CN1635346A - Space modulation type interference spectrum imager on-satellite calibration method - Google Patents

Space modulation type interference spectrum imager on-satellite calibration method Download PDF

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CN1635346A
CN1635346A CN 200310124756 CN200310124756A CN1635346A CN 1635346 A CN1635346 A CN 1635346A CN 200310124756 CN200310124756 CN 200310124756 CN 200310124756 A CN200310124756 A CN 200310124756A CN 1635346 A CN1635346 A CN 1635346A
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相里斌
黄旻
计忠瑛
王忠厚
袁艳
李立英
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XiAn Institute of Optics and Precision Mechanics of CAS
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Abstract

一种空间调制型干涉光谱成像仪星上定标方法。该方法是:光谱曲线平坦的均匀面光源进入积分球,得到面均匀性更高的面光源;使该光源的光谱曲线产生吸收峰;经准直镜系统产生具有一定视场角的平行光,成为带有特征谱线的宽谱定标光源,用仪器测得该定标光源的光谱曲线。定标光源经超光谱成像仪的前置镜成像在一次像面狭缝上,再经干涉仪、傅立叶透镜、柱面镜在探测器阵列上产生干涉图像,经计算机复原,得到定标光源的光谱曲线;将该光谱曲线与预先获得的光谱曲线比对,得到所需的定标参数。用上述定标参数对仪器获得的数据进行修正,完成定标。An on-board calibration method for a spatially modulated interferometric spectroscopic imager. The method is: a uniform surface light source with a flat spectral curve enters the integrating sphere to obtain a surface light source with higher surface uniformity; the spectral curve of the light source produces an absorption peak; the collimator system produces parallel light with a certain field of view, Become a wide-spectrum calibration light source with characteristic spectral lines, and use the instrument to measure the spectral curve of the calibration light source. The calibration light source is imaged on the slit of the primary image plane by the front mirror of the hyperspectral imager, and then an interference image is generated on the detector array by the interferometer, Fourier lens, and cylindrical mirror, and the calibration light source is obtained by computer restoration. Spectral curve; compare the spectral curve with the pre-obtained spectral curve to obtain the required calibration parameters. Correct the data obtained by the instrument with the above calibration parameters to complete the calibration.

Description

空间调制型干涉光谱成像仪星上定标方法On-board Calibration Method for Spatial Modulation Interferometric Spectral Imager

技术领域technical field

本发明涉及一种空间调制型干涉光谱成像仪星上定标方法。The invention relates to an on-board calibration method for a space modulation type interference spectrum imager.

背景技术Background technique

干涉型光谱成像技术,亦称干涉成像光谱技术,发展于上世纪90年代,采用的是遥感观测手段,星上定标是其核心关键技术之一,目前国际上也正处于研究阶段。Interferometric spectral imaging technology, also known as interferometric imaging spectroscopy technology, was developed in the 1990s and uses remote sensing observation methods. On-board calibration is one of its core key technologies, and it is currently in the research stage internationally.

在工程实践中,由于材料的性质、装调的精度等原因,仪器获得的目标信息总会与实际目标存在一定差距,需要通过定标获得修正的参数,使仪器获得的结果尽量符合实际目标情况,故需进行定标。In engineering practice, due to the nature of materials, the accuracy of installation and other reasons, there will always be a certain gap between the target information obtained by the instrument and the actual target. It is necessary to obtain corrected parameters through calibration to make the results obtained by the instrument as close as possible to the actual target situation. , so calibration is required.

干涉型超光谱成像仪的定标与普通的CCD遥感相机不同。普通CCD遥感相机获得的是目标的几何图像,只需要进行辐射度定标即可满足要求;而干涉型超光谱成像仪除了获得目标的几何图像外,还要得到目标的光谱信息,所以其既要进行辐射度定标,还要进行光谱定标。The calibration of the interferometric hyperspectral imager is different from that of the common CCD remote sensing camera. The ordinary CCD remote sensing camera obtains the geometric image of the target, and only needs to perform radiometric calibration to meet the requirements; while the interferometric hyperspectral imager not only obtains the geometric image of the target, but also obtains the spectral information of the target, so it is both To perform radiometric calibration, spectral calibration is also performed.

