用差分相位参考法对β Lyrics的线发射区进行海军原型光学干涉仪成像
Navy Prototype Optical Interferometer Imaging of Line Emission Regions of beta Lyrae Using Differential Phase Referencing
摘要：
我们提出了一个实验的结果，图像的相互作用的双星β天琴座与数据从海军原型光学干涉仪（NPOI），使用差分相位技术来纠正的影响的仪器和大气的干涉相位。我们利用的事实是，我们使用的β Lyrics和可见度校准器的视觉原色几乎是未解决的和近中心对称的，因此具有接近零的干涉相位。我们用这个属性来检测和校正的影响，仪器和大气的相位β天琴座，并获得差分相位的通道中包含的Halpha发射线。结合半通道相位与有关线强度的信息，我们恢复了复杂的vibrium和成像的Halpha发射使用标准的无线电干涉测量方法。我们发现，从我们的微分相位技术的结果是一致的，从一个更标准的分析，使用平方维（V^2的）。我们的图像显示了作为轨道相位的函数的相对于连续光中心的H α发射区域的位置，并且表明轨道的长轴沿着p.a.= 248.8+/-1.7度轨道比先前预测的要小，如果我们假设该系统离我们更远，或者恒星连续体对H α通道的贡献比估计的要大，这种差异就可以得到缓解。最后，我们还检测到一个微分相位信号的通道中含有HeI发射线在587.6和706.5nm，与轨道行为不同的Halpha，表明它起源于这个相互作用系统的不同部分。
英文摘要：
We present the results of an experiment to image the interacting binary star beta Lyrae with data from the Navy Prototype Optical Interferometer (NPOI), using a differential phase technique to correct for the effects of the instrument and atmosphere on the interferometer phases. We take advantage of the fact that the visual primary of beta Lyrae and the visibility calibrator we used are both nearly unresolved and nearly centrally symmetric, and consequently have interferometric phases near zero. We used this property to detect and correct for the effects of the instrument and atmosphere on the phases of beta Lyrae and to obtain differential phases in the channel containing the Halpha emission line. Combining the Halpha-channel phases with information about the line strength, we recovered complex visibilities and imaged the Halpha emission using standard radio interferometry methods. We find that the results from our differential phase technique are consistent with those obtained from a more-standard analysis using squared visibilities (V^2's). Our images show the position of the Halpha emitting regions relative to the continuum photocenter as a function of orbital phase and indicate that the major axis of the orbit is oriented along p.a.=248.8+/-1.7 deg. The orbit is smaller than previously predicted, a discrepancy that can be alleviated if we assume that the system is at a larger distance from us, or that the contribution of the stellar continuum to the Halpha channel is larger than estimated. Finally, we also detected a differential phase signal in the channels containing HeI emission lines at 587.6 and 706.5nm, with orbital behavior different from that of the Halpha, indicating that it originates from a different part of this interacting system.
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