angSize;srcfloatrap(pol)Aperture radius for polarisation observationarcsecphys.angSize;srcfloatFhostphContribution of the host-galaxy flux (R-band) within the aperture for optical photometrymJyphot.flux.density;em.opt.Rfloatn_Fhostph[cbd] Note on Fhostphmeta.notecharFhostpolContribution of the host-galaxy flux (R-band) within the aperture for polarisation observationmJyphot.flux.density;em.opt.Rfloatn_Fhostpol[cbd] Note on Fhostpol (3)meta.notecharlcoptShow the optical R light curvemeta.ref.urlcharlcxShow the Swift-XRT light curvesmeta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/640/A132/tablea2Results of Swift-XRT observationsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameTarget Namemeta.id;meta.maincharMJDModified Julian date (start of observation)dtime.epochdoubleOIDSwift observation IDmeta.id;obsExpTimeExposure timestime.duration;obs.exposureintGamma-PL? Spectral index of power the law modelspect.indexfloatnullablee_Gamma-PL? Spectral index error of the power law modelstat.errorfloatnullableCHI2-PL? Chi^2^ value of the fitted power law modelstat.fit.chi2floatnullableDOF-PL? Degree of the freedom of the fitted power law modelstat.fit.dofintnullableGamma-LP? Spectral index of the logparabola modelspect.indexfloatnullablee_Gamma-LP? Spectral index error of the logparabola modelstat.errorfloatnullableBeta-LP? Curvature parameter of the logparabola modelstat.param;meta.modelledfloatnullablee_Beta-LP? Curvature parameter error of the logparabola modelstat.errorfloatnullableCHI2-LP? Chi^2 value of the fitted logparabola modelstat.fit.chi2floatnullableDOF-LP? Degree of the freedom of the fitted logparabola modelstat.fit.dofintnullablel_ProbLimit flag on Probmeta.code.errorcharProbNull-hypotheses probability of the F-test (1)%statfloatF1X-ray flux in the range of 2-10keV1e-15W.m**-2phot.flux;em.X-ray.mediumfloate_F1X-ray flux error in the range of 2-10keV1e-15W.m**-2stat.errorfloatF2X-ray flux in the range of 0.3-10keV1e-15W.m**-2phot.flux;em.X-ray.mediumfloate_F2X-ray flux error in the range of 0.3-10keV1e-15W.m**-2stat.errorfloatJ/A+A/640/A132/tablea1The optical (R-band) light-curve datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameTaget namemeta.id;meta.maincharJDJulian datedtime.epochdoubleFluxOptical (R-band) fluxmJyphot.flux.density;em.opt.Rfloate_FluxOptical (R-band) flux errormJystat.error;phot.fluxfloat