OBSERVATIONS OF ENERGETIC HIGH MAGNETIC FIELD PULSARS WITH THE<i>FERMI</i>LARGE AREA TELESCOPE

Parent, D.; Kerr, M.; Hartog, P. R. den; Baring, Matthew G.; DeCesar, Megan E.; Espinoza, C. M.; Gotthelf, E. V.; Harding, A. K.; Johnston, S.; Kaspi, V. M.; Livingstone, Margaret A.; Romani, Roger W.; Stappers, B. W.; Watters, K.; Weltevrede, P.; Abdo, A. A.; Burgay, M.; Camilo, F.; Craig, H. A.; Freire, P. C. C.; Giordano, F.; Guillemot, L.; Hobbs, G.; Keith, Michael; Krämer, M.; Lyne, A. G.; Manchester, R. N.; Noutsos, A.; Possenti, A.; Smith, David A.

doi:10.1088/0004-637x/743/2/170

Cited by 37 publications

(44 citation statements)

References 83 publications

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“…In its normal rotation-powered state, PSRJ1119-6127 has a single-peaked pulse profile at 1.4 GHz (Camilo et al 2000) that is aligned with a single-peaked (Gonzalez et al 2005) broad profile in the 0.5-2 keV emission band, which is consistent with thermal emission from the polar cap. In γ-rays, PSRJ1119-6127 also shows a single-peaked profile consistent with outer gap emission (Parent et al 2011). Our observation of multicomponent emission at S-band shortly after the outburst is indicative of a more complex emission geometry and possibly non-dipolar field components near the neutron star surface.…”

Section: Discussionsupporting

confidence: 50%

“…PSRJ1119-6127 was initially discovered in the Parkes multibeam pulsar survey (Camilo et al 2000) and is likely associated with the Galactic supernova remnant G292.2-0.5 (Crawford et al 2001) at a distance of 8.4 kpc (Caswell et al 2004). This pulsar has been detected in X-rays (Gonzalez & Safi-Harb 2003) and gamma-rays (Parent et al 2011), and it is also known to glitch (Weltevrede et al 2011). Unusual pulse profile changes, short radio bursts, and irregular timing recoveries (Weltevrede et al 2011;Antonopoulou et al 2015) have been observed following a glitching event.…”

Section: Introductionmentioning

confidence: 96%

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Post-Outburst Radio Observations of the High Magnetic Field Pulsar PSR J1119-6127

Majid

Pearlman

Dobreva

et al. 2016

ApJL

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We have carried out high-frequency radio observations of the high magnetic field pulsar PSRJ1119-6127 following its recent X-ray outburst. While initial observations showed no evidence of significant radio emission, subsequent observations detected pulsed emission across a large frequency band. In this Letter, we report on the initial disappearance of the pulsed emission and its prompt reactivation and dramatic evolution over several months of observation. The periodic pulse profile at S-band (2.3 GHz) after reactivation exhibits a multi-component emission structure, while the simultaneous X-band (8.4 GHz) profile shows a single emission peak. Single pulses were also detected at S-band near the main emission peaks. We present measurements of the spectral index across a wide frequency bandwidth, which captures the underlying changes in the radio emission profile of the neutron star. The high-frequency radio detection, unusual emission profile, and observed variability suggest similarities with magnetars, which may independently link the high-energy outbursts to magnetar-like behavior.

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Section: Discussionsupporting

confidence: 50%

Section: Introductionmentioning

confidence: 96%

Post-Outburst Radio Observations of the High Magnetic Field Pulsar PSR J1119-6127

Majid

Pearlman

Dobreva

et al. 2016

ApJL

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“…In young radio pulsars like PSR J1119-6127, hard X-ray emission is thought to arise in the context of outer-gap models (e.g., Wang et al 2013) from synchrotron radiation from secondary electron/positron pairs produced by inward propagating curvature radiation γ-rays. As discussed by Parent et al (2011), in PSR J1119-6127, the X-ray/γ-ray phase offset, together with the single-peak morphology of the γ-ray pulse, are well explained in outer-gap models. The luminosity of both the X-ray and γ-ray emission in this picture must be bounded by the spin-down power.…”

