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arXiv · 1709.07562

3xmm j181923.7$-$170616: an x-ray binary with a 408s pulsar

Hao Qiu·Ping Zhou·Wenfei Yu·Xiangdong Li·Xiaojie Xu
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Abstract

We carry out a dedicated study of 3XMM J181923.7$-$170616\ with an approximate pulsation period of 400~s using the XMM-Newton and Swift observations spanning across nine years. We have refined the period of the source to 407.904(7) s (at epoch MJD 57142) and determined a period derivative limit of $\dot{P}{\leq} 5.9\pm 5.4\times 10^{-9} s s^{-1}$ ($1σ$). The source radiates hard, persistent X-ray emission during the observation epochs, which is best described by an absorbed \powerlaw\ model ($Γ\sim 0.2$--0.8) plus faint Fe lines at 6.4 keV and 6.7 keV. The X-ray flux revealed a variation within a factor of 2, along with a spectral hardening as the flux increased. The pulse shape is sinusoid-like and the spectral properties of different phases do not present significant variation. The absorption N$_H$ $\sim 1.3\times 10^{22} cm^{-2}$ is similar to the total Galactic hydrogen column density along the direction, indicating that it is a distant source. A search for the counterpart in optical and near-infrared surveys reveals a low mass K-type giant, while the existence of a Galactic OB supergiant is excluded. A symbiotic X-ray binary is the favored nature of 3XMM J181923.7$-$170616 and can essentially explain the low luminosity of ${2.78\times 10^{34} d_{10}^{2} erg s^{-1}}$, slow pulsation, hard X-ray spectrum, and possible K3~III companion. An alternative explanation of the source is a persistent Be/X-ray binary with a companion star no earlier than B3-type.

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Hao Qiu, Ping Zhou, Wenfei Yu, Xiangdong Li, Xiaojie Xu. 2017-09-22. 3xmm j181923.7$-$170616: an x-ray binary with a 408s pulsar. https://doi.org/10.3847/1538-4357%2Faa8728

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