Volume 440, Number 2, September III 2005
|Page(s)||693 - 700|
|Section||Stellar structure and evolution|
|Published online||01 September 2005|
The near-UV pulse profile and spectrum of the pulsar PSR B0656+14
Ioffe Physico-Technical Institute, Politekhnicheskaya 26, 194021 St. Petersburg, Russia e-mail: firstname.lastname@example.org
2 Stockholm Observatory, AlbaNova Science Center, Department of Astronomy, 106 91 Stockholm, Sweden
3 Goddard Space Flight Center, Exploration of the Universe Division, Code 667, USA
4 Advanced Computer Concepts, Inc. Potomac, MD, USA
Accepted: 1 June 2005
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 %. The spectral slope of the dereddened phase-integrated spectrum in the ~ Å range is ~ which together with the high pulse fraction indicates a non-thermal origin for the NUV emission. The total flux in the range ~ Å is estimated to be erg s-1 cm-2 when corrected for mag. At a distance of 288 pc this corresponds to a luminosity 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.
Key words: stars: pulsars: individual: PSR B0656+14 / stars: pulsars: individual: PSR J0659+1414
© ESO, 2005
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