Abstract

In 2022 we carried out an upgrade of the speckle polarimeter (SPP)—the facility instrument of the 2.5-m telescope of the Caucasian Observatory of the SAI MSU. During the overhaul, CMOS Hamamatsu ORCA-Quest qCMOS C15550-20UP was installed as the main detector, some drawbacks of the previous version of the instrument were eliminated. In this paper, we present a description of the instrument, as well as study some features of the CMOS detector and ways to take them into account in speckle interferometric processing. Quantitative comparison of CMOS and EMCCD in the context of speckle interferometry is performed using numerical simulation of the detection process. Speckle interferometric observations of 25 young variable stars are given as an example of astronomical result. It was found that BM And is a binary system with a separation of 273 mas. The variability of the system is dominated by the brightness variations of the main component. A binary system was also found in NSV 16694 (TYC 120-876-1). The separation of this system is 202 mas.

中文翻译：

---

采用 CMOS 探测器的散斑干涉测量

摘要

2022年，我们对SAI MSU高加索天文台2.5米望远镜的设施仪器——散斑偏振计（SPP）进行了升级。此次大修期间，安装了CMOS Hamamatsu ORCA-Quest qCMOS C15550-20UP作为主探测器，消除了之前版本仪器的一些缺陷。在本文中，我们介绍了该仪器，并研究了 CMOS 探测器的一些特性以及在散斑干涉处理中考虑这些特性的方法。使用检测过程的数值模拟对散斑干涉测量中的 CMOS 和 EMCCD 进行定量比较。给出了 25 颗年轻变星的散斑干涉观测作为天文结果的例子。结果发现，BM And 是一个分离度为 273 mas 的双星系统。系统的可变性主要由主要部件的亮度变化决定。NSV 16694 (TYC 120-876-1) 中也发现了二元系统。该系统的分离度为202 mas。