Hints for a fast precessing relativistic radio jet in LS I+61·303

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dc.contributor	Universitat de Barcelona
dc.contributor.author	Massi, M.
dc.contributor.author	Ribó Gomis, Marc
dc.contributor.author	Paredes i Poy, Josep Maria
dc.contributor.author	Garrington, S. T.
dc.contributor.author	Peracaula i Bosch, Marta
dc.contributor.author	Martí Ribas, Josep
dc.date	2013-08-01T11:42:52Z
dc.date	2013-08-01T11:42:52Z
dc.date	2004
dc.date	2013-08-01T11:42:52Z
dc.identifier.citation	0004-6361
dc.identifier.citation	511670
dc.identifier.uri	http://hdl.handle.net/2445/45340
dc.format	4 p.
dc.format	application/pdf
dc.language.iso	eng
dc.publisher	Springer Verlag
dc.relation	Versió postprint del document publicat a: http://dx.doi.org/10.1051/0004-6361:20031760
dc.relation	Astronomy and Astrophysics, 2004, vol. 414, num. 1, p. L1-L4
dc.relation	http://dx.doi.org/10.1051/0004-6361:20031760
dc.rights	(c) Springer Verlag, 2004
dc.rights	info:eu-repo/semantics/openAccess
dc.subject	Estels
dc.subject	Estels binaris de raigs X
dc.subject	Radioastronomia
dc.subject	Raigs gamma
dc.subject	Astronomia de raigs gamma
dc.subject	Astrofísica
dc.subject	Stars
dc.subject	X-ray binaries
dc.subject	Radio astronomy
dc.subject	Gamma rays
dc.subject	Gamma ray astronomy
dc.subject	Astrophysics
dc.title	Hints for a fast precessing relativistic radio jet in LS I+61·303
dc.type	info:eu-repo/semantics/article
dc.type	info:eu-repo/semantics/acceptedVersion
dc.description.abstract	Here we discuss two consecutive MERLIN observations of the X-ray binary LS I +61◦303. The first observation shows a double-sided jet extending up to about 200 AU on both sides of a central source. The jet shows a bent S-shaped struct ure similar to the one displayed by the well-known precessing jet of SS 433. The precession suggested in the first MERLIN image becomes evident in the second one, showing a one-sided bent jet significantly rotated with respect to the jet of the day before. We conclude that the derived precession of the relativistic (β=0.6) jet explains puzzling previous VLBI results. Moreover , the fact that the precession is fast could be the explanation of the never understood short term (days) variability of the associated gamma-ray source 2CG 135 + 01 / 3EG J0241 + 6103.

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