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000390249 0247_ $$2doi$$a10.1051/0004-6361/201629540
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000390249 0247_ $$2arXiv$$aarXiv:1612.09472
000390249 0247_ $$2WOS$$aWOS:000406619100031
000390249 0247_ $$2datacite_doi$$a10.3204/PUBDB-2017-09408
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000390249 037__ $$aPUBDB-2017-09408
000390249 041__ $$aEnglish
000390249 082__ $$a520
000390249 0881_ $$aarXiv:1612.09472
000390249 088__ $$2arXiv$$aarXiv:1612.09472
000390249 1001_ $$aAhnen, M. L.$$b0
000390249 245__ $$aMultiband variability studies and novel broadband SED modeling of Mrk 501 in 2009
000390249 260__ $$aLes Ulis$$bEDP Sciences$$c2017
000390249 3367_ $$2DRIVER$$aarticle
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000390249 3367_ $$00$$2EndNote$$aJournal Article
000390249 500__ $$a © ESO
000390249 520__ $$aWe present an extensive study of the BL Lac object Mrk 501 based on a data set collected during the multi-instrument campaign spanning from 2009 March 15 to 2009 August 1, which includes, among other instruments, MAGIC, VERITAS, Whipple 10 m, and Fermi-LAT to cover the γ-ray range from 0.1 GeV to 20 TeV; RXTE and Swift to cover wavelengths from UV tohard X-rays; and GASP-WEBT, which provides coverage of radio and optical wavelengths. Optical polarization measurements were provided for a fraction of the campaign by the Steward and St. Petersburg observatories. We evaluate the variability of the source and interband correlations, the γ-ray flaring activity occurring in May 2009, and interpret the results within two synchrotron self-Compton (SSC) scenarios. Aims. The multiband variability observed during the full campaign is addressed in terms of the fractional variability, and the possible correlations are studied by calculating the discrete correlation function for each pair of energy bands where the significance was evaluated with dedicated Monte Carlo simulations. The space of SSC model parameters is probed following a dedicated grid-scan strategy, allowing for a wide range of models to be tested and offering a study of the degeneracy of model-to-data agreement in the individual model parameters, hence providing a less biased interpretation than the “single-curve SSC model adjustment” typically reported in the literature. Methods. We find an increase in the fractional variability with energy, while no significant interband correlations of flux changes are found on the basis of the acquired data set. The SSC model grid-scan shows that the flaring activity around May 22 cannot be modeled adequately with a one-zone SSC scenario (using an electron energy distribution with two breaks), while it can be suitably described within a two (independent) zone SSC scenario. Here, one zone is responsible for the quiescent emission from the averaged 4.5-month observing period, while the other one, which is spatially separated from the first, dominates the flaring emission occurring at X-rays and very-high-energy (>100 GeV, VHE) γ rays. The flaring activity from May 1, which coincides with a rotation of the electric vector polarization angle (EVPA), cannot be satisfactorily reproduced by either a one-zone or a two-independent-zone SSC model, yet this is partially affected by the lack of strictly simultaneous observations and the presence of large flux changes on sub-hour timescales (detected at VHE γ rays). Results. The higher variability in the VHE emission and lack of correlation with the X-ray emission indicate that, at least during the 4.5-month observing campaign in 2009, the highest energy (and most variable) electrons that are responsible for the VHE γ rays do not make a dominant contribution to the ~1 keV emission. Alternatively, there could be a very variable component contributing to the VHE γ-ray emission in addition to that coming from the SSC scenario. The studies with our dedicated SSC grid-scan show that there is some degeneracy in both the one-zone and the two-zone SSC scenarios probed, with several combinations of model parameters yielding a similar model-to-data agreement, and some parameters better constrained than others. The observed γ-ray flaring activity, with the EVPA rotation coincident with the first γ-ray flare, resembles those reported previously for low frequency peaked blazars, hence suggesting that there are many similarities in the flaring mechanisms of blazars with different jet properties.
