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Simultaneous radio-interferometric and high-energy TeV observations of the gamma-ray blazar Mkn 421

hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCHARLOT, P.
hal.structure.identifierDepartment of Physics [Cork]
dc.contributor.authorGABUZDA, D. C.
hal.structure.identifierObservatoire de Paris - Site de Meudon [OBSPM]
dc.contributor.authorSOL, H.
hal.structure.identifierLaboratoire Leprince-Ringuet [LLR]
dc.contributor.authorDEGRANGE, B.
hal.structure.identifierLaboratoire de Physique Théorique et Astroparticules [LPTA]
dc.contributor.authorPIRON, F.
dc.date.created2006
dc.date.issued2006
dc.identifier.issn0004-6361
dc.description.abstractEnThe TeV-emitting BL Lac object Mkn 421 was observed with very long baseline interferometry (VLBI) at three closely-spaced epochs one-month apart in March-April 1998. The source was also monitored at very-high gamma-ray energies (TeV measurements) during the same period in an attempt to search for correlations between TeV variability and the evolution of the radio morphology on parsec scales. While the VLBI maps show no temporal changes in the Mkn 421 VLBI jet, there is strong evidence of complex variability in both the total and polarized fluxes of the VLBI core of Mkn 421 and in its spectrum over the two-month span of our data. The high-energy measurements indicate that the overall TeV activity of the source was rising during this period, with a gamma-ray flare detected just three days prior to our second VLBI observing run. Although no firm correlation can be established, our data suggest that the two phenomena (TeV activity and VLBI core variability) are connected, with the VLBI core at 22 GHz being the self-absorbed radio counterpart of synchrotron self-Compton (SSC) emission at high energies. Based on the size of the VLBI core, we could derive an upper limit of 0.1 pc (3 x 10**17 cm) for the projected size of the SSC zone. This determination is the first model-free estimate of the size of the gamma-ray emitting region in a blazar.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enSimultaneous radio-interferometric and high-energy TeV observations of the gamma-ray blazar Mkn 421
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361:20054078
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxivastro-ph/0607258
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page455-465
bordeaux.volume457
bordeaux.peerReviewedoui
hal.identifierhal-00096030
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00096030v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2006&rft.volume=457&rft.spage=455-465&rft.epage=455-465&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=CHARLOT,%20P.&GABUZDA,%20D.%20C.&SOL,%20H.&DEGRANGE,%20B.&PIRON,%20F.&rft.genre=article


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