Direct Measurement of Neutron Star Recoil in the Oxygen‐rich Supernova Remnant Puppis A

Winkler, P. F.; Petre, Robert

doi:10.1086/522101

Cited by 57 publications

(63 citation statements)

References 43 publications

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“…The large offset between RX J0852 and the SNR center requires a high space velocity for the compact object, inherited from a natal kick during the supernova explosion. Indeed, evidence for a large proper motion in good agreement with the expected one (both in direction and in magnitude) has been reported, based on the analysis of multi-epoch Chandra images [36,90].…”

Section: Other Ccos: More Of the Same? The Central Source In Puppis Asupporting

confidence: 66%

Central Compact Objects in Supernova Remnants

Luca¹,

Bassa²,

Wang³

et al. 2008

AIP Conference Proceedings

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Abstract. Central Compact Objects (CCOs) are a handful of soft X-ray sources located close to the centers of Supernova Remnants and supposed to be young, radio-quiet Isolated Neutron Stars (INSs). A clear understanding of their physics would be crucial in order to complete our view of the birth properties of INSs. We will review the phenomenologies of CCOs, underlining the most important, recent results, and we will discuss the possible relationships of such sources with other classes of INSs.

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Section: Other Ccos: More Of the Same? The Central Source In Puppis Asupporting

confidence: 66%

Central Compact Objects in Supernova Remnants

Luca¹,

Bassa²,

Wang³

et al. 2008

AIP Conference Proceedings

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“…As a reference for the RX J0822.0−4300 position we used the Chandra coordinates reported in Winkler & Petre (2007) (Winkler & Petre 2007), obtaining α(J2000) = 08 h 21 m 57.309 s , δ(J2000) = −43 • 00 17. 28.…”

Section: Resultsmentioning

confidence: 99%

Deep optical observations of the central X-ray source in the Puppis A supernova remnant

Mignani¹,

Luca

Mereghetti

et al. 2009

A&A

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Context. X-ray observations revealed a group of radio-silent isolated neutron stars (INSs) at the centre of young supernova remnants (SNRs), dubbed central compact objects or CCOs, with properties different from those of classical rotation-powered pulsars. In at least three cases, evidence points towards CCOs being low-magnetized INSs, born with slow rotation periods, and possibly accreting from a debris disc of material formed out of the supernova event. Understanding the origin of the diversity of the CCOs can shed light on supernova explosion and neutron star formation models. Optical/infrared (IR) observations are crucial to test different CCO interpretations. Aims. The aim of our work is to perform a deep optical investigation of the CCO RX J0822.0−4300 in the Puppis A SNR, one of the most poorly understood in the CCO family. Methods. By using as a reference the Chandra X-ray coordinates of RX J0822.0−4300 we performed deep optical observations in the B, V and I bands with the Very Large Telescope (VLT). Results. We found no candidate optical counterpart within 3σ of the computed Chandra X-ray position down to 5σ limits of B ∼ 27.2, V ∼ 26.9, and I ∼ 25.6, the deepest obtained in the optical band for this source. Conclusions. These limits confirm the non-detection of a companion brighter than an M 5 dwarf. At the same time, they do not constrain optical emission from the neutron star surface, while emission from the magnetosphere would require a spectral break in the optical/IR.

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“…The fastest pulsar with parallax and proper-motion measurements has a velocity of 1100 km s −1 (Chatterjee et al 2005). Although there is evidence for pulsar or compact object velocities in excess of 1100 km s −1 (Hui & Becker 2006;Winkler & Petre 2007), >1000 km s −1 (Ng et al 2011), and >1400 km s −1 (Lovchinsky et al 2011), the velocities implied by an association between PSR J1105-6107 and MSH 11-61A are likely too high.…”

Section: Discussionmentioning

confidence: 96%

Is Igr J11014-6103 a Pulsar With the Highest Known Kick Velocity?

Tomsick

Bodaghee

Rodríguez

et al. 2012

ApJ

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We report on Chandra X-ray and Parkes radio observations of IGR J11014-6103, which is a possible pulsar wind nebula with a complex X-ray morphology and a likely radio counterpart. With the superb angular resolution of Chandra, we find evidence that a portion of the extended emission may be related to a bow shock due to the putative pulsar moving through the interstellar medium. The inferred direction of motion is consistent with IGR J11014-6103 having been born in the event that produced the supernova remnant (SNR) MSH 11-61A. If this association is correct, then previous constraints on the expansion of MSH 11-61A imply a transverse velocity for IGR J11014-6103 of 2400-2900 km s −1 , depending on the SNR model used. This would surpass the kick velocities of any known pulsars and rival or surpass the velocities of any compact objects that are associated with SNRs. While it is important to confirm the nature of the source, our radio pulsation search did not yield a detection.

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Direct Measurement of Neutron Star Recoil in the Oxygen‐rich Supernova Remnant Puppis A

Cited by 57 publications

References 43 publications

Central Compact Objects in Supernova Remnants

Central Compact Objects in Supernova Remnants

Deep optical observations of the central X-ray source in the Puppis A supernova remnant

Is Igr J11014-6103 a Pulsar With the Highest Known Kick Velocity?

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