星云气体光谱研究（SING）：仪器设计、组装和校准

IF 2.7 3区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Experimental Astronomy Pub Date : 2024-04-18 DOI:10.1007/s10686-024-09937-9

Bharat Chandra P., Binukumar G. Nair, Shubham Jankiram Ghatul, Shubhangi Jain, S. Sriram, Mahesh Babu S., Rekhesh Mohan, Margarita Safonova, Jayant Murthy, Mikhail Sachkov

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引用次数: 0

摘要

星云气体光谱研究（SING）是一个近紫外线（NUV）低分辨率摄谱仪有效载荷，设计用于从一个稳定的空间平台在 1400 Å - 2700 Å 的 NUV 范围内运行。SING 望远镜的主孔径为 298 毫米，为长狭缝紫外摄谱仪提供光线。SING 的视场为 1^{\circ}\，空间分辨率为 1.33 弧分，中心波长的光谱分辨率为 3.7 Å(\({R\sim 600}\))。SING 采用了一个微通道板（MCP）和一个基于 CMOS 读出的光子计数探测器。该仪器设计用于观测星云、超新星遗迹和星际介质（ISM）等弥散源，以了解它们的化学性质。SING 被联合国外层空间事务厅选中在中国空间站托管。该仪器将按照发射要求进行鉴定测试。本文将介绍该仪器的硬件设计、光学机械组装和校准。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

Spectroscopic Investigation of Nebular Gas (SING): instrument design, assembly and calibration

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Spectroscopic Investigation of Nebular Gas (SING): instrument design, assembly and calibration

The Spectroscopic Investigation of Nebular Gas (SING) is a near-ultraviolet (NUV) low-resolution spectrograph payload designed to operate in the NUV range, 1400 Å – 2700 Å, from a stable space platform. SING telescope has a primary aperture of 298 mm, feeding the light to the long-slit UV spectrograph. SING has a field of view (FOV) of \(1^{\circ }\), achieving a spatial resolution of 1.33 arcminute and spectral resolution of 3.7 Å(\({R\sim 600}\)) at the central wavelength. SING employs a micro-channel plate (MCP) with a CMOS readout-based photon-counting detector. The instrument is designed to observe diffuse sources such as nebulae, supernova remnants, and the interstellar medium (ISM) to understand their chemistry. SING was selected by the United Nations Office for Outer Space Affairs to be hosted on the Chinese Space Station. The instrument will undergo qualification tests as per the launch requirements. In this paper, we describe the hardware design, optomechanical assembly, and calibration of the instrument.

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来源期刊

Experimental Astronomy 地学天文-天文与天体物理

CiteScore

5.30

自引率

3.30%

发文量

审稿时长

6-12 weeks

期刊介绍： Many new instruments for observing astronomical objects at a variety of wavelengths have been and are continually being developed. Furthermore, a vast amount of effort is being put into the development of new techniques for data analysis in order to cope with great streams of data collected by these instruments. Experimental Astronomy acts as a medium for the publication of papers of contemporary scientific interest on astrophysical instrumentation and methods necessary for the conduct of astronomy at all wavelength fields. Experimental Astronomy publishes full-length articles, research letters and reviews on developments in detection techniques, instruments, and data analysis and image processing techniques. Occasional special issues are published, giving an in-depth presentation of the instrumentation and/or analysis connected with specific projects, such as satellite experiments or ground-based telescopes, or of specialized techniques.