由于干涉型超光谱成像仪的工作原理与色散型成像光谱仪的原理不同,色散型成像光谱仪探测器接收到的是目标的直接光谱信息,而干涉型成像光谱仪探测器接收到的是目标光谱的傅里叶变换信息。两者定标目的相同,但方法差异较大。Because the working principle of the interferometric hyperspectral imager is different from that of the dispersive imaging spectrometer, the detector of the dispersive imaging spectrometer receives the direct spectral information of the target, while the detector of the interferometric imaging spectrometer receives the Fu of the target spectrum. Leaf transformation information. Both have the same purpose, but the method is quite different.

美国于2000年7月发射的强力小卫星是世界上第一台投入实用的干涉型超光谱成像仪,强力小卫星起初想用一根光纤将太阳光引入至仪器作为定标的光源,希籍将仪器获得的数据与已知的太阳光谱作比对,而得到修正的参数。但该设想最终并未付诸实践,而是以地面辐射场定标进行比较修正。由于对太阳光谱特性了解的欠缺,目前国内还生产不出适于航天应用的光纤。The powerful small satellite launched by the United States in July 2000 is the first practical interferometric hyperspectral imager in the world. At first, the powerful small satellite wanted to use an optical fiber to introduce sunlight into the instrument as a light source for calibration. The data obtained by the instrument is compared with the known solar spectrum, and the corrected parameters are obtained. However, this idea was not put into practice in the end, but was compared and corrected by calibration of the ground radiation field. Due to the lack of understanding of the characteristics of the solar spectrum, there is currently no domestic production of optical fibers suitable for aerospace applications.

发明内容Contents of the invention

本发明解决了背景技术无法实现星载干涉型超光谱成像仪定标,即不能同时进行辐射度定标和光谱定标的技术问题。The invention solves the technical problem that the background technology cannot realize the calibration of the space-borne interferometric hyperspectral imager, that is, the radiometric calibration and the spectral calibration cannot be performed simultaneously.

本发明的技术解决方案是:Technical solution of the present invention is:

一种空间调制型干涉光谱成像仪星上定标方法,其特殊之处在于:该方法包括:An on-board calibration method for a space-modulated interferometric spectroscopic imager, which is special in that the method includes:

1).由 柯拉照明系统或积分球系统光源发出光谱曲线平坦的均匀面光源,由入口3进入积分球4,得到面均匀性更高的面光源。1). A uniform surface light source with a flat spectral curve is emitted by the Kohler lighting system or an integrating sphere system light source, and enters the integrating sphere 4 from the entrance 3 to obtain a surface light source with higher surface uniformity.

2).使该光源的光谱曲线产生吸收峰。在出口5处放置钕镨玻璃或其他具有吸收峰透明材料使其光谱曲线产生两个、三个或多个吸收峰。2). Make the spectral curve of the light source produce an absorption peak. Placed at the outlet 5, dodman-praseodymium glass or other transparent materials with absorption peaks make the spectral curve produce two, three or more absorption peaks.

3).经准直镜系统产生具有一定视场角的平行光,即成为带有特征谱线的宽谱定标光源,用标准仪器测得该定标光源的光谱曲线。 3). The collimator system produces parallel light with a certain field of view, which becomes a wide-spectrum calibration light source with characteristic spectral lines, and the spectral curve of the calibration light source is measured with standard instruments.

4).定标光源经过超光谱成像仪的前置镜成像在一次像面狭缝上,然后再经过干涉仪、傅立叶透镜、柱面镜在探测器阵列上产生干涉图像。该图像,经过计算机复原软件复原后,得到超光谱成像仪获得的定标光源的光谱曲线,4). The calibration light source is imaged on the slit of the primary image plane through the front mirror of the hyperspectral imager, and then passes through the interferometer, Fourier lens, and cylindrical mirror to generate an interference image on the detector array. After the image is restored by the computer restoration software, the spectral curve of the calibration light source obtained by the hyperspectral imager is obtained.

