J/A+A/684/A127ivo://CDS.VizieR/J/A+A/684/A127doi:10.26093/cds/vizier.36840127CDSAbe S.Abhir J.Acciari V.A.Agudo I.Aniello T.Ansoldi S.,Antonelli L.A.Arbet Engels A.Arcaro C.Artero M.Asano K.Babic A.,Baquero A.Barres de Almeida U.Barrio J.A.Batkovic I.Baxter J.,Becerra Gonzalez J.Bednarek W.Bernardini E.Bernete J.Berti A.,Besenrieder J.Bigongiari C.Biland A.Blanch O.Bonnoli G.Bosnjak Z.,Burelli I.Busetto G.Campoy-Ordaz A.Carosi A.Carosi R.,Carretero-Castrillo M.Castro-Tirado A.J.Ceribella G.Chai Y.,Cifuentes A.Cikota S.Colombo E.Contreras J.L.Cortina J.Covino S.,D'Ammando F.D'Amico G.D'Elia V.Da Vela P.Dazzi F.De Angelis A.,De Lotto B.de Menezes R.Del Popolo A.Delgado J.Delgado Mendez C.,Di Pierro F.Di Venere L.Dominis Prester D.Donini A.Dorner D.,Doro M.Elsaesser D.Emery G.Escudero J.Farina L.Fattorini A.,Foffano L.Font L.Froese S.Fukami S.Fukazawa Y.Garcia Lopez R.J.,Garczarczyk M.Gasparyan S.Gaug M.Giesbrecht Paiva J.G.Giglietto N.,Giordano F.Gliwny P.Godinovic N.Gradetzke T.Grau R.Green D.,Green J.G.Guenther P.Hadasch D.Hahn A.Hassan T.Heckmann L.,Herrera J.Hrupec D.Huetten M.Imazawa R.Inada T.Ishio K.,Jimenez Martinez I.Jormanainen J.Kerszberg D.Kluge G.W.Kobayashi Y.,Kouch P.M.Kubo H.Kushida J.Lainez Lezaun M.Lamastra A.Leone F.,Lindfors E.Linhoff L.Lombardi S.Longo F.Lopez-Coto R.,Lopez-Moya M.Lopez-Oramas A.Loporchio S.Lorini A.,Machado de Oliveira Fraga B.Majumdar P.Makariev M.Maneva G.Mang N.,Manganaro M.Mangano S.Mannheim K.Mariotti M.Martinez M.,Martinez-Chicharro M.Mas-Aguilar A.Mazin D.Menchiari S.Mender S.,Miceli D.Miener T.Miranda J.M.Mirzoyan R.Molero Gonzalez M.,Molina E.Mondal H.A.Moralejo A.Morcuende D.Nakamori T.Nanci C.,Nava L.Neustroev V.Nickel L.Nievas Rosillo M.Nigro C.Nikolic L.,Nilsson K.Nishijima K.Njoh Ekoume T.Noda K.Nozaki S.Ohtani Y.,Okumura A.Otero-Santos J.Paiano S.Palatiello M.Paneque D.,Paoletti R.Paredes J.M.Pavlovic D.Peresano M.Persic M.Pihet M.,Pirola G.Podobnik F.Prada Moroni P.G.Prandini E.Principe G.,Priyadarshi C.Rhode W.Ribo M.Rico J.Righi C.Sahakyan N.Saito T.,Satalecka K.Saturni F.G.Schleicher B.Schmidt K.Schmuckermaier F.,Schubert J.L.Schweizer T.Sciaccaluga A.Sitarek J.Sliusar V.,Sobczynska D.Stamerra A.Striskovic J.Strom D.Strzys M.Suda Y.,Suutarinen S.Tajima H.Takahashi M.Takeishi R.Tavecchio F.,Temnikov P.Terauchi K.Terzic T.Teshima M.Tosti L.Truzzi S.,Tutone A.Ubach S.van Scherpenberg J.Vazquez Acosta M.Ventura S.,Viale I.Vigorito C.F.Vitale V.Vovk I.Walter R.Will M.,Wunderlich C.Yamamoto T.Liodakis I.Jorstad S.G.Gesu L.D.,Donnarumma I.Kim D.E.Marscher A.P.Middei R.Perri M.Puccetti S.,Verrecchia F.Leto C.De La Calle Perez I.Jimenez-Bailon E.Blinov D.,Bourbah I.G.Kiehlmann S.Kontopodis E.Mandarakas N.Skalidis R.,Vervelaki A.Aceituno F.J.Agis-Gonzalez B.Sota A.Sasada M.,Fukazawa Y.Kawabata K.S.Uemura M.Mizuno T.Akitaya H.Casadio C.,Myserlis I.Sievers A.Laehteenmaeki A.Syrjaerinne I.Tornikoski M.,Salome Q.Gurwell M.Keating G.K.Rao R.2024-11-29T20:01:36Z2024-04-11T09:16:32ZCDS support team

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

cds-question@unistra.frbl-lacertae-objectsradio-sourcesx-ray-sourcesgamma-ray-astronomyWe have performed the first broadband study of Mrk 421 from radio to TeV gamma rays with simultaneous measurements of the X-ray polarization from IXPE. The data were collected as part of an extensive multiwavelength campaign carried out between May and June 2022 using MAGIC, Fermi-LAT, NuSTAR, XMM-Newton, Swift, and several optical and radio telescopes to complement IXPE data. During the IXPE exposures, the measured 0.2-1TeV flux was close to the quiescent state and ranged from 25% to 50% of the Crab Nebula without intra-night variability. Throughout the campaign, the very high-energy (VHE) and X-ray emission are positively