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The near-UV pulse profile and spectrum of the pulsar PSR B0656+14
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.
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2005 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 440, 693-700 p.Article in journal (Refereed) Published
Abstract [en]

We have observed the middle-aged pulsar PSR B0656+14 with the prism and the NUV MAMA detector of the Space Telescope Imaging Spectrograph (STIS) to measure the pulsar spectrum and periodic pulsations in the near-ultraviolet (NUV). The pulsations are clearly detected, double-peaked and very similar to the optical pulse profile. The NUV pulsed fraction is 70±12%. The spectral slope of the dereddened phase-integrated spectrum in the ~1800-3200 Å range is ~αν=0.35±0.5 which together with the high pulse fraction indicates a non-thermal origin for the NUV emission. The total flux in the range ~1700-3400 Å is estimated to be 3.4±0.3×10-15 erg s-1 cm-2 when corrected for E(B-V)=0.03 mag. At a distance of 288 pc this corresponds to a luminosity LNUV=3.4×1028 erg s-1 assuming isotropy of the emission. We compare the NUV pulse profile with observations from radio to gamma-rays. The first NUV sub-pulse is in phase with the gamma-ray pulse marginally detected with EGRET, while the second NUV sub-pulse is similar both in shape and in phase with the non-thermal pulse in hard X-rays. This indicates a single origin of the non-thermal emission in the optical-NUV and in the X-rays. This is also supported by the observed NUV spectral slope, which is compatible with a blackbody plus power-law fit extended from the X-ray range, but dominated by the power-law component in most of the NUV range.

Place, publisher, year, edition, pages
2005. Vol. 440, 693-700 p.
Keyword [en]
stars: pulsars: individual: PSR B0656+14, stars: pulsars: individual: PSR J0659+1414
Research subject
URN: urn:nbn:se:su:diva-30942DOI: 10.1051/0004-6361:20052987OAI: diva2:274781
Available from: 2009-11-01 Created: 2009-11-01 Last updated: 2011-02-15Bibliographically approved

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Sollerman, J.Lundqvist, P.
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