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题名:
抚仙湖一米新真空太阳望远镜空间二维偏振光谱观测模式设计与实现
其他题名: The Design and Implementation of Spectropolarimetric Observation Mode at 1-Meter New Vacuum Solar Telescope
作者: 陈宇超1,2; 徐稚2; 李正刚2; 袁沭2; 柳光乾2; 许骏2; 金振宇2
刊名: 天文研究与技术( Astronomical Research & Technology)
出版日期: 2018-04
DOI: 10.14005/j.cnki.issn1672-7673.20180427.001
分类号: TP311.1
学科分类: 天文学::太阳与太阳系
产权排序: 第2完成单位
收录类别: CSCD
关键词: 太阳光谱 ; 偏振光谱测量 ; 空间二维扫描 ; 观测模式
中文摘要: 作为抚仙湖1m新真空太阳望远镜的观测终端之一,多波段光谱仪需具备两个观测模式,即空间二维扫描观测以及偏振光谱测量,从而实现诊断太阳矢量磁场及其动力学特征的科学目标,本文工作则紧紧围绕如何架构和实现上述两种观测模式而展开。首先明确观测模式对三大重要光电机构(即空间扫描机构、偏振分析器和仪器偏振定标机构)的基本要求,其次从实测太阳物理需要出发,分析这些要求的具体实现方法(连续式或步进式)、控制精度(10-2或10-3)以及信噪比提高方法(多帧叠加或多组叠加)等。最后梳理并给出了多种观测模式的流程图,并将不同观测模式集成于一个采集控制程序之中,投入实测,分别进行了多组活动区二维空间扫描观测和黑子偏振光谱测量,取得了较好的结果。
英文摘要: Multi-band spectrometer is one of the terminals used at Fuxian-Lake 1-meter New Vacuum Solar Telescope (NVST). Its major objective is to investigate the vector magnetogram and dynamics of the solar features. To achieve this, two features, imaging observation and spectropolarimetric observation, are realized based on three groups of instruments: field scanner, polarimeter and instrumental calibration unit. For the calibration of the instruments, the instrumental calibration unit (ICU) is installed inside the vacuum telescope tube, near the F2 focus. It consists of two optical elements, a linear polarizer and a retarder, mounted on two independent rotating motorized stages. Both will be moved into the beam, rotating around the optical axis respectively with predefined angles during calibration, and moved out of the beam during observation. The polarimeter and field scanner are mounted in the coude room. The field scanner, for 2D spectrometric observation, is mounted before the beam splitter, which splits the incident beam into two parts, one reflected into the multi-channel high-resolution imaging system and the other passing the splitter and then entering the spectrometers through the slit. The field scanner is made up of two sets of K-shaped mirrors, one of which is mounted on a vertical direction motorized stage. The scanning observation is realized by vertically moving stage in the direction perpendicular to the slit, which will shifts the incident light across the slit. The polarimeter is installed beneath the previous mentioned beam splitter and above the slit. It consists of a retarder, mounted on a rotating motorized stage, and a polarizer, fixed on the base of the same rotating stage, beneath the retarder. During spectropolarimetric observation or calibration, the retarder will be rotated around the optical axis. Since the ICU is installed inside the vacuum tube, a complicated deployment approach is thus used. The power cables and communication cables of the ICU are all connected to the external environment through sealed plug. The RS232 cables are converted to the Ethernet cable and then connected the router which is accessible to the data-acquisition and control PC in coude room. The power cables are connected to a Ethernet-controlled power relay which is also connected to the above the router. The remote PC could control the power switch-off/on action of the ICU and any operations of the motorized stages through Ethernet. The field scanner and polarimeter are connected to the PC by RS232 cable for versatility and flexibility. This paper focuses on the design and implementation of imaging and spectropolarimetric observation mode at NVST. The scientific requirements of the field scanner, polarimeter and instrumental calibration unit are given in section 1. There are two working approaches of the field scanner available for scanning observation. One is acquiring the spectra continuously as the scanner is moved from the start position to the end position in steady velocity, while the other one is acquiring the n (n>=1) frames of the spectra after the scanner stops at the specific position. Considering spectropolarimetric observation, the field scanner uses step-by-step approach as the default mode. Since the step-by-step method is used to demodulate the Stokes parameters, the polarimeter also uses similar approach as the scanner does. The spectra are acquired after the rotation stage stops the specific angle. And to avoid introducing extra polarimetric measurements errors, the accuracy of the rotation stage is within 0.002 degrees. And multiple successive frames are acquired at each polarimetric status and then averaged in post data-proccess to achieve better signal-to-noise ratio. This, however, degrades the temporal resolution. Hence, the spatial resolution is sacrificed, a 2x2 binning is adopted for scientific observation. For