Author(s): A. Abdo A., Ackermann M., Ajello M., B. Atwood W., Axelsson M., Baldini L., Ballet J., Barbiellini G., Bruel P., Cognard I., Cohen-Tanugi J., Dumora D., Farnier C., Giebels B., A. Grenier I., Grondin M.-H., Guillemot L., Knodlseder J., Lemoine-Goumard M., Lott B., Nuss E., Parent D., Pelassa V., Pierbattista M., Piron F., Reposeur T., Sanchez D., A. Smith D., Theureau G., Vilchez N.
(Article) Published:
The Astrophysical Journal / The Astrophysical Journal Letters, vol. 699 p.102-107 (2009)
Links openAccess full text : 
Ref HAL: in2p3-00410517_v1
Ref Arxiv: 0906.1217
DOI: 10.1088/0004-637X/699/2/L102
Ref. & Cit.: NASA ADS
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27 citations
Abstract:
We report the discovery of γ-ray pulsations (≥0.1 GeV) from the young radio and X-ray pulsar PSR J0205 + 6449 located in the Galactic supernova remnant 3C 58. Data in the γ-ray band were acquired by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope (formerly GLAST), while the radio rotational ephemeris used to fold γ-rays was obtained using both the Green Bank Telescope and the Lovell telescope at Jodrell Bank. The light curve consists of two peaks separated by 0.49 ± 0.01 ± 0.01 cycles which are aligned with the X-ray peaks. The first γ-ray peak trails the radio pulse by 0.08 ± 0.01 ± 0.01, while its amplitude decreases with increasing energy as for the other γ-ray pulsars. Spectral analysis of the pulsed γ-ray emission suggests a simple power law of index –2.1 ± 0.1 ± 0.2 with an exponential cutoff at 3.0+1.1 –0.7 ± 0.4 GeV. The first uncertainty is statistical and the second is systematic. The integral γ-ray photon flux above 0.1 GeV is (13.7 ± 1.4 ± 3.0) × 10–8 cm–2 s–1, which implies for a distance of 3.2 kpc and assuming a broad fan-like beam a luminosity of 8.3 × 1034 erg s–1 and an efficiency η of 0.3%. Finally, we report a 95% upper limit on the flux of 1.7 × 10–8 cm–2 s–1 for off-pulse emission from the object.
Comments: 7 pages, 1 figure