The near-UV pulse profile and spectrum of the pulsar PSR B0656+14

被引:16
作者
Shibanov, YA
Sollerman, J
Lundqvist, P
Gull, T
Lindler, D
机构
[1] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia
[2] Stockholm Observ, AlbaNova Sci Ctr, Dept Astron, S-10691 Stockholm, Sweden
[3] Adv Comp Concepts Inc, Potomac, MD USA
来源
ASTRONOMY & ASTROPHYSICS | 2005年 / 440卷 / 02期
关键词
stars : pulsars : individual : PSR B0656+14; stars : pulsars : individual : PSR J0659+1414;
D O I
10.1051/0004-6361:20052987
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 similar to 1800-3200 angstrom range is similar to alpha(nu) = 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 similar to 1700-3400 angstrom is estimated to be 3.4 +/- 0.3 x 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 L-NUV = 3.4 x 10(28) 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.
引用
收藏
页码:693 / 700
页数:8
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