Automated Panoramic Photopolarimeter of High Time Resolution of the BTA N1 Focus

IF 1.3 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Astrophysical Bulletin Pub Date : 2023-02-08 DOI:10.1134/S1990341322040083

V. L. Plokhotnichenko, G. M. Beskin, S. V. Karpov, V. S. Shergin, E. P. Gorodovoy, A. G. Gutaev, A. P. Lyubetsky, V. V. Pavlova, V. N. Chernenkov

{"title":"Automated Panoramic Photopolarimeter of High Time Resolution of the BTA N1 Focus","authors":"V. L. Plokhotnichenko, G. M. Beskin, S. V. Karpov, V. S. Shergin, E. P. Gorodovoy, A. G. Gutaev, A. P. Lyubetsky, V. V. Pavlova, V. N. Chernenkov","doi":"10.1134/S1990341322040083","DOIUrl":null,"url":null,"abstract":"<div><div><p><b>Abstract</b>—The design and functions of the main component of the automated complex for the study of astrophysical objects with high time resolution at the 6-m telescope of SAO RAS—a permanently available photopolarimeter installed at the N1 focus of the BTA for alert observations of optical transient sources are described. The device operates in several modes (up to six in perspective)—spectral, polarimetric, photometric, the choice of which is determined after real-time analysis of the image of the object localization area, recorded in the subview with a field of view of <span>\\(2\\mathop .\\limits^\\prime 5 \\times 3'\\)</span>. The radiation from the vicinity of the detected source is transferred to a diaphragm of variable size from <span>\\(10'' \\times 10''\\)</span> to <span>\\(60'' \\times 10''\\)</span> and, depending on its brightness, passed through one of the <span>\\(UBVR\\)</span> filters or dispersed by the Abbe prism, is recorded by the EMCCD with a time resolution of 0.1 s. In this case, it is possible to introduce a double Wollaston prism into the input beam, which ensures the measurement of the object’s linear polarization. To compensate for the rotation of the instrument’s field of view during observations on the balcony of the N1 focus, a turntable is used, the position of which is set by the telescope’s control system. Control of the observation process, selection and change of modes is carried out using a graphical interface. The automatic implementation of these operations is being tested.</p></div></div>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":null,"pages":null},"PeriodicalIF":1.3000,"publicationDate":"2023-02-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astrophysical Bulletin","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1134/S1990341322040083","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}

引用次数: 0

Abstract—The design and functions of the main component of the automated complex for the study of astrophysical objects with high time resolution at the 6-m telescope of SAO RAS—a permanently available photopolarimeter installed at the N1 focus of the BTA for alert observations of optical transient sources are described. The device operates in several modes (up to six in perspective)—spectral, polarimetric, photometric, the choice of which is determined after real-time analysis of the image of the object localization area, recorded in the subview with a field of view of \(2\mathop .\limits^\prime 5 \times 3'\). The radiation from the vicinity of the detected source is transferred to a diaphragm of variable size from \(10'' \times 10''\) to \(60'' \times 10''\) and, depending on its brightness, passed through one of the \(UBVR\) filters or dispersed by the Abbe prism, is recorded by the EMCCD with a time resolution of 0.1 s. In this case, it is possible to introduce a double Wollaston prism into the input beam, which ensures the measurement of the object’s linear polarization. To compensate for the rotation of the instrument’s field of view during observations on the balcony of the N1 focus, a turntable is used, the position of which is set by the telescope’s control system. Control of the observation process, selection and change of modes is carried out using a graphical interface. The automatic implementation of these operations is being tested.

Abstract Image

查看原文

微信好友朋友圈 QQ好友复制链接

本刊更多论文

BTA N1焦高时间分辨率自动全景光偏振仪

摘要:介绍了SAO as 6 m望远镜高时间分辨率天体物理研究自动化系统的主要组成部分的设计和功能，该系统是安装在BTA N1焦点上的永久可用光偏振计，用于光瞬态源的预警观测。该设备可在多种模式下工作(多达六种视角)-光谱，偏振，光度，其中的选择是在对目标定位区域的图像进行实时分析后确定的，该图像记录在具有\(2\mathop .\limits^\prime 5 \times 3'\)视场的子视图中。来自探测源附近的辐射被转移到从\(10'' \times 10''\)到\(60'' \times 10''\)的可变尺寸的膜片上，并根据其亮度，通过\(UBVR\)滤波器之一或被阿贝棱镜分散，由EMCCD以0.1 s的时间分辨率记录下来。在这种情况下，可以在输入光束中引入双沃拉斯顿棱镜，以确保测量物体的线偏振。在N1焦点的阳台上观察时，为了补偿仪器视场的旋转，使用了一个转台，其位置由望远镜的控制系统设置。观察过程的控制，模式的选择和变化是通过图形界面进行的。正在测试这些操作的自动实现。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

求助全文

约1分钟内获得全文去求助

来源期刊

Astrophysical Bulletin 地学天文-天文与天体物理

CiteScore

2.00

自引率

33.30%

发文量

审稿时长

>12 weeks

期刊介绍： Astrophysical Bulletin is an international peer reviewed journal that publishes the results of original research in various areas of modern astronomy and astrophysics, including observational and theoretical astrophysics, physics of the Sun, radio astronomy, stellar astronomy, extragalactic astronomy, cosmology, and astronomy methods and instrumentation.