2012A&A...544A...3R -
Astronomy and Astrophysics, volume 544A, 3-3 (2012/8-1)
Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026.
ROUSSEAU R., GRONDIN M.-H., VAN ETTEN A., LEMOINE-GOUMARD M., BOGDANOV S., HESSELS J.W.T., KASPI V.M., ARZOUMANIAN Z., CAMILO F., CASANDJIAN J.M., ESPINOZA C.M., JOHNSTON S., LYNE A.G., SMITH D.A., STAPPERS B.W. and CALIANDRO G.A.
Abstract (from CDS):
Since its launch, the Fermi satellite has firmly identified 5 pulsar wind nebulae plus a large number of candidates, all powered by young and energetic pulsars. HESS J1857+026 is a spatially extended γ-ray source detected by H.E.S.S. and classified as a possible pulsar wind nebula candidate powered by PSR J1856+0245. We search for γ-ray pulsations from PSR J1856+0245 and explore the characteristics of its associated pulsar wind nebula.Using a rotational ephemeris obtained from the Lovell telescope at Jodrell Bank Observatory at 1.5GHz, we phase-fold 36 months of γ-ray data acquired by the Large Area Telescope (LAT) aboard Fermi. We also perform a complete γ-ray spectral and morphological analysis.No γ-ray pulsations were detected from PSR J1856+0245. However, significant emission is detected at a position coincident with the TeV source HESS J1857+026. The γ-ray spectrum is well described by a simple power-law with a spectral index of Γ=1.53±0.11stat±0.55syst and an energy flux of G(0.1-100GeV)=(2.71 ±0.52stat±1.51syst)x10–11erg/cm2/s. The γ-ray luminosity is LPWNγ(0.1-100 GeV)=(2.5±0.5stat±1.5syst)x1035((d)/(9kpc))2erg/s, assuming a distance of 9kpc. This implies a γ-ray efficiency of ∼5% for {dot}(E)=4.6x1036erg/s, in the range expected for pulsar wind nebulae. Detailed multi-wavelength modeling provides new constraints on its pulsar wind nebula nature.
Abstract Copyright:
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Journal keyword(s):
pulsars: general - pulsars: individual: PSR J1856+0245 - ISM: individual objects: HESS J1857+026 - gamma rays: general
Simbad objects:
7
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