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dc.contributor.authorGallo, E.
dc.contributor.authorPlotkin, Richard
dc.contributor.authorJonker, P.
dc.identifier.citationGallo, E. and Plotkin, R. and Jonker, P. 2014. V4641 Sgr: A candidate precessing microblazar. Monthly Notices of the Royal Astronomical Society: Letters. 438 (1): L41-L45.

The X-ray spectrum of the Galactic X-ray binary V4641 Sgr in outburst has been found to exhibit a remarkably broad emission feature above 4 keV, with inferred equivalent widths up to 2 keV. Such a feature was first detected during the X-ray flaring activity associated with the giant outburst that the source experienced in 1999 September. The extraordinarily large equivalent width line was then ascribed to reflection/reprocessing of fluorescent Fe emission within an extended optically thick outflow enshrouding the binary system as a result of a shortlived, super-Eddington accretion episode. Making use of new and archival X-ray observations, we show here that a similar feature persists over four orders of magnitude in luminosity, down to Eddington ratios as low as log (LX/LEdd)~-4.5, where the existence of an optically thick envelope appears at odds with any viable accretion flow model. Possible interpretations for this highly unusual X-ray spectrum include a blend of Doppler-shifted/boosted Fe lines from unresolved X-ray jets (a la SS433), or, the first Galactic analogue of a blazar spectrum, where the >4 keV emission would correspond to the onset of the inverse Compton hump. This either requires a low-inclination angle of the jet with respect to the line of sight, in agreement with the estimates for the 1999 superluminal jet (ijet <10°). The fast variability of the feature, combined with the high orbital axis inclination (60° <iorb <71°), argue for a rapidly precessing accretion flow around V4641 Sgr, possibly leading to a transient microblazar behaviour. © 2013 The Authors.

dc.publisherOxford Academic
dc.titleV4641 Sgr: A candidate precessing microblazar
dc.typeJournal Article
dcterms.source.titleMonthly Notices of the Royal Astronomical Society: Letters

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

curtin.departmentDepartment of Physics and Astronomy
curtin.accessStatusOpen access

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