instrumental calibration, however, the temporal resolution is considered the most important, for the effect of the variation of alt-azimuth of the telescope on cross-talk. A 2x8 binning is thus adopted in this case. To simplify the observation operations and minimize the manual errors, all the functions are integrated into the observation control program, which is illustrated in section 2. And the observation result of active regions are also shown in this section.Multi-band spectrometer is one of the terminals used at Fuxian-Lake 1-meter New Vacuum Solar Telescope (NVST). Its major objective is to investigate the vector magnetogram and dynamics of the solar features. To achieve this, two features, imaging observation and spectropolarimetric observation, are realized based on three groups of instruments: field scanner, polarimeter and instrumental calibration unit. For the Multi-band spectrometer is one of the terminals used at Fuxian-Lake 1-meter New Vacuum Solar Telescope (NVST). Its major objective is to investigate the vector magnetogram and dynamics of the solar features. To achieve this, two features, imaging observation and spectropolarimetric observation, are realized based on three groups of instruments: field scanner, polarimeter and instrumental calibration unit. For the calibration of the instruments, the instrumental calibration unit (ICU) is installed inside the vacuum telescope tube, near the F2 focus. It consists of two optical elements, a linear polarizer and a retarder, mounted on two independent rotating motorized stages. Both will be moved into the beam, rotating around the optical axis respectively with predefined angles during calibration, and moved out of the beam during observation. The polarimeter and field scanner are mounted in the coude room. The field scanner, for 2D spectrometric observation, is mounted before the beam splitter, which splits the incident beam into two parts, one reflected into the multi-channel high-resolution imaging system and the other passing the splitter and then entering the spectrometers through the slit. The field scanner is made up of two sets of K-shaped mirrors, one of which is mounted on a vertical direction motorized stage. The scanning observation is realized by vertically moving stage in the direction perpendicular to the slit, which will shifts the incident light across the slit. The polarimeter is installed beneath the previous mentioned beam splitter and above the slit. It consists of a retarder, mounted on a rotating motorized stage, and a polarizer, fixed on the base of the same rotating stage, beneath the retarder. During spectropolarimetric observation or calibration, the retarder will be rotated around the optical axis. Since the ICU is installed inside the vacuum tube, a complicated deployment approach is thus used. The power cables and communication cables of the ICU are all connected to the external environment through sealed plug. The RS232 cables are converted to the Ethernet cable and then connected the router which is accessible to the data-acquisition and control PC in coude room. The power cables are connected to a Ethernet-controlled power relay which is also connected to the above the router. The remote PC could control the power switch-off/on action of the ICU and any operations of the motorized stages through Ethernet. The field scanner and polarimeter are connected to the PC by RS232 cable for versatility and flexibility. This paper focuses on the design and implementation of imaging and spectropolarimetric observation mode at NVST. The scientific requirements of the field scanner, polarimeter and instrumental calibration unit are given in section 1. There are two working approaches of the field scanner available for scanning observation. One is acquiring the spectra continuously as the scanner is moved from the start position to the end position in steady velocity, while the other one is acquiring the n (n>=1) frames of the spectra after the scanner stops at the specific position. Considering spectropolarimetric observation, the field scanner uses step-by-step approach as the default mode. Since the step-by-step method is used to demodulate the Stokes parameters, the polarimeter also uses similar approach as the scanner does. The spectra are acquired after the rotation stage stops the specific angle. And to avoid introducing extra polarimetric measurements errors, the accuracy of the rotation stage is within 0.002 degrees. And multiple successive frames are acquired at each polarimetric status and then averaged in post data-proccess to achieve better signal-to-noise ratio. This, however, degrades the temporal