Volume 591, July 2016
|Number of page(s)||11|
|Section||Interstellar and circumstellar matter|
|Published online||21 June 2016|
Closer view of the IGR J11014-6103 outflows
Université de Genève, Departement d’Astronomie –
ISDC, chemin d’Écogia
2 Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
3 Max-Planck-Institut für Kernphysik Saupfercheckweg 1, 69117 Heidelberg, Germany
4 Western Sydney University, Locked Bag 1797, Penrith South DC, NSW 1797, Australia
5 Department for Astrophysics, University of Vienna, Türkenschanzstr. 17, 1180 Vienna, Austria
Received: 5 November 2015
Accepted: 5 April 2016
IGR J11014-6103 (also known as the Lighthouse Nebula) is composed of a bow-shock pulsar wind nebula (PWN) and large-scale X-ray jet-like features, all powered by PSR J1101-6101. Previous observations suggest that the jet features stem from a ballistic jet of relativistic particles. In order to confirm the nature of the jet and the counter-jet, we obtained a new deep 250 ks Chandra observation of the Lighthouse Nebula. We performed detailed spatial and spectral analysis of all X-ray components of the system. The X-ray PWN is now better resolved and shows a peculiar morphology resembling the shape of an arrow. The overall helical pattern of the main jet is confirmed. However, there are large deviations from a simple helical model at small and large scales. Significant extended emission is now detected, encompassing the main jet all along its length. The presence of an apparent gap along the main jet at ~50″ distance from the pulsar is confirmed; however, the surrounding extended emission prevents conclusions on the coherence at this position of the jet. The counter-jet is now detected at high statistical significance. In addition, we found two small-scale arcs departing from the pulsar towards the jets. We also looked for possible bow-shock emission due to the pulsar motion, with a short VLT/FORS2 H-α observation. No clear emission is found, most likely because of the contamination from a diffuse nebulosity. The results of our X-ray analysis show that both a ballistic jet scenario and an alternative scenario involving the diffusion of particles along pre-existing interstellar magnetic field lines are able to satisfactorily explain some of the observational evidence, but cannot fully reproduce the observations.
Key words: X-rays: individuals: IGR J11014-6103 / stars: neutron / stars: jets / ISM: jets and outflows / ISM: supernova remnants / supernovae: individual: MSH 11-61A
© ESO, 2016
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