Section: Discussionmentioning

confidence: 80%

“…Including the flux from 10 keV extrapolated to the top of the NuSTAR band increases this value by ∼20%. The efficiency for conversion of Ė to Fermi-band γ-ray emission, at least in quiescence, was estimated by Parent et al (2011) to be 0.23. With a comparable amount of energy suddenly appearing in X-rays, the Fermi-band emission may have been affected during this outburst.…”

Section: Discussionmentioning

confidence: 99%

A Magnetar-Like Outburst From a High-B Radio Pulsar

Archibald

Kaspi

Tendulkar

et al. 2016

ApJL

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119

121

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Radio pulsars are believed to have their emission powered by the loss of rotational kinetic energy. By contrast, magnetars show intense X-ray and γ-ray radiation whose luminosity greatly exceeds that due to spin down and magnetar luminosity is believed to be powered by intense internal magnetic fields. A basic prediction of this picture is that radio pulsars of high magnetic field should show magnetar-like emission. Here we report on a magnetar-like X-ray outburst from the radio pulsar PSR J1119-6127, heralded by two short bright X-ray bursts on 2016 July 27 and 28. Using target of opportunity data from the Swift X-ray Telescope and NuSTAR, we show that this pulsar's flux has brightened by a factor of >160 in the 0.5-10 keV band, and that its previously soft X-ray spectrum has undergone a strong hardening with strong pulsations appearing for the first time above 2.5 keV, with phase-averaged emission detectable up to 25 keV. By comparing Swift-XRT and NuSTAR timing data with a preoutburst ephemeris derived from Fermi Large Area Telescope data, we find that the source has contemporaneously undergone a large spin-up glitch of amplitude n n D =´-5.74 8 10 6 ( ) . The collection of phenomena observed thus far in this outburst strongly mirrors those in most magnetar outbursts and provides an unambiguous connection between the radio pulsar and magnetar populations.

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“…No evidence of pulsations was detected above 2.5 keV (Ng et al 2012). Gamma-ray pulsations were reported from PSR J1119-6127 using Fermi, making it the source with the highest inferred B-field detected among γ-ray pulsars (Parent et al 2011).…”

Section: Introductionmentioning

confidence: 89%

PSR J1119–6127 and Its Pulsar Wind Nebula Following the Magnetar-like Bursts

Blumer

Safi‐Harb

McLaughlin

2017

ApJL

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We present a Chandra Director's Discretionary Time observation of PSR J1119-6127 and its compact X-ray pulsar wind nebula (PWN) obtained on 27 October 2016, three months after the Fermi and Swift detection of millisecond bursts in hard X-rays, accompanied by 160 times increase in flux. This magnetar-like activity, the first observed from a rotation-powered radio pulsar, provides an important probe of the physical processes that differentiate radio pulsars from magnetars. The post-burst X-ray spectrum of the pulsar can be described by a single powerlaw model with a photon index of 2.0±0.2 and an unabsorbed flux of 5.7−12 ergs cm −2 s −1 in the 0.5-7.0 keV energy range. At the time of Chandra observations, the pulsar was still brighter by a factor of ∼22 in comparison with its quiescence. The X-ray images reveal a nebula brighter than in the pre-burst Chandra observations (from 2002 and 2004), with an unabsorbed flux of 2.2 +1.1 −0.9 ×10 −13 ergs cm −2 s −1 . This implies a current X-ray efficiency of ≈0.001 at a distance of 8.4 kpc. In addition, a faint torus-like structure is visible along the southeast-northwest direction and a jet-like feature perpendicular to the torus towards the southwest. The PWN is best fitted by an absorbed powerlaw with a photon index of 2.2±0.5 (post-burst). While the pulsar can still be energetically powered by rotation, the observed changes in PSR J1119-6127 and its PWN following the magnetar-like bursts point to an additional source of energy powered by its high-magnetic field.

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OBSERVATIONS OF ENERGETIC HIGH MAGNETIC FIELD PULSARS WITH THEFERMILARGE AREA TELESCOPE

Cited by 37 publications

References 83 publications

Post-Outburst Radio Observations of the High Magnetic Field Pulsar PSR J1119-6127

Post-Outburst Radio Observations of the High Magnetic Field Pulsar PSR J1119-6127

A Magnetar-Like Outburst From a High-B Radio Pulsar

PSR J1119–6127 and Its Pulsar Wind Nebula Following the Magnetar-like Bursts

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