resolution. Hence, the spatial resolution is sacrificed, a 2x2 binning is adopted for scientific observation. For instrumental calibration, however, the temporal resolution is considered the most important, for the effect of the variation of alt-azimuth of the telescope on cross-talk. A 2x8 binning is thus adopted in this case. To simplify the observation operations and minimize the manual errors, all the functions are integrated into the observation control program, which is illustrated in section 2. And the observation result of active regions are also shown in this section.calibration of the instruments, the instrumental calibration unit (ICU) is installed inside the vacuum telescope tube, near the F2 focus. It consists of two optical elements, a linear polarizer and a retarder, mounted on two independent rotating motorized stages. Both will be moved into the beam, rotating around the optical axis respectively with predefined angles during calibration, and moved out of the beam during observation. The polarimeter and field scanner are mounted in the coude room. The field scanner, for 2D spectrometric observation, is mounted before the beam splitter, which splits the incident beam into two parts, one reflected into the multi-channel high-resolution imaging system and the other passing the splitter and then entering the spectrometers through the slit. The field scanner is made up of two sets of K-shaped mirrors, one of which is mounted on a vertical direction motorized stage. The scanning observation is realized by vertically moving stage in the direction perpendicular to the slit, which will shifts the incident light across the slit. The polarimeter is installed beneath the previous mentioned beam splitter and above the slit. It consists of a retarder, mounted on a rotating motorized stage, and a polarizer, fixed on the base of the same rotating stage, beneath the retarder. During spectropolarimetric observation or calibration, the retarder will be rotated around the optical axis. Since the ICU is installed inside the vacuum tube, a complicated deployment approach is thus used. The power cables and communication cables of the ICU are all connected to the external environment through sealed plug. The RS232 cables are converted to the Ethernet cable and then connected the router which is accessible to the data-acquisition and control PC in coude room. The power cables are connected to a Ethernet-controlled power relay which is also connected to the above the router. The remote PC could control the power switch-off/on action of the ICU and any operations of the motorized stages through Ethernet. The field scanner and polarimeter are connected to the PC by RS232 cable for versatility and flexibility. This paper focuses on the design and implementation of imaging and spectropolarimetric observation mode at NVST. The scientific requirements of the field scanner, polarimeter and instrumental calibration unit are given in section 1. There are two working approaches of the field scanner available for scanning observation. One is acquiring the spectra continuously as the scanner is moved from the start position to the end position in steady velocity, while the other one is acquiring the n (n>=1) frames of the spectra after the scanner stops at the specific position. Considering spectropolarimetric observation, the field scanner uses step-by-step approach as the default mode. Since the step-by-step method is used to demodulate the Stokes parameters, the polarimeter also uses similar approach as the scanner does. The spectra are acquired after the rotation stage stops the specific angle. And to avoid introducing extra polarimetric measurements errors, the accuracy of the rotation stage is within 0.002 degrees. And multiple successive frames are acquired at each polarimetric status and then averaged in post data-proccess to achieve better signal-to-noise ratio. This, however, degrades the temporal resolution. Hence, the spatial resolution is sacrificed, a 2x2 binning is adopted for scientific observation. For
