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dc.contributor.author
Aleksic, J.
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Ansoldi, S.
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Antonelli, L. A.
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Antoranz, P.
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Babic, A.
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Bangale, P.
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Barres de Almeida, U.
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Barrio, J. A.
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Becerra Gonzalez, J.
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Bednarek, W.
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Bernardini, E.
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Biasuzzi, B.
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Biland, A.
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Blanch, O.
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Boller, A.
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Bonnefoy, S.
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Bonnoli, G.
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Borracci, F.
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Bretz, T.
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Carmona, E.
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Carosi, A.
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Colin, P.
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Colombo, E.
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Contreras, J. L.
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Cortina, J.
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Covino, S.
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Da Vela, P.
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Dazzi, F.
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Pichel, Ana Carolina
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Rovero, Adrian Carlos
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The Veritas Collaboration
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The MAGIC Collaboration
dc.date.available
2017-06-13T13:53:55Z
dc.date.issued
2015-06
dc.identifier.citation
Aleksic, J.; Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Babic, A.; et al.; Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010; Edp Sciences; Astronomy And Astrophysics; 578; 6-2015; A22,1-26
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/18076
dc.description.abstract
Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED).
Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail.
Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E> 100 GeV) γ-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population.
Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2–10 keV band and the VHE γ-ray flux above 200 GeV, consistent with the γ-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE γ-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 × 104<γ< 6 × 105, where γ is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands.
Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (δ, B and R), in addition to the parameters related to the particle population.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Edp Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by/2.5/ar/
dc.subject
Bl Lacertae Objects
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Gamma Rays
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Agn
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Non Thermal Radiation
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Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-06-06T14:48:55Z
dc.journal.volume
578
dc.journal.pagination
A22,1-26
dc.journal.pais
Francia
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dc.journal.ciudad
Paris
dc.description.fil
Fil: Aleksic, J.. IFAE; España
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Fil: Ansoldi, S.. Università di Udine; Italia
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Fil: Antonelli, L. A.. INAF National Institute for Astrophysics; Italia
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Fil: Antoranz, P.. Università di Siena; Italia
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Fil: Babic, A.. University of Rijeka; Croacia
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Fil: Bangale, P.. Max-Planck-Institut für Physik; Alemania
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Fil: Barres de Almeida, U.. Max-Planck-Institut für Physik; Alemania
dc.description.fil
Fil: Barrio, J. A.. Universidad Complutense de Madrid; España
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Fil: Becerra Gonzalez, J.. Inst. de Astrofísica de Canarias; España
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Fil: Bednarek, W.. University of Łódź,; Polonia
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Fil: Bernardini, E.. Deutsches Elektronen-Synchrotron (DESY); Alemania
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Fil: Biasuzzi, B.. Università di Udine; Italia
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Fil: Biland, A.. ETH Zurich; Suiza
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Fil: Blanch, O.. IFAE; España
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Fil: Boller, A.. ETH Zurich; Suiza
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Fil: Bonnefoy, S.. Universidad Complutense de Madrid; España
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Fil: Bonnoli, G.. INAF National Institute for Astrophysics ; Italia
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Fil: Borracci, F.. Max-Planck-Institut für Physik; Alemania
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Fil: Bretz, T.. Universität Würzburg ; Alemania
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Fil: Carmona, E.. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas ; España
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Fil: Carosi, A.. INAF National Institute for Astrophysics; Italia
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Fil: Colin, P.. Max-Planck-Institut für Physik; Alemania
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Fil: Colombo, E.. Inst. de Astrofísica de Canarias; España
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Fil: Contreras, J. L.. Universidad Complutense; España
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Fil: Cortina, J.. IFAE; España
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Fil: Covino, S.. INAF National Institute for Astrophysics; Italia
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Fil: Da Vela, P.. Università di Siena; Italia
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Fil: Dazzi, F.. Max-Planck-Institut für Physik; Alemania
dc.description.fil
Fil: Pichel, Ana Carolina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
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Fil: Rovero, Adrian Carlos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
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Fil: The Veritas Collaboration.
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Fil: The MAGIC Collaboration.
dc.journal.title
Astronomy And Astrophysics
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201424811
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2015/06/aa24811-14/aa24811-14.html
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/1412.3576
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