X-Ray Observations of the Young Pulsar J1357—6429 and Its Pulsar Wind Nebula

Chang, Chulhoon; Pavlov, G. G.; Kargaltsev, Oleg; Shibanov, Yurii A.

doi:10.1088/0004-637x/744/2/81

Cited by 34 publications

(35 citation statements)

References 49 publications

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“…In addition to those obtained from our observations, we collected γ-and X-ray best-fit spectra from the 2PC and papers published afterwards (PSR J1357−6429, Chang et al (2012); J1741−2054, Marelli et al (2014a); J1813−1246, Marelli et al (2014b); J0357+3205, Marelli et al (2013); J2055+2539, Marelli et al (in preparation)). Figure 2 reports the histogram of the Log(F γ /F X ) values for all pulsars, both RL and RQ, detected in the X-rays and with a nonthermal X-ray spectrum.…”

Section: Discussionmentioning

confidence: 99%

Radio-Quiet and Radio-Loud Pulsars: Similar in Gamma-Rays but Different in X-Rays

Marelli

Mignani

Luca

et al. 2015

ApJ

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We present new Chandra and XMM-Newton observations of a sample of eight radio-quiet γ-ray pulsars detected by the Fermi Large Area Telescope. For all eight pulsars we identify the X-ray counterpart, based on the X-ray source localization and the best position obtained from γ-ray pulsar timing. For PSR J2030+4415 we found evidence for a ∼ 10 -long pulsar wind nebula. Our new results consolidate the work from Marelli et al. (2011) and confirm that, on average, the γ-ray-to-X-ray flux ratios (F γ /F X ) of radio-quiet pulsars are higher than for the radio-loud ones. Furthermore, while the F γ /F X distribution features a single peak for the radio-quiet pulsars, the distribution is more dispersed for the radio-loud ones, possibly showing two peaks. We discuss possible implications of these different distributions based on current models for pulsar X-ray emission.

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Section: Discussionmentioning

confidence: 99%

Radio-Quiet and Radio-Loud Pulsars: Similar in Gamma-Rays but Different in X-Rays

Marelli

Mignani

Luca

et al. 2015

ApJ

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“…Deeper X-ray observations (Chang et al 2012;Lemoine-Goumard et al 2011) have firmly established X-ray pulsations with the pulsar period and found the tail-like structure to be extended out to several tens arcseconds from the pulsar. In addition, a fainter extended X-ray emission was detected on a few tens of arcminutes scale (Chang et al 2012;Abramowski et al 2011), showing a plerion-like structure, which is typical of many young pulsars. Finally, periodic pulsations of PSR J1357−6429 were discovered in the GeV range with Fermi (Lemoine-Goumard et al 2011), and an extended source, HESS J1356−645, associated with the pulsar has been found in the TeV range with H.E.S.S.…”

Section: Introductionmentioning

confidence: 97%

Possible optical counterpart of PSR J1357−6429

Danilenko¹,

Kirichenko

Mennickent

et al. 2012

A&A

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Context. PSR J1357−6429 is a Vela-like radio pulsar that has been recently detected in X-rays and γ-rays. It powers a compact taillike X-ray pulsar wind nebula and X-ray-radio plerion associated with an extended TeV source HESS J1356−645. Aims. We present our deep optical observations with the Very Large Telescope to search for an optical counterpart of the pulsar and its nebula. Methods. The observations were carried out using a direct imaging mode in the V, R, and I bands. We also analysed archival X-ray data obtained with Chandra and XMM-Newton. Results. In all three optical bands, we detect a point-like source with V = 27.3 ± 0.3, R = 25.52 ± 0.07, and I = 24.13 ± 0.05, whose position is within the 1σ error circle of the X-ray position of the pulsar, and whose colours are distinct from those of ordinary stars. We consider it as a candidate optical counterpart of the pulsar. If it is indeed the counterpart, its 5σ offset from the radio pulsar position, measured about 9 yr earlier, implies that the transverse velocity of the pulsar is in the range of 1600-2000 km s −1 at the distance of 2-2.5 kpc, making it the fastest moving pulsar known. The direction of the estimated proper motion coincides with the extension of the pulsar's X-ray tail, suggesting that this is a jet. The tentative optical luminosity and efficiency of the pulsar are similar to those of the Vela pulsar, which also supports the optical identification. However, the candidate undergoes an unusually steep dereddened flux increase towards the infrared with a spectral index α ν ∼ 5, that is not typical of optical pulsars. It implies a strong double-knee spectral break in the pulsar emission between the optical and X-rays. The reasons for the spectral steepness are unclear. It may be caused by a nebula knot projected onto the jet and strongly overlapping with the pulsar, as observed for the Crab, where the knot has a significantly steeper spectrum than the pulsar. We find no other signs of the pulsar nebula in the optical. Alternatively, the detected source may be a faint AGN, that has not yet been seen at other wavelengths. Conclusions. The position and peculiar colours of the detected source suggest that it is an optical counterpart of the pulsar. Further high spatial-resolution infrared observations can help to verify its real nature.

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“…XMM-Newton and Chandra X-ray observations have revealed the pulsar X-ray counterpart and the pulsar wind nebula (PWN) containing a tail-like structure extended to several tens of arcseconds from the pulsar and a fainter plerion extended up to a few tens of arcminutes (Esposito et al 2007;Zavlin 2007;Chang et al 2012;Lemoine-Goumard et al 2011). The plerion was detected in the TeV range with the High Energy Stereoscopic System (H.E.S.S.)…”

Section: Introductionmentioning

confidence: 99%

“…Pulsations of J1357 with the pulsar period were discovered in X-rays with XMM-Newton and in the GeV range with Fermi ( Lemoine-Goumard et al 2011;Chang et al 2012). The pulsar X-ray spectrum shows a thermal component originating from the surface of the neutron star (NS) and a non-thermal power-law component describing the pulsar magnetosphere emission (Lemoine-Goumard et al 2011;Chang et al 2012;Danilenko et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Near-infrared observations of PSR J1357−6429

Zyuzin

Zharikov

Shibanov

et al. 2015

Monthly Notices of the Royal Astronomical Society

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PSR J1357−6429 is a young radio pulsar that was detected in X-rays and γ-rays. We present the high spatial resolution near-infrared imaging of the pulsar field in J, H and K s bands obtained with the VLT/NaCo using the Adaptive Optic system. We found a faint source at the most precise pulsar radio position which we propose as the pulsar near-infrared counterpart candidate. It is confidently detected in the J and K s bands, with J = 23.51±0.24 and K s = 21.82±0.25. There is a hint of the source in the H band with an upper limit H > 22.8. The dereddened source fluxes are compatible with the extrapolation of the pulsar X-ray spectrum towards the near-infrared. If the candidate is the true counterpart, by this property PSR J1357−6429 would be similar to the nearby middle-age pulsar PSR B0656+14. In this case, both pulsars demonstrate an unusually high near-infrared efficiency relative to the X-ray efficiency as compared to other pulsars detected in both ranges.

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X-Ray Observations of the Young Pulsar J1357—6429 and Its Pulsar Wind Nebula

Cited by 34 publications

References 49 publications

Radio-Quiet and Radio-Loud Pulsars: Similar in Gamma-Rays but Different in X-Rays

Radio-Quiet and Radio-Loud Pulsars: Similar in Gamma-Rays but Different in X-Rays

Possible optical counterpart of PSR J1357−6429

Near-infrared observations of PSR J1357−6429

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