instrumental calibration, however, the temporal resolution is considered the most important, for the effect of the variation of alt-azimuth of the telescope on cross-talk. A 2x8 binning is thus adopted in this case. To simplify the observation operations and minimize the manual errors, all the functions are integrated into the observation control program, which is illustrated in section 2. And the observation result of active regions are also shown in this section.Multi-band spectrometer is one of the terminals used at Fuxian-Lake 1-meter New Vacuum Solar Telescope (NVST). Its major objective is to investigate the vector magnetogram and dynamics of the solar features. To achieve this, two features, imaging observation and spectropolarimetric observation, are realized based on three groups of instruments: field scanner, polarimeter and instrumental calibration unit. For the calibration of the instruments, the instrumental calibration unit (ICU) is installed inside the vacuum telescope tube, near the F2 focus. It consists of two optical elements, a linear polarizer and a retarder, mounted on two independent rotating motorized stages. Both will be moved into the beam, rotating around the optical axis respectively with predefined angles during calibration, and moved out of the beam during observation. The polarimeter and field scanner are mounted in the coude room. The field scanner, for 2D spectrometric observation, is mounted before the beam splitter, which splits the incident beam into two parts, one reflected into the multi-channel high-resolution imaging system and the other passing the splitter and then entering the spectrometers through the slit. The field scanner is made up of two sets of K-shaped mirrors, one of which is mounted on a vertical direction motorized stage. The scanning observation is realized by vertically moving stage in the direction perpendicular to the slit, which will shifts the incident light across the slit. The polarimeter is installed beneath the previous mentioned beam splitter and above the slit. It consists of a retarder, mounted on a rotating motorized stage, and a polarizer, fixed on the base of the same rotating stage, beneath the retarder. During spectropolarimetric observation or calibration, the retarder will be rotated around the optical axis. Since the ICU is installed inside the vacuum tube, a complicated deployment approach is thus used. The power cables and communication cables of the ICU are all connected to the external environment through sealed plug. The RS232 cables are converted to the Ethernet cable and then connected the router which is accessible to the data-acquisition and control PC in coude room. The power cables are connected to a Ethernet-controlled power relay which is also connected to the above the router. The remote PC could control the power switch-off/on action of the ICU and any operations of the motorized stages through Ethernet. The field scanner and polarimeter are connected to the PC by RS232 cable for versatility and flexibility. This paper focuses on the design and implementation of imaging and spectropolarimetric observation mode at NVST. The scientific requirements of the field scanner, polarimeter and instrumental calibration unit are given in section 1. There are two working approaches of the field scanner available for scanning observation. One is acquiring the spectra continuously as the scanner is moved from the start position to the end position in steady velocity, while the other one is acquiring the n (n>=1) frames of the spectra after the scanner stops at the specific position. Considering spectropolarimetric observation, the field scanner uses step-by-step approach as the default mode. Since the step-by-step method is used to demodulate the Stokes parameters, the polarimeter also uses similar approach as the scanner does. The spectra are acquired after the rotation stage stops the specific angle. And to avoid introducing extra polarimetric measurements errors, the accuracy of the rotation stage is within 0.002 degrees. And multiple successive frames are acquired at each polarimetric status and then averaged in post data-proccess to achieve better signal-to-noise ratio. This, however, degrades the temporal resolution. Hence, the spatial resolution is sacrificed, a 2x2 binning is adopted for scientific observation. For instrumental calibration, however, the temporal resolution is considered the most important, for the effect of the variation of alt-azimuth of the telescope on cross-talk. A 2x8 binning is thus adopted in this case. To simplify the observation operations and minimize the manual errors, all the functions are integrated into the observation control program, which is illustrated in section 2. And the observation result of active regions are also shown in this section.
项目资助者: 国家自然科学基金(11473064)
语种: 中文
ISSN号: 1672-7673
Citation statistics:
内容类型: 期刊论文
URI标识: http://ir.ynao.ac.cn/handle/114a53/12157
Appears in Collections:抚仙湖太阳观测站_期刊论文

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作者单位: 1.中国科学院大学,北京 ,100049
2.中国科学院云南天文台,云南 ,昆明 ,650011

Recommended Citation:
陈宇超,徐稚,李正刚,等. 抚仙湖一米新真空太阳望远镜空间二维偏振光谱观测模式设计与实现[J]. 天文研究与技术( Astronomical Research & Technology),2018.
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