5).将这条光谱曲线与我们预先获得的光谱曲线比对,就可以得到我们需要的定标参数。平坦的宽谱可以用来作辐射度定标,光源的吸收峰可以用来确定仪器的光谱分辨率,以及谱线的位置和相对幅值。5). Comparing this spectral curve with the spectral curve we obtained in advance, we can get the calibration parameters we need. The flat broad spectrum can be used for radiometric calibration, and the absorption peak of the light source can be used to determine the spectral resolution of the instrument, as well as the position and relative amplitude of the spectral lines.

6).用上述定标参数对仪器获得的数据进行修正,完成定标。6). Use the above calibration parameters to correct the data obtained by the instrument to complete the calibration.

上述准直镜焦距和相对孔径与成像光谱仪前置镜相同;准直镜6与超光谱成像仪的前置镜一起将积分球4出射的光会聚在超光谱成像仪光学系统的狭缝上,然后通过干涉仪、富里叶透镜、柱面镜在探测器上成像;准直镜6——将光源变为平行光;由此,整个定标系统产生的定标光源就成为带有特征谱线的宽谱光源。宽谱光源将可以用作辐射度定标,光源的特征谱线通过光谱复原进行光谱特性分析,可以确定光谱线位置的变化情况,达到星上相对定标的目的;再经准直镜系统6,最后光线经反射镜7折转光路,被引入仪器的光学系统进行定标。The above-mentioned collimating lens focal length and relative aperture are identical with imaging spectrometer front mirror; Then image on the detector through the interferometer, Fourier lens, and cylindrical mirror; collimator 6——change the light source into parallel light; thus, the calibration light source generated by the entire calibration system becomes a beam with characteristic spectral lines wide-spectrum light source. The wide-spectrum light source can be used for radiometric calibration, and the characteristic spectral lines of the light source can be analyzed through spectral restoration to determine the change of the spectral line position and achieve the purpose of relative calibration on the star; , and finally the light is refracted by the mirror 7 and introduced into the optical system of the instrument for calibration.

上述定标是指确定遥感器输出准确数值的过程,主要手段是测定遥感器对一个已知辐射特性目标的响应。对干涉型超光谱成像仪来说,定标内容主要包括光谱定标和辐射度定标两方面,其中辐射度定标又包括相对辐射度定标和绝对辐射度定标两种,相对辐射度定标用来确定仪器各谱段的相对辐射响应和探测器不同单元的相对辐射响应,绝对辐射定标用来确定仪器输出信号,使之能够反应输入信号的绝对辐射强度。The above-mentioned calibration refers to the process of determining the accurate value output by the remote sensor, and the main method is to measure the response of the remote sensor to a target with known radiation characteristics. For the interferometric hyperspectral imager, the calibration content mainly includes two aspects: spectral calibration and radiometric calibration, and radiometric calibration includes relative radiometric calibration and absolute radiometric calibration. Calibration is used to determine the relative radiation response of each spectral band of the instrument and the relative radiation response of different units of the detector. Absolute radiation calibration is used to determine the output signal of the instrument so that it can reflect the absolute radiation intensity of the input signal.

所述的光谱定标:就是确定干涉图零光程差的位置、频率以及最大光程差,从而确定各谱段的中心波长和半波宽度。它对保证仪器的光谱分辨率十分重要,同时对干涉仪的工作状态是否正常是最主要的判据。The spectral calibration is to determine the position, frequency and maximum optical path difference of the interferogram zero optical path difference, so as to determine the center wavelength and half-wave width of each spectral segment. It is very important to ensure the spectral resolution of the instrument, and at the same time it is the most important criterion for the normal working state of the interferometer.

所述的辐射度定标:通常星上主要进行相对辐射度定标。The radiometric calibration: Usually, the relative radiometric calibration is mainly performed on the star.

已知光谱强度分布B(σ)的定标光源进入超光谱成像仪,得到像元的干涉强度分布为:The calibration light source with known spectral intensity distribution B(σ) enters the hyperspectral imager, and the interference intensity distribution of the pixel is obtained as:

I(x)=∫K(σ)B(σ)cos(2πxσ)dσ+INI(x)=∫K(σ)B(σ)cos(2πxσ)dσ+IN

IN是像元的零输入响应,x为光程差,σ为波数。K(σ)是系统的光谱响应函数。IN is the zero-input response of the pixel, x is the optical path difference, and σ is the wavenumber. K(σ) is the spectral response function of the system.

