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CN112097907B - A method for locating the moon with a slit spectrometer - Google Patents

A method for locating the moon with a slit spectrometer Download PDF

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CN112097907B
CN112097907B CN202010878151.2A CN202010878151A CN112097907B CN 112097907 B CN112097907 B CN 112097907B CN 202010878151 A CN202010878151 A CN 202010878151A CN 112097907 B CN112097907 B CN 112097907B
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lunar
spectral image
moon
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CN112097907A (en
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王一豪
王爽
李娟�
刘欢
武俊强
安玲坪
胡炳樑
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XiAn Institute of Optics and Precision Mechanics of CAS
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Abstract

本发明涉及对月定标方法，为解决采用狭缝型光谱仪、赤道仪和导星镜配合进行地基对月观测时，建立光谱图像变换，以及赤道仪赤经、赤纬坐标变换对应关系困难，造成观测误差大的技术问题，提供一种狭缝型光谱仪对月定位方法，通过建立狭缝型光谱仪月球图像变化与作为转台的赤道仪赤经坐标、赤纬坐标变化的对应关系，能够在对月定位过程中对赤道仪进行准确纠正，规避其指向误差，提高对月定标的准确性，解决了狭缝型光谱仪对月精确定位的难题。

Figure 202010878151

The invention relates to a method for calibrating the moon, in order to solve the difficulty of establishing spectral image transformation and the corresponding relationship between the equatorial mount ascension and declination coordinate transformation when a slit spectrometer, an equatorial mount and a guide mirror are used for ground-based moon observation, Due to the technical problem of large observation error, a method for locating the moon with a slit spectrometer is provided. In the process of moon positioning, the equatorial mount is accurately corrected to avoid its pointing error, improve the accuracy of the moon calibration, and solve the problem of precise moon positioning by the slit spectrometer.

