VLT observations of the two<i>Fermi</i>pulsars PSR  J1357−6429 and PSR  J1048−5832

Mignani, Roberto; Shearer, A.; Luca, A. De; Moran, Paul; Collins, S.; Marelli, M.

doi:10.1051/0004-6361/201117318

Cited by 22 publications

(55 citation statements)

References 34 publications

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“…The 5σ offset of the source from the pulsar radio interferometric position, which was obtained ≈9 years earlier (Camilo et al 2004), implied a very high pulsar transverse velocity of ≈ 2000d 2.5 km s −1 (Danilenko et al 2012). Similar velocity was obtained by Mignani et al (2011) based on the comparison of the pulsar radio and X-ray positions. However, Kirichenko et al (2015) showed that Camilo et al (2004) underestimated the uncertainties of the pulsar radio position obtained with the Australia Telescope Compact Ar- ray (ATCA) in 2000.…”

Section: Introductionsupporting

confidence: 82%

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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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Section: Introductionsupporting

confidence: 82%

“…The J1357 field was observed in the optical V RI bands with the ESO Very Large Telescope (VLT) in 2009 (Mignani et al 2011;Danilenko et al 2012). Danilenko et al (2012) detected a point source in all these bands within 1σ uncertainties of the pulsar X-ray position and suggested it as a pulsar optical counterpart candidate.…”

Section: Introductionmentioning

confidence: 99%

Near-infrared observations of PSR J1357−6429

Zyuzin

Zharikov

Shibanov

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Another interesting point to mention is that the elongation of the detected X-ray PWN, about 60 • to northeast, may indicate the direction of the pulsar's proper motion (see also Mignani et al 2011). …”

Section: Spatial and Spectral Analysis Of The X-ray Datamentioning

confidence: 99%

“…Recently, Very Large Telescope data were used to search for optical emission from PSR J1357−6429 (Mignani et al 2011). No counterpart was found, and an upper limit of V 27 was determined.…”

Section: Introductionmentioning

confidence: 99%

Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357−6429 withFermiandXMM-Newton

Lemoine‐Goumard

Zavlin

Grondin

et al. 2011

A&A

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Context. Since the launch of the Fermi satellite, the number of known gamma-ray pulsars has increased tenfold. Most gamma-ray detected pulsars are young and energetic, and many are associated with TeV sources. PSR J1357−6429 is a high spin-down power pulsar (Ė = 3.1 × 10 36 erg s −1 ), discovered during the Parkes multibeam survey of the Galactic plane, with significant timing noise typical of very young pulsars. In the very-high-energy domain (E > 100 GeV), H.E.S.S. has reported the detection of the extended source HESS J1356−645 (intrinsic Gaussian width of 12 ) whose centroid lies 7 from PSR J1357−6429. Aims. We search for gamma-and X-ray pulsations from this pulsar, characterize the neutron star emission and explore the environment of PSR J1357−6429. Methods. Using a rotational ephemeris obtained with 74 observations made with the Parkes telescope at 1.4 GHz, we phase-fold more than two years of gamma-ray data acquired by the Large Area Telescope on-board Fermi as well as those collected with XMM-Newton, and perform gamma-ray spectral modeling. Results. Significant gamma-and X-ray pulsations are detected from PSR J1357−6429. The light curve in both bands shows one broad peak. Gamma-ray spectral analysis of the pulsed emission suggests that it is well described by a simple power-law of index 1.5 ± 0.3 stat ± 0.3 syst with an exponential cut-off at 0.8 ± 0.3 stat ± 0.3 syst GeV and an integral photon flux above 100 MeV of (6.5 ± 1.6 stat ± 2.3 syst ) × 10 −8 cm −2 s −1 . The X-ray spectra obtained from the new data provide results consistent with previous work. Upper limits on the gamma-ray emission from its potential pulsar wind nebula (PWN) are also reported. Conclusions. Assuming a distance of 2.4 kpc, the Fermi LAT energy flux yields a gamma-ray luminosity for PSR J1357−6429 of L γ = (2.13 ± 0.25 stat ± 0.83 syst ) × 10 34 erg s −1 , consistent with an L γ ∝ √Ė relationship. The Fermi non-detection of the pulsar wind nebula associated with HESS J1356−645 provides new constraints on the electron population responsible for the extended TeV emission.

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“…A possible detection of J1357 with AGILE at lower γ -ray energies (100 MeV-10 GeV) was reported by Pellizzoni et al (2009). 5 No optical counterpart to the pulsar or its PWN has been detected yet (Mignani et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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

Chang

Pavlov

Kargaltsev

et al. 2011

ApJ

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We observed the young pulsar J1357-6429 with the Chandra and XMM-Newton observatories. The pulsar spectrum fits well a combination of an absorbed power-law model (Γ = 1.7 ± 0.6) and a blackbody model (kT = 140 +60 −40 eV, R ∼ 2 km at the distance of 2.5 kpc). Strong pulsations with pulsed fraction of 42% ± 5%, apparently associated with the thermal component, were detected in 0.3-1.1 keV. Surprisingly, the pulsed fraction at higher energies, 1.1-10 keV, appears to be smaller, 23% ± 4%. The small emitting area of the thermal component either corresponds to a hotter fraction of the neutron star surface or indicates inapplicability of the simplistic blackbody description. The X-ray images also reveal a pulsar wind nebula (PWN) with complex, asymmetric morphology comprised of a brighter, compact PWN surrounded by the fainter, much more extended PWN whose spectral slopes are Γ = 1.3±0.3 and Γ = 1.7 ± 0.2, respectively. The extended PWN with the observed flux of ∼7.5 × 10 −13 erg s −1 cm −2 is a factor of 10 more luminous then the compact PWN. The pulsar and its PWN are located close to the center of the extended TeV source HESS J1356-645, which strongly suggests that the very high energy emission is powered by electrons injected by the pulsar long ago. The X-ray to TeV flux ratio, ∼0.1, is similar to those of other relic PWNe. We found no other viable candidates to power the TeV source. A region of diffuse radio emission, offset from the pulsar toward the center of the TeV source, could be synchrotron emission from the same relic PWN rather than from the supernova remnant.

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VLT observations of the twoFermipulsars PSR J1357−6429 and PSR J1048−5832

Cited by 22 publications

References 34 publications

Near-infrared observations of PSR J1357−6429

Near-infrared observations of PSR J1357−6429

Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357−6429 withFermiandXMM-Newton

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

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