科研之友
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摘要
We report on a similar to 12 hr XMM-Newton observation of the supergiant high-mass X-ray binary (HMXB) IGR J16207-5129. This is only the second soft X-ray (0.4-15 keV, in this case) study of the source since it was discovered by the International Gamma-Ray Astrophysics Laboratory satellite. The average energy spectrum is very similar to those of neutron star HMXBs, being dominated by a highly absorbed power-law component with a photon index of Gamma = 1.15(-0.05)(+0.07). The spectrum also exhibits a soft excess below similar to 2 keV and an iron K alpha emission line at 6.39 +/- 0.03 keV. For the primary power-law component, the column density is (1.19(-0.05)(+0.06)) x 10(23) cm(-2), indicating local absorption, likely from the stellar wind, and placing IGR J16207-5129 in the category of obscured IGR HMXBs. The source exhibits a very high level of variability with an rms noise level of 64% +/- 21% in the 10(-4)-0.05 Hz frequency range. Although the energy spectrum suggests that the system may harbor a neutron star, no pulsations are detected with a 90% confidence upper limit of similar to 2% in a frequency range from similar to 10(-4) to 88 Hz. We discuss similarities between IGR J16207-5129 and other apparently nonpulsating HMXBs, including other IGR HMXBs as well as 4U 2206+54 and 4U 1700-377.
- 出版日期2009-3-20
- 单位中国地震局