上述干涉图经滤波、相位修正后,进行反傅里叶变换,得到复原光谱强度分布B’(σ),则有After filtering and phase correction, the above interferogram is subjected to inverse Fourier transform to obtain the restored spectral intensity distribution B’(σ), then there is

B’(σ)=K(i,j)×B(σ)B'(σ)=K(i,j)×B(σ)

在K(i,j)中,i与j分别表示空间方向像元数与谱段数。K(i,j)就是第i列探测器单元的光谱修正值,(j=1,2……N,N为谱段数),即光谱响应函数。In K(i, j), i and j represent the number of pixels in the spatial direction and the number of spectral segments, respectively. K(i, j) is the spectral correction value of the i-th detector unit, (j=1, 2...N, N is the number of spectral segments), that is, the spectral response function.

用同样的方法,可对各列(i=2……M)单元求出修正值,最后得到一个完整的二维修正系数矩阵K(i,j),提供光谱辐射度修正数据,完成光谱辐射度的定标。Using the same method, the correction value can be obtained for each column (i=2...M) unit, and finally a complete two-dimensional correction coefficient matrix K(i, j) can be obtained to provide spectral radiance correction data and complete the spectral radiance degree calibration.

本发明具有以下优点:The present invention has the following advantages:

1.实现了星载干涉型超光谱成像仪的定标;1. Realized the calibration of the spaceborne interferometric hyperspectral imager;

2.可同时完成辐射度定标及光谱定标;2. Radiometric calibration and spectral calibration can be completed at the same time;

3.定标精度可以达到:相对精度为5%,绝对精度为10%;3. Calibration accuracy can reach: relative accuracy is 5%, absolute accuracy is 10%;

4.材料、仪器不需要特制;4. Materials and instruments do not need to be specially made;

5.采用现有的材料、仪器即可实现定标目的。5. The purpose of calibration can be achieved by using existing materials and instruments.

附图说明Description of drawings

附图为本发明星上定标光学系统的结构示意图。The accompanying drawing is a structural schematic diagram of the on-board calibration optical system of the present invention.

附图标号说明:1-光源,2-聚光镜,3-入口,4-积分球,5-出口,6-准直 系统,7-反射镜。Description of reference numerals: 1-light source, 2-condenser, 3-inlet, 4-integrating sphere, 5-exit, 6-collimating mirror system, 7-reflector.

具体实施方式Detailed ways

本发明定标系统光源的光谱曲线可预先测得。卤钨灯的光谱是比较平坦的,经过积分球系统,谱线上会产生一些尖锐的吸收峰,吸收峰的数目、位置与积分球口的材质有关。利用光谱的平坦部分做辐射度定标,用吸收峰的位置以及半高宽做光谱定标。The spectrum curve of the light source of the calibration system of the present invention can be measured in advance. The spectrum of the tungsten-halogen lamp is relatively flat. After passing through the integrating sphere system, there will be some sharp absorption peaks on the spectral line. The number and position of the absorption peaks are related to the material of the integrating sphere. The flat part of the spectrum is used for radiometric calibration, and the position of the absorption peak and the full width at half maximum are used for spectral calibration.

参见附图,本发明由 柯拉照明系统积分球系统准直镜系统组成。Referring to accompanying drawing, the present invention is made up of Cora lighting system , integrating sphere system and collimating mirror system .

1.由 柯拉照明系统或积分球系统光源发出光谱曲线平坦的均匀面光源,由入口3进入积分球4,得到面均匀性更高的面光源。1. A uniform surface light source with a flat spectral curve is emitted by the Kohler lighting system or an integrating sphere system light source, and enters the integrating sphere 4 from the entrance 3 to obtain a surface light source with higher surface uniformity.

