行星科学研究中热发射光谱的实验测量与定标方法
doi: 10.11728/cjss2024.01.2023-0116 cstr: 32142.14.cjss2024.01.2023-0116
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杨亚洲：男, 1990年9月出生于湖北省孝感市, 现为中国科学院国家空间科学中心副研究员, 主要研究方向为行星光谱学、无大气天体表面的空间风化作用等. E-mail: yangyazhou@nssc.ac.cn
作者简介:
Laboratory Thermal Emission Spectral Measurement and Calibration Methods for Planetary Science Research
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摘要: 准确的物质组成信息是解译行星体形成与演化历史的关键, 可见–近红外遥感光谱探测一直是获取行星表面成分的主要技术手段. 在热红外谱段光谱特征更为丰富, 因此随着探测技术的发展, 其在行星探测中得到越来越多的应用. 尤其是在目前已经实施与立项的国内外小行星探测任务中, 都将热发射光谱仪作为核心载荷之一. 为了更好地对将来获取的热发射光谱数据进行解译, 建立科学合理的数据处理与定标方案是必不可少的. 本文对用于行星科学研究的热发射光谱测量装置的设计、测量及数据处理方法进行了系统分析. 针对低温、真空条件下热发射测量过程中样品辐射信号与仪器辐射信号难以分离的问题, 提出并论证了基于傅里叶变换红外光谱仪原始测量信号–干涉图的数据处理方法. 该方法可以更为有效地分离出样品实际辐射信号, 从而获得更为准确的发射率光谱数据. 研究结果可为国内相关热发射测量装置的设计与搭建以及未来天问二号等探测数据的处理与科学解译提供参考.Abstract: Accurate information regarding the surface composition is crucial for understanding the formation and evolution history of planetary bodies. Visible and near-infrared remote sensing spectroscopic techniques have long been used for the detection of surface composition. However, in the thermal infrared spectral range, various types of planetary surface materials exhibit richer spectral features. With the development of thermal emission spectroscopic techniques, it has been increasingly used in planetary exploration. Particularly, in the ongoing and planned asteroid exploration missions, thermal emission spectrometers are employed as key payloads. In order to better interpret the thermal emission spectral data to be obtained in the future, it is essential to establish scientifically reasonable data processing and calibration schemes. This paper provides a comprehensive overview on the design of thermal emission spectral measurement devices for planetary science research, the measurement process, and data reduction methods. To obtain accurate emissivity spectra data, the challenge of distinguishing sample radiation signals from instrument radiation during thermal emission measurements must be properly addressed first. Especially, for measurements conducted under low-temperature and vacuum conditions that are similar to the surface conditions of the Moon and asteroids. This paper proposes and demonstrates a data reduction method based on interferograms, which are the original signals measured by FTIR spectrometer. This method can effectively separate the actual radiation signal from the samples, thus yielding more accurate emissivity spectra data. The insights derived from this study can serve as valuable references for the development and construction of thermal emission measurement devices and can facilitate the processing and scientific interpretation of data from future missions such as Tianwen-2.
