Acciari, V. A.V. A.AcciariAnsoldi, S.S.AnsoldiANTONELLI, Lucio AngeloLucio AngeloANTONELLIAsano, K.K.AsanoBabić, A.A.BabićBanerjee, B.B.BanerjeeBaquero, A.A.Baquerode Almeida, U. BarresU. Barresde AlmeidaBarrio, J. A.J. A.BarrioBecerra González, J.J.Becerra GonzálezBednarek, W.W.BednarekPriyadarshi, C.C.PriyadarshiPuljak, I.I.PuljakRhode, W.W.RhodeRibó, M.M.RibóRico, J.J.RicoRighi, ChiaraChiaraRighiRugliancich, A.A.RugliancichSaha, L.L.SahaSahakyan, N.N.SahakyanBretz, T.T.BretzFruck, C.C.FruckBesenrieder, J.J.BesenriederSaito, T.T.SaitoSakurai, S.S.SakuraiSatalecka, K.K.SataleckaSchleicher, B.B.SchleicherSchmidt, K.K.SchmidtSchweizer, T.T.SchweizerSitarek, J.J.SitarekŠnidarić, I.I.ŠnidarićSobczynska, D.D.SobczynskaFukami, S.S.FukamiBONNOLI, GiacomoGiacomoBONNOLISpolon, A.A.SpolonBhattacharyya, W.W.BhattacharyyaSTAMERRA, AntonioAntonioSTAMERRAStrom, D.D.StromStrzys, M.M.StrzysSuda, Y.Y.SudaSurić, T.T.SurićTakahashi, M.M.TakahashiTAVECCHIO, FabrizioFabrizioTAVECCHIOGarcía López, R. J.R. 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V.FonsecaMazin, D.D.MazinFont, L.L.FontGREEN, JARRED GERSHONJARRED GERSHONGREENGreen, D.D.GreenHadasch, D.D.HadaschHahn, A.A.HahnHeckmann, L.L.HeckmannHerrera, J.J.HerreraHoang, J.J.HoangHrupec, D.D.HrupecHütten, M.M.HüttenZarić, D.D.ZarićMićanović, S.S.MićanovićInada, T.T.InadaInoue, S.S.InoueIshio, K.K.IshioIwamura, Y.Y.IwamuraJormanainen, J.J.JormanainenJouvin, L.L.JouvinKajiwara, Y.Y.KajiwaraKarjalainen, M.M.KarjalainenKerszberg, D.D.KerszbergArbet-Engels, A.A.Arbet-EngelsKobayashi, Y.Y.KobayashiBellizzi, L.L.BellizziKubo, H.H.KuboKushida, J.J.KushidaLAMASTRA, AlessandraAlessandraLAMASTRALelas, D.D.LelasLEONE, FRANCESCOFRANCESCOLEONELindfors, E.E.LindforsLOMBARDI, SaverioSaverioLOMBARDILongo, F.F.LongoBaack, D.D.BaackLópez, M.M.LópezLópez-Coto, R.R.López-CotoMiceli, D.D.MiceliLópez-Oramas, A.A.López-OramasLoporchio, S.S.LoporchioMachado de Oliveira Fraga, B.B.Machado de Oliveira FragaMaggio, C.C.MaggioMajumdar, P.P.MajumdarMiener, T.T.MienerMinev, M.M.MinevBalbo, M.M.BalboMiranda, J. M.J. M.MirandaMirzoyan, R.R.MirzoyanMolina, E.E.MolinaMoralejo, A.A.MoralejoMorcuende, D.D.MorcuendeMoreno, V.V.MorenoMoretti, E.E.MorettiBernardini, E.E.BernardiniMunar-Adrover, P.P.Munar-AdroverNeustroev, V.V.NeustroevBeck, M.M.BeckNigro, C.C.NigroNilsson, K.K.NilssonNinci, D.D.NinciNishijima, K.K.NishijimaNoda, K.K.NodaNozaki, S.S.NozakiOhtani, Y.Y.OhtaniOka, T.T.OkaBernardos, M.M.BernardosOtero-Santos, J.J.Otero-SantosBiederbeck, N.N.BiederbeckPalatiello, M.M.PalatielloPaneque, D.D.PanequePaoletti, R.R.PaolettiParedes, J. M.J. M.ParedesPavletić, L.L.PavletićPeñil, P.P.PeñilPerennes, C.C.PerennesPERSIC, MassimoMassimoPERSICPrada Moroni, P. G.P. G.Prada MoroniBerti, A.A.BertiBiland, A.A.BilandPRANDINI, ELISAELISAPRANDINI2022-03-212022-03-2120210035-8711http://hdl.handle.net/20.500.12386/31730We report a characterization of the multiband flux variability and correlations of the nearby (z = 0.031) blazar Markarian 421 (Mrk 421) using data from Metsähovi, Swift, Fermi-LAT, MAGIC, FACT, and other collaborations and instruments from 2014 November till 2016 June. Mrk 421 did not show any prominent flaring activity, but exhibited periods of historically low activity above 1 TeV (F<SUB>>1 TeV</SUB> < 1.7 × 10<SUP>-12</SUP> ph cm<SUP>-2</SUP> s<SUP>-1</SUP>) and in the 2-10 keV (X-ray) band (F$_{2-10\, \mathrm{keV}}\lt 3.6\times 10^{-11}$ erg cm<SUP>-2</SUP> s<SUP>-1</SUP>), during which the Swift-BAT data suggest an additional spectral component beyond the regular synchrotron emission. The highest flux variability occurs in X-rays and very high-energy (E > 0.1 TeV) γ-rays, which, despite the low activity, show a significant positive correlation with no time lag. The HR<SUB>keV</SUB> and HR<SUB>TeV</SUB> show the harder-when-brighter trend observed in many blazars, but the trend flattens at the highest fluxes, which suggests a change in the processes dominating the blazar variability. Enlarging our data set with data from years 2007 to 2014, we measured a positive correlation between the optical and the GeV emission over a range of about 60 d centred at time lag zero, and a positive correlation between the optical/GeV and the radio emission over a range of about 60 d centred at a time lag of $43^{+9}_{-6}$ d. This observation is consistent with the radio-bright zone being located about 0.2 parsec downstream from the optical/GeV emission regions of the jet. The flux distributions are better described with a lognormal function in most of the energy bands probed, indicating that the variability in Mrk 421 is likely produced by a multiplicative process.STAMPAenArticle10.1093/mnras/staa37272-s2.0-85107947535http://arxiv.org/abs/2012.01348v1https://academic.oup.com/mnras/article/504/1/1427/6027705?login=true2021MNRAS.504.1427AFIS/05 - ASTRONOMIA E ASTROFISICA