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Title: Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357$-$6429 with Fermi and XMM-Newton

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 (È = 3.1 × 1036 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 wellmore » 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) × 1034 erg s -1, consistent with an 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.« less
Authors:
 [1] ;  [2] ;  [3] ;  [4] ;  [1] ;  [5] ;  [6] ;  [7] ;  [8] ; ;  [8] ;  [4] ;  [4] ;  [9] ;  [4] ;  [10] ;  [11] ;  [5] ;  [12] ;  [7] more »;  [13] ;  [14] ;  [12] « less
  1. Univ. Bordeaux (France)
  2. NASA Marshall Space Flight Center (MSFC), Huntsville, AL (United States)
  3. Univ. Tubingen (Germany)
  4. Australia Telescope National Facility, Epping NSW (Australia)
  5. Cagliari Astronomical Observatory, Capoterra (Italy)
  6. Columbia Univ., New York, NY (United States). Columbia Astrophysics Lab.
  7. Univ. Montpellier II (France). Lab. Univers. et Particules de Monpellier
  8. Max Planck Inst. for Radioastronomy, Bonn (Germany)
  9. Max Planck Inst. for Radioastronomy, Bonn (Germany); Univ. of Manchester (United Kingdom)
  10. SLAC National Accelerator Lab., Menlo Park, CA (United States)
  11. George Mason Univ., Fairfax, VA (United States)
  12. Naval Research Lab. (NRL), Washington, DC (United States)
  13. Univ. of California, Santa Cruz, CA (United States)
  14. Univ. of Manchester (United Kingdom)
Publication Date:
Grant/Contract Number:
AC02-76SF00515
Type:
Accepted Manuscript
Journal Name:
Astronomy and Astrophysics
Additional Journal Information:
Journal Volume: 533; Journal ID: ISSN 0004-6361
Publisher:
EDP Sciences
Research Org:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org:
USDOE
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; gamma rays; pulsars; PSR J1357 / 6429
OSTI Identifier:
1357196