Discovery of X-ray Jets in the Microquasar H 1743-322

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dc.creatorCorbel, S.
dc.creatorKaaret, P.
dc.creatorFender, R. P.
dc.creatorTzioumis, A. K.
dc.creatorTomsick, J. A.
dc.creatorOrosz, J. A.
dc.date2005-05-26
dc.date.accessioned2026-07-07T10:27:29Z
dc.date.available2026-07-07T10:27:29Z
dc.descriptionWe report on the formation and evolution of two large-scale, synchrotron-emitting jets from the black hole candidate H 1743-322 following its reactivation in 2003. In November 2003 after the end of its 2003 outburst, we noticed, in observations with the Australia Telescope Compact Array, the presence of a new and variable radio source about 4.6" to the East of H 1743-322, that was later found to move away from H 1743-322. In February 2004, we detected a radio source to the West of H 1743-322, symmetrically placed relative to the Eastern jet. In 2004, follow-up X-ray observations with {\em Chandra} led to the discovery of X-ray emission associated with the two radio sources. This likely indicates that we are witnessing the interaction of relativistic jets from H 1743-322 with the interstellar medium causing in-situ particle acceleration. The spectral energy distribution of the jets during the decay phase is consistent with a classical synchrotron spectrum of a single electron distribution from radio up to X-rays, implying the production of very high energy ($>$ 10 TeV) particles in those jets. We discuss the jet kinematics, highlighting the presence of a significantly relativistic flow in H 1743-322 almost a year after the ejection event.
dc.descriptionAccepted for publication in The Astrophysical Journal. 17 pages, 9 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0505526
dc.identifierhttp://arxiv.org/abs/astro-ph/0505526
dc.identifierAstrophys.J.632:504-513,2005
dc.identifierdoi:10.1086/432499
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/177165
dc.subjectAstrophysics
dc.titleDiscovery of X-ray Jets in the Microquasar H 1743-322
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