<i>XMM-NEWTON</i>OBSERVATION OF PSR B2224+65 AND ITS JET

Hui, C. Y.; Huang, R. H. H.; Trepl, L.; Tetzlaff, N.; Takata, Jumpei; Wu, E. M. H.; Cheng, K. S.

doi:10.1088/0004-637x/747/1/74

Cited by 33 publications

(33 citation statements)

References 49 publications

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“…We remark that for the Guitar nebula (Hui et al 2012), the pulsar's jet nature of the X-ray linear feature is not proven yet, and the originating SNR is not known so far. Nevertheless, if the feature will be confirmed as a true pulsar's jet, the supernova responsible for the system could already constitute the second example for such an unusual core-collapse episode, similar to the one originating the Lighthouse nebula.…”

Section: Discussionmentioning

confidence: 90%

“…Although observations performed at different epochs confirmed the link between this extended X-ray feature and the pulsar (Johnson & Wang 2010), its nature is still under discussion, and different scenarios, including a truly ballistic jet (Johnson & Wang 2010;Hui et al 2012) or a flow of high-energy electrons diffusing into the ambient magnetic field (Bandiera 2008), have been proposed.…”

Section: Introductionmentioning

confidence: 99%

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The long helical jet of the Lighthouse nebula, IGR J11014-6103

Pavan

Bordas

Puehlhofer

et al. 2014

A&A

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Context. Jets from rotation-powered pulsars so far have only been observed in systems moving subsonically through their ambient medium and/or embedded in their progenitor supernova remnant (SNR). Supersonic runaway pulsars are also expected to produce jets, but they have not been confirmed so far. Aims. We investigated the nature of the jet-like structure associated with the INTEGRAL source IGR J11014-6103 (the "Lighthouse nebula"). The source is a neutron star escaping its parent SNR MSH 11-61A supersonically at a velocity exceeding 1000 km s −1 . Methods. We observed the Lighthouse nebula and its jet-like X-ray structure through dedicated high spatial resolution observations in X-rays (with Chandra) and in the radio band (with ATCA). Results. Our results show that the feature is a true pulsar's jet. It extends highly collimated over 11pc, displays a clear precessionlike modulation, and propagates nearly perpendicular to the system direction of motion, implying that the neutron star's spin axis in IGR J11014-6103 is almost perpendicular to the direction of the kick received during the supernova explosion. Conclusions. Our findings suggest that jets are common to rotation-powered pulsars, and demonstrate that supernovae can impart high kick velocities to misaligned spinning neutron stars, possibly through distinct, exotic, core-collapse mechanisms.

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Section: Discussionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

The long helical jet of the Lighthouse nebula, IGR J11014-6103

Pavan

Bordas

Puehlhofer

et al. 2014

A&A

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“…This scenario has also been proposed (and is still being debated) for the Guitar Nebula (Bandiera 2008;Johnson & Wang 2010;Hui et al 2012). In the case of electrons diffusing into the ambient magnetic field, the existence of additional helices would require the presence of a particular geometry of the ISM magnetic field.…”

Section: Main Jetmentioning

confidence: 99%

“…Gaensler et al 2004;McGowan et al 2006;Kargaltsev & Pavlov 2008), only a few other systems share a geometry similar to the one seen in the Lighthouse Nebula: the Guitar Nebula, powered by PSR B2224+65 (Cordes et al 1993;Chatterjee & Cordes 2002;Johnson & Wang 2010;Hui et al 2012), and possibly the PWN system powered by PSR J1509-5850, for which the presence of a large-scale outflow misaligned to the direction of motion have only very recently been reported (Klingler et al 2016). Similarly to the IGR J11014-6103 case, the Guitar Nebula's pulsar is producing a bright and elongated X-ray jet, extending over ∼1 pc in a direction almost perpendicular to the pulsar direction of motion.…”

Section: Introductionmentioning

confidence: 97%

Closer view of the IGR J11014-6103 outflows

Pavan

Pühlhofer

Bordas

et al. 2016

A&A

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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.

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“…The background-subtracted counts are 68 ± 14 for region 1 and 29 ± 12 for region 2, respectively. In order to better constrain the spectral properties, we followed the method adopted by Johnson & Wang (2010) and Hui et al (2012) to jointly fit individual power-law models for the X-ray spectra of these two regions assuming the column density, N H , does not change significantly along the proper motion direction. Due to low photon statistics in each segment, we then fixed the N H value at 1.8 × 10 21 cm −2 (Stappers et al 2003) in the joint fit.…”

Section: The X-ray Tailmentioning

confidence: 99%

X-ray studies of the black widow pulsar PSR B1957+20

Huang¹,

Kong²,

Takata

et al. 2012

Proc. IAU

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We report on Chandra observations of the black widow pulsar, PSR B1957+20. Evidence for a binary-phase dependence of the X-ray emission from the pulsar is found with a deep observation. The binary-phase resolved spectral analysis reveals non-thermal X-ray emission of PSR B1957+20, confirming the results of previous studies. This suggests that the X-rays are mostly due to intra-binary shock emission which is strongest when the pulsar wind interacts with the ablated material from the companion star. The geometry of the peak emission is determined in our study. The marginal softening of the spectrum of the non-thermal X-ray tail may indicate that particles injected at the termination shock is dominated by synchrotron cooling.

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XMM-NEWTONOBSERVATION OF PSR B2224+65 AND ITS JET

Cited by 33 publications

References 49 publications

The long helical jet of the Lighthouse nebula, IGR J11014-6103

The long helical jet of the Lighthouse nebula, IGR J11014-6103

Closer view of the IGR J11014-6103 outflows

X-ray studies of the black widow pulsar PSR B1957+20

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