Deep Chandra observations of TeV binaries - II. LS 5039

被引:23
作者
Rea, N. [1 ]
Torres, D. F. [1 ,2 ]
Caliandro, G. A. [1 ]
Hadasch, D. [1 ]
van der Klis, M. [3 ]
Jonker, P. G. [4 ,5 ,6 ]
Mendez, M. [7 ]
Sierpowska-Bartosik, A. [8 ]
机构
[1] Fac Ciencies, Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain
[2] ICREA, Barcelona, Spain
[3] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands
[4] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands
[5] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[6] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands
[7] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands
[8] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland
关键词
binaries: general; X-rays: binaries; X-RAY-EMISSION; PULSAR PSR J0218+4232; YOUNG PULSAR; MILLISECOND PULSARS; TIMING OBSERVATIONS; WIND NEBULA; I+61 303; DISCOVERY; VARIABILITY; I+61-DEGREES-303;
D O I
10.1111/j.1365-2966.2011.19148.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report on Chandra observations of the TeV-emitting high-mass X-ray binary LS 5039, for a total exposure of similar to 70 ks, using the ACIS-S camera in continuous clocking mode to search for a possible X-ray pulsar in this system. We did not find any periodic or quasi-periodic signal in the 0.3-0.4 and 0.75-0.9 orbital phases, and in a frequency range of 0.005-175 Hz. We derived an average pulsed fraction 3 sigma upper limit for the presence of a periodic signal of less than or similar to 15 per cent (depending on the frequency and the energy band), the deepest limit ever reached for this object. If the X-ray emission of LS 5039 is due (at least in part) to a rotational powered pulsar, the latter is either spinning faster than similar to 5.6 ms, or having a beam pointing away from our line of sight, or contributing to less than or similar to 15 per cent of the total X-ray emission of the system in the orbital phases we observed.
引用
收藏
页码:1514 / 1521
页数:8
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