2.使该光源的光谱曲线产生吸收峰。在出口5处放置钕镨玻璃或其他具有吸收峰透明材料使其光谱曲线产生两个、三个或多个吸收峰。2. Make the spectral curve of the light source produce an absorption peak. Placed at the outlet 5, dodman-praseodymium glass or other transparent materials with absorption peaks make the spectral curve produce two, three or more absorption peaks.

3.经准直镜系统产生具有一定视场角的平行光,即成为带有特征谱线的宽谱定标光源,用标准仪器测得该定标光源的光谱曲线。 3. The collimator system produces parallel light with a certain field of view, which becomes a wide-spectrum calibration light source with characteristic spectral lines, and the spectral curve of the calibration light source is measured with standard instruments.

4.定标光源经过超光谱成像仪的前置镜成像在一次像面狭缝上,然后再经过干涉仪、傅立叶透镜、柱面镜在探测器阵列上产生干涉图像。该图像,经过计算机复原软件复原后,得到超光谱成像仪获得的定标光源的光谱曲线,4. The calibration light source is imaged on the slit of the primary image plane through the front mirror of the hyperspectral imager, and then passes through the interferometer, Fourier lens, and cylindrical mirror to generate an interference image on the detector array. After the image is restored by the computer restoration software, the spectral curve of the calibration light source obtained by the hyperspectral imager is obtained.

5.将这条光谱曲线与我们预先获得的光谱曲线比对,就可以得到我们需要的定标参数。平坦的宽谱可以用来作辐射度定标,光源的吸收峰可以用来确定仪器的光谱分辨率,以及谱线的位置和相对幅值。5. Comparing this spectral curve with the spectral curve we obtained in advance, we can get the calibration parameters we need. The flat broad spectrum can be used for radiometric calibration, and the absorption peak of the light source can be used to determine the spectral resolution of the instrument, as well as the position and relative amplitude of the spectral lines.

6.用上述定标参数对仪器获得的数据进行修正,完成定标。6. Use the above calibration parameters to correct the data obtained by the instrument to complete the calibration.

准直镜焦距和相对孔径与成像光谱仪前置镜相同。The focal length and relative aperture of the collimating mirror are the same as those of the front mirror of the imaging spectrometer.

准直镜6与超光谱成像仪的前置镜一起将积分球4出射的光会聚在超光谱成像仪光学系统的狭缝上,然后通过干涉仪、富里叶透镜、柱面镜在探测器上成像。准直镜6——将光源变为平行光。The collimating mirror 6 and the front mirror of the hyperspectral imager converge the light emitted by the integrating sphere 4 on the slit of the optical system of the hyperspectral imager, and then pass through the interferometer, Fourier lens, and cylindrical mirror on the detector imaging. Collimating mirror 6——to change the light source into parallel light.

这样,整个定标系统产生的定标光源就成为带有特征谱线的宽谱光源。宽谱光源将可以用作辐射度定标,光源的特征谱线通过光谱复原进行光谱特性分析,可以确定光谱线位置的变化情况,达到星上相对定标的目的。再经准直镜系统6,最后光线经反射镜7折转光路,被引入仪器的光学系统进行定标。朗伯板8,In this way, the calibration light source generated by the entire calibration system becomes a wide-spectrum light source with characteristic spectral lines. The wide-spectrum light source can be used for radiometric calibration, and the characteristic spectral lines of the light source can be analyzed through spectral restoration to determine the changes in the position of the spectral lines and achieve the purpose of relative calibration on the star. After passing through the collimating mirror system 6, the light is finally refracted by the reflector 7 and introduced into the optical system of the instrument for calibration. Lambert Plate 8,

在工程实践中,由于材料性质,加工、装调精度等原因,以及空间环境与地面环境的不同,会引起仪器采集到的信号的变化,因此,需要通过定标获得修正的参数。In engineering practice, the signal collected by the instrument will change due to the nature of the material, the accuracy of processing and assembly, and the difference between the space environment and the ground environment. Therefore, it is necessary to obtain corrected parameters through calibration.