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Key words:
- Planetary exploration /
- Thermal emission /
- Spectroscopy /
- Laboratory measurements /
- Calibration
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图 1 可见–近红外与中红外波段月表反射太阳光与自身热发射的光强分布
Figure 1. Light reflected and emitted from the Moon surface in the visible and near-infrared and mid-infrared wavelengths
图 2 月表主要矿物的可见–近红外反射光谱与热红外发射光谱. 光谱数据分别源自RELAB[24]与ASU光谱数据库(
http://speclib.asu.edu/ ), #后编号为对应的光谱数据IDFigure 2. Visible and near-infrared reflectance and thermal infrared emission spectra of typical lunar-type minerals. The spectral data are collected from the RELAB[24] and ASU spectral databases (
http://speclib.asu.edu/ ), respectively. The numbers after # are the corresponding spectral data ID in those two database
图 3 热发射测量装置的组成与辐射信号光路(Es表示从样品表面辐射与反射出的能量; Ed表示由探测器辐射出的经干涉仪调制后又反射到探测器的能量; Rs为样品表面反射率, Rs·Eenv表示样品腔内部环境辐射能量经样品表面反射后 进入探测器的能量. 左边FTIR光谱仪光路图是基于Bruker VertexTM光谱仪内部光路图绘制的)
Figure 3. Configurations for general setup of thermal emission measurement device and the optical path of emitted light. Es represents the energies emitted and reflected by the sample surface. Ed represents the energy emitted from the detector that is modulated by the interferometer and then reflected back to the detector. Rs is the reflectance of sample surface, and Rs·Eenv represents the energy emitted by the internal environment of the chamber and reflected by the sample (The optical path diagram of the FTIR spectrometer in the left is based on the internal configuration of the Bruker VertexTM spectrometer)
图 4 基于普朗克黑体辐射公式计算得到的探测器与 红外光源辐射能量对比
Figure 4. Comparison of radiation energy between detector and infrared light source calculated based on the Planck blackbody radiation formula
图 5 温度偏差对发射率的影响
Figure 5. Effects of temperature differences on the derived emissivity
图 6 低温真空条件下将黑体1加热至不同温度测得的信号(箭头所示方向为黑体温度逐渐升高的方向)
Figure 6. Signals measured by heating blackbody-1 to different temperatures under cold vacuum conditions. The arrows in the plot indicate the increasing trend of the blackbody’s temperature
图 7 低温真空条件下将黑体2加热至不同温度测得的信号(箭头所示方向为黑体温度逐渐升高的方向)
Figure 7. Signals measured by heating blackbody-2 to different temperatures under cold vacuum conditions. The arrows in the plot indicate the increasing trend of the blackbody’s temperature
图 9 基于理论公式计算得到的红外光源光强与包含不同相位偏差的干涉信号示例
Figure 9. Spectra of infrared light source and corresponding interferograms with or without phase error based on theoretical calculations
图 10 探测器与不同温度下黑体的实测干涉信号对比
Figure 10. Comparison of measured interferograms between the detector and the blackbody with varied temperatures
图 11 源自外部光源与探测器本身辐射的光经过分束器后的相位变化
Figure 11. Phase changes of the radiation light from the external light source and the detector itself after passing through the beam splitter
图 12 在干涉图层面扣除仪器辐射信号后再进行傅里叶变换等处理得到的两个自制黑体在不同温度下的实际辐射信号
Figure 12. Actual radiation signals of two self-made blackbodies at different temperatures with the instrument radiation signal subtracted based on their interferograms
表 1 热发射测量装置的指标参考
Table 1. Some references for thermal emission measurement device
指标类型 ALEC[52] PARSEC[54] PASCALE[59,60] FTIR光谱仪型号 NicoletTM Nexus 870 NicoletTM 6700 BrukerTM Vertex 70 V 分束器 KBr KBr 宽谱段T240/3 检测器类型 DTGS DLaTGS 宽谱段DTGS 光谱范围 400～4000 cm–1 400～2200 cm–1 6000～50 cm–1 温度传感器与温控精度 铂电阻温度计, <1 K (未提及) 铂电阻温度计, ±0.3 K 样品腔真空度 <10–4 mbar 10–5 mbar <10–4 mbar 样品杯底部加热 电阻加热
最高可达约620 K电阻加热 电阻加热 顶部模拟太阳光照 卤钨灯: 功率可调
照射角度: 30°卤钨灯: 功率可调
照射角度: 55°卤钨灯: 功率可调
照射角度: 55°样品腔最低温度 约85 K <150 K <125 K 低温真空下测量时
样品温度设定值底部加热+顶部加热: 350～500 K 底部加热+顶部加热: 约350 K 底部加热+顶部加热: 亮温350±3 K 低温真空下测量时
黑体温度设定值低温: 约85 K
高温: ≥500 K低温: 330±0.5 K
高温: 370±0.5 K低温: 340 K
高温: 360 K注 ALEC: Asteroid and Lunar Environmental Chamber at Brown University. PARSEC: Planetary and Asteroid Regolith Spectroscopy Environmental Chamber at Stony Brook University. PASCALE: Planetary Analogue Surface Chamber for Asteroid and Lunar Environments at Oxford University. 
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