倾斜源4U 1323-619的新轨道星历：限制到源的距离
New orbital ephemerides for the dipping source 4U 1323-619: constraining the distance to the source
摘要：
4U 1323-619是一个低质量的X射线双星系统，显示出I型X射线爆发和下降。对轨道周期的最准确估计是2.941923（36）小时，并提出了与源的距离低于11千秒差距的建议。我们的目标是获得轨道星历，轨道周期的系统，以及它的衍生物比较观测到的光度与长期演化理论的预测。我们利用了大约26年的X射线数据，并在时间上接近时对选定的观测结果进行了分组。我们折叠光变曲线并使用计时技术，获得12个倾角到达时间。我们用线性和二次函数拟合倾角到达时间的延迟。我们将4U 1323-619定位在以RA（J2000）= 201.6543 \degree和DEC（J2000）= -62.1358 \degree为中心的圆形区域内，相关误差为0.0002 \degree，并证实了文献中已经讨论过的IR对应物的检测。我们估计的轨道周期为P=2.9419156（6）hrs，与文献中的估计一致，但精度高出十倍。我们还首次获得了对轨道周期导数的约束，估计了$\dot{P}=(8\pm 13)\times 10^{-12}$ s/s。假设伴星处于主序下部的热平衡状态，并且是一颗$_{\odot}$为1.4 M的中子星，我们推断伴星的质量为0.28 $\pm$ 0.03 M $_{\odot}$。假设距离为10千秒差距，我们得到了（4.3 $\pm$ 0.5）$\times 10^{36}$ erg s $^{-1}$的光度值，这与长期演化理论的预言不符。利用银河系$_{s}$辐射的三维消光图，在68%的置信水平上，得到了4.2 $^{+0.8}_{-0.7}$ kpc的距离。（节录）
英文摘要：
4U 1323-619 is a low mass X-ray binary system that shows type I X-ray bursts and dips. The most accurate estimation of the orbital period is 2.941923(36) hrs and a distance from the source that is lower than 11 kpc has been proposed. We aim to obtain the orbital ephemeris, the orbital period of the system, as well as its derivative to compare the observed luminosity with that predicted by the theory of secular evolution. We took the advantage of about 26 years of X-ray data and grouped the selected observations when close in time. We folded the light curves and used the timing technique, obtaining 12 dip arrival times. We fit the delays of the dip arrival times both with a linear and a quadratic function. We locate 4U 1323-619 within a circular area centred at RA (J2000)= 201.6543\degree and DEC (J2000)= -62.1358\degree with an associated error of 0.0002\degree, and confirm the detection of the IR counterpart already discussed in literature. We estimate an orbital period of P=2.9419156(6) hrs compatible with the estimations that are present in the literature, but with an accuracy ten times higher. We also obtain a constraint on the orbital period derivative for the first time, estimating $\dot{P}=(8\pm 13)\times 10^{-12}$ s/s. Assuming that the companion star is in thermal equilibrium in the lower main sequence, and is a neutron star of 1.4 M$_{\odot}$, we infer a mass of 0.28$\pm$0.03 M$_{\odot}$ for the companion star. Assuming a distance of 10 kpc, we obtained a luminosity of (4.3$\pm$0.5)$\times 10^{36}$ erg s$^{-1}$, which is not in agreement with what is predicted by the theory of secular evolution. Using a 3D extinction map of the K$_{s}$ radiation in our Galaxy, we obtain a distance of 4.2$^{+0.8}_{-0.7}$ kpc at 68\% confidence level. (Abridged)
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