补充说明:Supplementary note:

定标是指确定遥感器输出准确数值的过程,主要手段是测定遥感器对一个已知辐射特性目标的响应。对干涉型超光谱成像仪来说,定标内容主要包括光谱定标和辐射度定标两方面,其中辐射度定标又包括相对辐射度定标和绝对辐射度定标两种,相对辐射度定标用来确定仪器各谱段的相对辐射响应和探测器不同单元的相对辐射响应,绝对辐射定标用来确定仪器输出信号,使之能够反应输入信号的绝对辐射强度。Calibration refers to the process of determining the accurate output value of the remote sensor. The main method is to measure the response of the remote sensor to a target with known radiation characteristics. For the interferometric hyperspectral imager, the calibration content mainly includes two aspects: spectral calibration and radiometric calibration, and radiometric calibration includes relative radiometric calibration and absolute radiometric calibration. Calibration is used to determine the relative radiation response of each spectral band of the instrument and the relative radiation response of different units of the detector. Absolute radiation calibration is used to determine the output signal of the instrument so that it can reflect the absolute radiation intensity of the input signal.

光谱定标:就是确定干涉图零光程差的位置、频率以及最大光程差,从而确定各谱段的中心波长和半波宽度。它对保证仪器的光谱分辨率十分重要,同时对干涉仪的工作状态是否正常是最主要的判据。Spectral calibration: It is to determine the position, frequency and maximum optical path difference of the interferogram, so as to determine the center wavelength and half-wave width of each spectral segment. It is very important to ensure the spectral resolution of the instrument, and at the same time it is the most important criterion for the normal working state of the interferometer.

辐射度定标:通常星上主要进行相对辐射度定标。Radiometric calibration: Usually, the relative radiometric calibration is mainly performed on the star.

已知光谱强度分布B(σ)的定标光源进入超光谱成像仪,得到像元的干涉强度分布为:The calibration light source with known spectral intensity distribution B(σ) enters the hyperspectral imager, and the interference intensity distribution of the pixel is obtained as:

I(x)=∫K(σ)B(σ)cos(2πxσ)dσ+INI(x)=∫K(σ)B(σ)cos(2πxσ)dσ+IN

IN是像元的零输入响应,x为光程差,σ为波数。K(σ)是系统的光谱响应函数。IN is the zero-input response of the pixel, x is the optical path difference, and σ is the wavenumber. K(σ) is the spectral response function of the system.

上述干涉图经滤波、相位修正后,进行反傅里叶变换,得到复原光谱强度分布B’(σ),则有After filtering and phase correction, the above interferogram is subjected to inverse Fourier transform to obtain the restored spectral intensity distribution B’(σ), then there is

B’(σ)=K(i,j)×B(σ)B'(σ)=K(i,j)×B(σ)

在K(i,j)中,i与j分别表示空间方向像元数与谱段数。K(i,j)就是第i列探测器单元的光谱修正值,(j=1,2……N,N为谱段数),即光谱响应函数。In K(i, j), i and j represent the number of pixels in the spatial direction and the number of spectral segments, respectively. K(i, j) is the spectral correction value of the i-th detector unit, (j=1, 2...N, N is the number of spectral segments), that is, the spectral response function.

用同样的方法,可对各列(i=2……M)单元求出修正值,最后得到一个完整的二维修正系数矩阵K(i,j),提供光谱辐射度修正数据,完成光谱辐射度的定标。Using the same method, the correction value can be obtained for each column (i=2...M) unit, and finally a complete two-dimensional correction coefficient matrix K(i, j) can be obtained to provide spectral radiance correction data and complete the spectral radiance degree calibration.