correlated at a 4{sigma} significance level. The IXPE measurements reveal an X-ray polarization degree that is a factor of 2-5 higher than in the optical/radio bands; that implies an energy-stratified jet in which the VHE photons are emitted co-spatially with the X-rays, in the vicinity of a shock front. The June 2022 observations exhibit a rotation of the X-ray polarization angle. Despite no simultaneous VHE coverage being available during a large fraction of the swing, the Swift-XRT monitoring reveals an X-ray flux increase with a clear spectral hardening. This suggests that flares in high synchrotron peaked blazars can be accompanied by a polarization angle rotation, as observed in some flat spectrum radio quasars. Finally, during the polarization angle rotation, NuSTAR data reveal two contiguous spectral hysteresis loops in opposite directions (clockwise and counterclockwise), implying important changes in the particle acceleration efficiency on approximately hour timescales.2024A&A...684A.127Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/684/A127CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/576/A126 : The 2009 multiwavelength campaign on Mrk421 (Aleksic+, 2015)J/A+A/578/A22 : Mrk421 in March 2010 (Aleksic+, 2015)J/A+A/593/A91 : Mrk 421 multi-wavelength variability, 2007-2009 (Ahnen+, 2016)J/ApJS/248/29 : Simultaneous X-ray & gamma obs. of Mrk421 in 2013J/A+A/655/A89 : Mrk421 multi-instrument observations in 2017 (Acciari+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/684/A127https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/684/A127http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/684/A127https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/684/A127https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/684/A127http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/684/A127GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-rayX-rayRadiodefaultJ/A+A/684/A127/fig1Multiwavelength light curves of Fig.1recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian date centerdtime.epochdoubleFlux/polFlux or polarization degree/anglephot.flux.densitydoublee_Flux/polFlux uncertainty or polarization degree/anglestat.errordoubleEnergyEnergy range or Filterinstr.bandwidthcharInstInstrumentmeta.id;instrcharUnitUnitsmeta.unitcharJ/A+A/684/A127/fig2Multiwavelength SED Fig.2recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFreqFrequency, bin centerHzem.freqdoublenuFnuEnergy fluxmW.m**-2.s**-1phot.flux.densitydoublee_nuFnuEnergy flux lower uncertaintymW.m**-2.s**-1stat.errordoubleE_nuFnuEnergy flux upper uncertaintymW.m**-2.s**-1stat.error;stat.maxdoubleU.L.[0/1] If 1, the 2nd column is a U.L. at 95% C.L.meta.codeintEpochCorresponding epoch of the SED (see paper for details)time.epochcharInstInstrument (1)meta.id;instrcharUnitUnitsmeta.unitcharJ/A+A/684/A127/fig5Multiwavelength light curves of Fig.5UnitUnitsmeta.unitcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian date centerdtime.epochdoubleMJDwidthWidth of time bindtime.intervaldoubleFluxFluxphot.flux.densitydoublee_FluxFlux uncertaintystat.error;phot.fluxdoubleEnergyEnergy rangeinstr.bandwidthcharInstInstrumentmeta.id;instrcharJ/A+A/684/A127/fig7_8*NuSTAR fluxes and spectral indices of Fig.7/8recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian date centerdtime.epochdoubleMJDwidthWidth of time bindtime.intervalfloatFlux3-7keVFlux in 3-7keV bandphot.flux;em.X-raydoublee_Flux3-7keVFlux uncertainty in 3-7keVstat.errordoubleFlux7-30keVFlux in 7-30keV bandphot.flux;em.X-raydoublee_Flux7-30keVFlux uncertainty in 7-30keVstat.errordoubleUnitUnitsmeta.unitcharAlphaIndex of the Log-parabolameta.code;spect.indexfloate_AlphaUncertainty on the index of the Log-parabolastat.error;pos.eq.rafloat