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000390249 7001_ $$aAnsoldi, S.$$b1
000390249 7001_ $$aAntonelli, L. A.$$b2
000390249 7001_ $$aAntoranz, P.$$b3
000390249 7001_ $$aBabic, A.$$b4
000390249 7001_ $$aBanerjee, B.$$b5
000390249 7001_ $$aBangale, P.$$b6
000390249 7001_ $$aBarres de Almeida, U.$$b7
000390249 7001_ $$aBarrio, J. A.$$b8
000390249 7001_ $$aBecerra González, J.$$b9
000390249 7001_ $$aBednarek, W.$$b10
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000390249 7001_ $$aBerti, A.$$b12
000390249 7001_ $$aBiasuzzi, B.$$b13
000390249 7001_ $$aBiland, A.$$b14
000390249 7001_ $$aBlanch, O.$$b15
000390249 7001_ $$aBonnefoy, S.$$b16
000390249 7001_ $$aBonnoli, G.$$b17
000390249 7001_ $$aBorracci, F.$$b18
000390249 7001_ $$aBretz, T.$$b19
000390249 7001_ $$aBuson, S.$$b20
000390249 7001_ $$aCarosi, A.$$b21
000390249 7001_ $$aChatterjee, A.$$b22
000390249 7001_ $$aClavero, R.$$b23
000390249 7001_ $$aColin, P.$$b24
000390249 7001_ $$aColombo, E.$$b25
000390249 7001_ $$aContreras, J. L.$$b26
000390249 7001_ $$aCortina, J.$$b27
000390249 7001_ $$aCovino, S.$$b28
000390249 7001_ $$aDa Vela, P.$$b29
000390249 7001_ $$aDazzi, F.$$b30
000390249 7001_ $$aDe Angelis, A.$$b31
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000390249 7001_ $$ade Oña Wilhelmi, E.$$b33
000390249 7001_ $$aDi Pierro, F.$$b34
000390249 7001_ $$0P:(DE-HGF)0$$aDoert, M.$$b35$$eCorresponding author
000390249 7001_ $$aDomínguez, A.$$b36
000390249 7001_ $$aDominis Prester, D.$$b37
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000390249 7001_ $$aDoro, M.$$b39
000390249 7001_ $$aEinecke, S.$$b40
000390249 7001_ $$aEisenacher Glawion, D.$$b41
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000390249 7001_ $$aFruck, C.$$b50
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000390249 7001_ $$aMaraschi, L.$$b87
000390249 7001_ $$aMarcote, B.$$b88
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000390249 7001_ $$0P:(DE-HGF)0$$aPaneque, D.$$b109$$eCorresponding author
000390249 7001_ $$aPaoletti, R.$$b110
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000390249 7001_ $$aShore, S. N.$$b131
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000390249 7001_ $$aKovalev, Yu. A.$$b271
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000390249 7001_ $$aPushkarev, A. B.$$b273
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000390249 7001_ $$aSokolovsky, K. V.$$b275
000390249 7001_ $$aKadler, M.$$b276
000390249 7001_ $$aPiner, G.$$b277
000390249 7001_ $$aLähteenmäki, A.$$b278
000390249 7001_ $$aTornikoski, M.$$b279
000390249 7001_ $$aAngelakis, E.$$b280
000390249 7001_ $$aKrichbaum, T. P.$$b281
000390249 7001_ $$aNestoras, I.$$b282
000390249 7001_ $$aFuhrmann, L.$$b283
000390249 7001_ $$aZensus, J. A.$$b284
000390249 7001_ $$aCassaro, P.$$b285
000390249 7001_ $$aOrlati, A.$$b286
000390249 7001_ $$aMaccaferri, G.$$b287
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000390249 7001_ $$aGiroletti, M.$$b289
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000390249 7001_ $$0P:(DE-HGF)0$$aMAGIC Collaboration$$b293$$eCollaboration author
000390249 7001_ $$0P:(DE-HGF)0$$aVERITAS Collaboration$$b294$$eCollaboration author
000390249 773__ $$0PERI:(DE-600)1458466-9$$a10.1051/0004-6361/201629540$$gVol. 603, p. A31 -$$pA31$$tAstronomy and astrophysics$$v603$$x1432-0746$$y2017
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