%0 Journal Article
%T Simultaneous radio-interferometric and high-energy TeV observations of the gamma-ray blazar Mkn 421
%+ Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB)
%+ Observatoire aquitain des sciences de l'univers (OASU)
%+ Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)
%+ Department of Physics [Cork]
%+ Observatoire de Paris - Site de Meudon (OBSPM)
%+ Laboratoire Leprince-Ringuet (LLR)
%+ Laboratoire de Physique Théorique et Astroparticules (LPTA)
%A Charlot, P.
%A Gabuzda, D. C.
%A Sol, H.
%A Degrange, B.
%A Piron, F.
%Z 12 pages, 9 figures, accepted for publication in Astronomy & Astrophysics
%< avec comité de lecture
%@ 0004-6361
%J Astronomy and Astrophysics - A&A
%I EDP Sciences
%V 457
%P 455-465
%8 2006
%D 2006
%Z astro-ph/0607258
%R 10.1051/0004-6361:20054078
%Z Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]Journal articles
%X The 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.
%G English
%L hal-00096030
%U https://hal.science/hal-00096030
%~ IN2P3
%~ OBSPM
%~ INSU
%~ X
%~ LPTA
%~ LLR
%~ CNRS
%~ UNIV-MONTP2
%~ L3AB
%~ X-LLR
%~ X-DEP
%~ X-DEP-PHYS
%~ LORIA2
%~ PSL
%~ UNIV-MONTPELLIER
%~ OBSPM-PSL
%~ UM1-UM2