Claims (3)

  1. Calibrating method on 1 one kinds of spatial modulation type interference spectrum imager stars, it is characterized in that: this method comprises:
    1). by Cola illuminator or integration sphere light source systemLight source sends the smooth uniform area light source of the curve of spectrum, enters integrating sphere 4 by inlet 3, obtains the higher area source of surface uniformity.
    2). make the curve of spectrum of this light source produce absorption peak.Place didymium glass or other has the absorption peak transparent material and makes its curve of spectrum produce two, three or more absorption peak at outlet 5 places.
    3). produce directional light through calibration lens system, promptly with certain visual angleBecome the wide range scaling light source that has characteristic spectral line, record the curve of spectrum of this scaling light source with reference instrument.
    4). scaling light source is imaged on image planes slit through the preset lens of hyperspectral imager, and then lists the generation interference image through interferometer, fourier transform lens, cylindrical mirror at detector array.This image after computing machine recovery software rejuvenation, obtains the curve of spectrum of the scaling light source of hyperspectral imager acquisition,
    5). with this curve of spectrum and the comparison of the curve of spectrum that we obtain in advance, just can obtain the calibration parameter of our needs.Smooth wide range can be used for the radiancy calibration, and the absorption peak of light source can be used for determining the spectral resolution of instrument, and the position of spectral line and relative amplitude.
    6). with above-mentioned calibration parameter the data that instrument obtains are revised, finished calibration.
  2. Calibrating method on the 2 spatial modulation type interference spectrum imager stars according to claim 1, it is characterized in that: described collimating mirror focal length is identical with the imaging spectrometer preset lens with relative aperture; Collimating mirror 6 with the preset lens of hyperspectral imager with the optical convergence of integrating sphere 4 outgoing on the slit of hyperspectral imager optical system, then by interferometer, Fourier lens, cylindrical mirror imaging on detector; Collimating mirror 6---light source is become directional light; Thus, the scaling light source of whole scaling system generation just becomes the wide spectrum light source that has characteristic spectral line.Wide spectrum light source can be as the radiancy calibration, and the characteristic spectral line of light source carries out the spectral characteristic analysis by spectrum recovering, can determine the situation of change of spectrum line position, reaches the purpose of relative calibration on the star; Again through calibration lens system 6, last light is through catoptron 7 light path of turning back, and the optical system that is introduced into instrument is calibrated.
  3. Calibrating method on the 3 spatial modulation type interference spectrum imager stars according to claim 1 and 2, it is characterized in that: described calibration is meant determines that remote sensor exports the process of accurate numerical value, and main means are to measure the response of remote sensor to a known radiation characteristic target.Concerning interference type super spectrum imager, the calibration content comprises that mainly spectral calibration and radiancy calibrate two aspects, wherein the radiancy calibration comprises that again relative radiancy is calibrated and the absolute radiation degree is calibrated two kinds, the radiancy calibration is used for determining the relative radiometric response of each spectral coverage of instrument and the relative radiometric response of detector different units relatively, absolute radiometric calibration is used for determining the instrument output signal, enables to react the absolute radiation intensity of input signal.
    Described spectral calibration: be exactly position, frequency and the maximum optical path difference of determining the interferogram zero optical path difference, thereby determine the centre wavelength and the half band-width of each spectral coverage.It is very important to the spectral resolution that guarantees instrument, and whether the duty to interferometer normally is topmost criterion simultaneously.
    Described radiancy calibration: mainly carry out relative radiancy calibration usually on the star.
    The scaling light source of known spectra intensity distributions B (σ) enters hyperspectral imager, and the interference strength that obtains pixel is distributed as:
    I(x)=∫K(σ)B(σ)cos(2π×σ)dσ+IN
    IN is the zero input response of pixel, and x is an optical path difference, and σ is a wave number.K (σ) is the spectral response functions of system.
    Above-mentioned interference figure carries out inversefouriertransform after filtering, phase place correction, obtain recovered light spectral intensity distribution B ' (σ), then has
    B’(σ)=K(i,j)×B(σ)
    K (i, j) in, i and j be representation space direction pixel number and spectral coverage number respectively.(i j) is exactly the spectrum modified value of i row detector unit, (j=1,2 to K ... N, N are the spectral coverage number), i.e. spectral response functions.
    Use the same method, can be listed as (i=2 each ... M) modified value is obtained in the unit, and (i j), provides spectral radiant emittance correction data, finishes the calibration of spectral radiant emittance to obtain a complete two-dimentional correction factor matrix K at last.
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CN101187705B (en) * 2007-12-19 2011-05-18 中国科学院空间科学与应用研究中心 Spectrum irradiance standard light source for ultraviolet optical instrument radiometric calibration
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