Figure 202010878151

Description

Moon positioning method of slit type spectrometer
Technical Field
The invention relates to a moon calibration method, in particular to a moon positioning method of a slit type spectrometer.
Background
The traditional calibration method has reached the bottleneck of improving the data radiation precision of the space remote sensor, and the moon is used as a highly stable radiation source, so that the development of on-orbit monthly calibration becomes a common research consensus at home and abroad. The earth-based moon observation is relied on to establish a full-moon phase period moon radiation model, and the method has important significance for on-orbit moon calibration.
At present, a slit type spectrometer and an equatorial telescope are often matched for monthly calibration. The equatorial telescope is a commonly used astronomical observation device and has the function of offsetting the influence of earth rotation on astronomical observation, the equatorial telescope is selected as a turntable for stably tracking the moon by a foundation-based moon observation system, however, the mechanical rotation of the equatorial telescope has accumulated errors, the equatorial telescope needs to be continuously corrected in order to ensure the pointing accuracy of long-time observation, and the equatorial telescope is usually corrected by tracking a guide mirror and correcting the position of the guide. The slit type spectrometer needs to be actively pushed to scan or be swept by a passive target to acquire a complete image of the target, and single imaging is only a spectral image of one slit in space dimension. In addition, strict optical axis alignment between the slit type spectrometer and the star guide lens is difficult to achieve, and the error of the star guide lens pointing to the moon is large. Therefore, how to establish the corresponding relation between the spectral image transformation and the equatorial telescope right ascension and declination coordinate transformation so as to control the equatorial telescope to accurately point to the moon is one of the technical difficulties in developing automatic ground-based moon observation.
Disclosure of Invention
The invention provides a slit type spectrometer moon-alignment positioning method, aiming at solving the technical problems that when a slit type spectrometer, an equatorial telescope and a star guide mirror are matched for carrying out ground-based moon-alignment observation, spectral image transformation is established, and the coordinate transformation corresponding relation of the right ascension and the declination of the equatorial telescope is difficult, so that the observation error is large.
In order to achieve the purpose, the invention provides the following technical scheme:
a moon positioning method of a slit type spectrometer is characterized by comprising the following steps:
s1, calculating the lunar right ascension coordinate Ra and the declination coordinate Dec at the current moment according to a lunar position formula;
s2, taking an equatorial telescope as a rotary table for observing the moon by a slit type spectrometer; controlling the equatorial telescope to point to the moon according to the lunar right ascension coordinate Ra and the declination coordinate Dec at the current moment to serve as coarse positioning;
s3, adjusting the right ascension coordinates and the declination coordinates of the equatorial telescope to enable the lunar spectrum image to completely appear in the view field of the slit spectrometer;
s4, adjusting the declination coordinate of the equatorial telescope to enable the moon spectral image to be positioned at the center of the view field of the slit spectrometer, and calculating the center position M of the moon spectral image at the moment0(ii) a Adjusting the right ascension coordinates of the equatorial telescope to make the lunar spectrum image reach the widest, and calculating the lunar light at the momentSpectral image width LmaxAnd then adjusting the right ascension coordinates of the equatorial telescope to change the lunar spectrum image from the widest to one fifth of the widest, and calculating the width L of the lunar spectrum image at the momentminAnd simultaneously, recording the equatorial telescope right ascension coordinate ra when the lunar spectrum image is widestmaxAnd equatorial instrument right ascension coordinate ra when the moon spectral image is narrowestmin；
S5, calculating a right ascension correction coefficient between the coordinates of the right ascension of the equatorial telescope and the coordinates of the lunar spectral image:
Figure BDA0002653262950000021
s6, adjusting the declination coordinate of the equatorial telescope to move the lunar spectrum image from the left edge to the right edge, and recording the declination coordinate dec of the equatorial telescope when the lunar spectrum image is positioned at the left edge1And the equatorial declination coordinate dec of the moon spectral image at the right edge2Calculating the center position M of the moon spectral image at the left edge1And the center position M of the moon spectral image at the right edge2；
S7, calculating a declination correction coefficient between the declination coordinate of the equatorial telescope and the moon spectrum image coordinate:
Figure BDA0002653262950000022
and S8, correcting the right ascension coordinate and the declination coordinate of the equatorial telescope according to the right ascension correction coefficient pra obtained in the step S5 and the declination correction coefficient pdec obtained in the step S7 during each observation, and finishing positioning.
Further, the step S1 is preceded by a step S0 of performing polar axis calibration and one-star correction on the equatorial instrument.
Further, the lunar right ascension coordinate Ra and the declination coordinate Dec at the current time are calculated by a SAMPA algorithm.
Further, in step S4, the calculating step calculates the center position of the moon spectral image at the timePut M0Specifically, the lunar spectrum image is integrated in the spectrum dimension direction at this time to obtain an integral curve, and then the integral curve is derived to obtain the maximum value D of the derivativeleftAnd derivative minimum DrightThen, then
Figure BDA0002653262950000023
Further, in step S6, the calculation results in the center position M of the moon spectral image at the left edge1And the center position M of the moon spectral image at the right edge2In particular to the method for preparing the nano-particles,
integrating the moon spectral image positioned at the left edge in the spectral dimension direction to obtain an integral curve, then deriving the integral curve to obtain a derivative maximum value and a derivative minimum value, and averaging the derivative maximum value and the derivative minimum value to obtain the central position M of the moon spectral image positioned at the left edge1；
Integrating the moon spectral image positioned at the right edge in the spectral dimension direction to obtain an integral curve, then deriving the integral curve to obtain a derivative maximum value and a derivative minimum value, and averaging the derivative maximum value and the derivative minimum value to obtain the central position M of the moon spectral image positioned at the right edge2。
Further, in step S8, specifically,
s8.1, during the nth observation, calculating the right ascension coordinate Ra of the moon at the moment according to a moon position formulanAnd declination coordinate DecnWherein n is an integer greater than or equal to 2;
