银河系中心附近红化恒星源的毫角秒角分辨率
Milliarcsecond angular resolution of reddened stellar sources in the vicinity of the Galactic Center
摘要：
月球掩星技术第一次被用于近红外甚大望远镜，目的是系统地获得恒星源的毫角秒分辨率。我们已经演示了ISAAC仪器的突发模式，使用检测器的小区域上的快速读出，在几个平方角秒的区域上一次记录几十秒的数据。我们已经利用这个机会记录了大量的LO事件期间，在2006年3月通过月球接近银河系中心。我们已经开发了一个用于处理LO数据的数据管道，包括使用基于小波的方法自动估计主要数据分析参数，以及初步拟合和绘制所有光变曲线。我们在大约四个小时内记录了51个LO事件。其中，30个结果足够的质量，使详细的拟合。我们检测到两个二进制subarcsec投影分离和三个恒星的边缘解决角直径约2 mas。两个以上的SiO脉泽，被发现解决，在一种情况下，我们可以恢复的亮度分布的扩展发射，这是很好地符合光学薄壳。剩余的未分辨星用于表征该方法的性能。超大望远镜的LO技术是一种强大而有效的方法，可以实现当今任何技术中最好的角分辨率、灵敏度和动态范围。目标的选择自然是有限的，联络点是固定时间的事件，但每次观测只需要几分钟，包括间接费用。因此，LO非常适合填补标准观测之间的空闲时间的小间隙。
英文摘要：
For the first time, the lunar occultation technique has been employed on a very large telescope in the near-IR with the aim of achieving systematically milliarcsecond resolution on stellar sources. We have demonstrated the burst mode of the ISAAC instrument, using a fast read-out on a small area of the detector to record many tens of seconds of data at a time on fields of few squared arcsec. We have used the opportunity to record a large number of LO events during a passage of the Moon close to the Galactic Center in March 2006. We have developed a data pipeline for the treatment of LO data, including the automated estimation of the main data analysis parameters using a wavelet-based method, and the preliminary fitting and plotting of all light curves. We recorded 51 LO events over about four hours. Of these, 30 resulted of sufficient quality to enable a detailed fitting. We detected two binaries with subarcsec projected separation and three stars with a marginally resolved angular diameter of about 2 mas. Two more SiO masers, were found to be resolved and in one case we could recover the brightness profile of the extended emission, which is well consistent with an optically thin shell. The remaining unresolved stars were used to characterize the performance of the method. The LO technique at a very large telescope is a powerful and efficient method to achieve angular resolution, sensitivity, and dynamic range that are among the best possible today with any technique. The selection of targets is naturally limited and LOs are fixed-time events, however each observation requires only a few minutes including overheads. As such, LOs are ideally suited to fill small gaps of idle time between standard observations.
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