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Discovery of pulsations from the pulsar J0205+6449 in SNR 3C 58 with the fermi gamma-ray space telescope
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.ORCID iD: 0000-0002-9769-8016
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
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2009 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, Vol. 699, no 2, L102-L107 p.Article in journal (Refereed) Published
Abstract [en]

We report the discovery of gamma-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 gamma-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 gamma-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 gamma-ray peak trails the radio pulse by 0.08 +/- 0.01 +/- 0.01, while its amplitude decreases with increasing energy as for the other gamma-ray pulsars. Spectral analysis of the pulsed gamma-ray emission suggests a simple power law of index -2.1 +/- 0.1 +/- 0.2 with an exponential cutoff at 3.0(-0.7)(+1.1) +/- 0.4 GeV. The first uncertainty is statistical and the second is systematic. The integral gamma-ray photon flux above 0.1 GeV is (13.7 +/- 1.4 +/- 3.0) x 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 x 10(34) erg s(-1) and an efficiency eta of 0.3%. Finally, we report a 95% upper limit on the flux of 1.7 x 10(-8) cm(-2) s(-1) for off-pulse emission from the object.

Place, publisher, year, edition, pages
2009. Vol. 699, no 2, L102-L107 p.
Keyword [en]
pulsars: general, stars: neutron
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:kth:diva-31951DOI: 10.1088/0004-637X/699/2/L102ISI: 000267372800011ScopusID: 2-s2.0-68949201407OAI: diva2:407482
QC 20110330Available from: 2011-03-30 Created: 2011-03-30 Last updated: 2011-03-30Bibliographically approved

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Conrad, JanRyde, FelixYlinen, Tomi
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