s8.2, adjusting the declination coordinate of the equatorial telescope to enable the moon spectral image to be positioned at the center of the view field of the slit spectrometer, and calculating the center position M of the moon spectral image at the momentnAnd recording the moon spectral image width L at the momentn；
S8.3, calculating the right ascension error compensation dra at the momentnAnd declination error compensation ddecn：
dran＝pra*(Lmax-Ln)
ddecn＝pdec(Mn-M0)
S8.4, calculating to obtain the accurate right ascension coordinate Ra of the moon at the momentn is repairedAnd precise declination coordinate Decn is repaired：
Ran is repaired＝Ran+dRan-1+dran
Decn is repaired＝Decn+dDecn-1+ddecn
Wherein, when n is more than 2,
dRan-1＝dRan-2+dran-2
dDecn-1＝dDecn-2+ddecn-2；
wherein, dRan-1The accumulated right ascension error of the equatorial telescope is observed for the first n-1 times; dRan-2The accumulated right ascension error of the equatorial telescope is observed for the first n-2 times; dDecn-1The accumulated declination error of the equatorial telescope is observed for the first n-1 times; dDecn-2The accumulated declination error of the equatorial telescope is observed for the first n-2 times;
when n is equal to 2, the compound is,
dRan-1＝dran-1
dDecn-1＝ddecn-1；
s8.5, according to the accurate right ascension coordinate Ran is repairedAnd precise declination coordinate Decn is repairedAnd correcting the right ascension coordinates and the declination coordinates of the equatorial telescope to finish positioning.
Compared with the prior art, the invention has the beneficial effects that:
1. according to the slit type spectrometer moon positioning method, by establishing the corresponding relation between the change of the moon image of the slit type spectrometer and the change of the right ascension coordinates and the declination coordinates of the equatorial telescope serving as the turntable, the equatorial telescope can be accurately corrected in the moon positioning process, the pointing error of the equatorial telescope is avoided, the moon calibration accuracy is improved, and the problem of accurate positioning of the slit type spectrometer on the moon is solved; in addition, the positioning method has strong robustness, and facilitates automatic implementation of moon positioning and equatorial instrument correction in the subsequent observation process.
2. Before formal positioning is started, polar axis calibration and one-star correction are carried out on the equatorial telescope, an internal coordinate system of the equatorial telescope is initialized, and errors accumulated by the equatorial telescope are avoided.
3. The lunar right ascension coordinates and the declination coordinates at the current moment are preferably obtained through an SAMPA algorithm, and the SAMPA algorithm can output the current date, the current moment and the altitude and is rich in acquired information.
Drawings
FIG. 1 is a schematic diagram of a lunar spectral image at the widest state in a slit-type spectrometer according to an embodiment of the present invention;
FIG. 2 is a schematic diagram of a lunar spectrum image in a state of one-fifth widest width in a slit-type spectrometer according to an embodiment of the present invention;
FIG. 3 is a spectral dimension direction integral curve of a moon spectral image according to an embodiment of the present invention;
FIG. 4 is a diagram illustrating the derivation of the spectral dimension direction integral curve to obtain the maximum and minimum values according to an embodiment of the present invention;
FIG. 5 is a schematic diagram of a moon spectral image at the left edge of a slit spectrometer according to an embodiment of the present invention;
FIG. 6 is a schematic diagram of a moon spectral image at the right edge of a slit spectrometer according to an embodiment of the present invention.
Detailed Description
The technical solution of the present invention will be clearly and completely described below with reference to the embodiments of the present invention and the accompanying drawings, and it is obvious that the described embodiments do not limit the present invention.
The invention provides a moon positioning method of a slit type spectrometer, which establishes a corresponding relation between the image change of a moon of the spectrometer and the changes of the right ascension and declination coordinates of a turntable of an equatorial telescope, realizes the accurate positioning of the moon by the slit type spectrometer and provides guarantee for long-period automatic ground-based moon observation.
Specifically, before the start of observation, the right ascension correction coefficient pra and the declination correction coefficient pdec are calculated:
(1) the method comprises the steps of selecting an equatorial instrument as a rotary table for observing the moon by a slit type spectrometer, carrying out initialization operation of polar axis calibration and one-star correction on the equatorial instrument before observation is started, and initializing an internal coordinate system of the equatorial instrument.
(2) Calculating and calculating a lunar right ascension coordinate Ra and a declination coordinate Dec of the moon at the current moment according to a moon position formula, controlling an equatorial telescope to point to the moon, and performing coarse positioning; the lunar Position formula can adopt a Solar and Moon Position Algorithm (SAMPA) Algorithm, the output parameters are the current date, the time, the longitude and latitude coordinates and the altitude of the observation point, and the output result is the lunar right ascension and declination coordinates of the observation point at the current time.
(3) Finely adjusting the right ascension coordinates and declination coordinates of the equatorial telescope to enable the lunar spectrum image to completely appear in the view field of the slit-type spectrometer;
(4) firstly, adjusting declination coordinates of an equatorial telescope to enable a moon spectral image to be positioned at the center of a view field of a slit type spectrometer, and calculating the center position M of the moon spectral image at the moment0(ii) a And then adjusting the right ascension coordinate of the equatorial telescope to change the lunar spectrum image from the widest width shown in figure 1 to the one fifth width of the widest width shown in figure 2, and recording the right ascension coordinate ra of the equatorial telescope when the lunar spectrum image is widestmaxAnd calculating the width L of the moon spectral image at the momentmaxAnd equatorial ascension coordinate ra at the narrowest lunar spectral imageminAnd calculating the width L of the moon spectral image at the momentmin；
Calculating a right ascension correction coefficient pra between the coordinates of the right ascension of the equatorial telescope and the coordinates of the lunar spectral image:
Figure BDA0002653262950000051
(5) firstly, adjusting the right ascension coordinate of the equatorial telescope to enable the lunar spectrum image to be moderate in width, then adjusting the declination coordinate of the equatorial telescope to enable the lunar spectrum image to move from the left side edge to the right side edge, and recording the declination coordinate dec of the equatorial telescope when the lunar spectrum image is located at the left side edge1And the equatorial declination coordinate dec of the moon spectral image at the right edge2Calculating the center position M of the moon spectral image at the left edge1And moon spectral image positionCenter position M at right edge2；
Calculating to obtain a declination correction coefficient pdec between the declination coordinate of the equatorial telescope and the moon spectrum image coordinate:
Figure BDA0002653262950000052
when the moon is observed subsequently every time, the equatorial telescope is firstly adjusted according to the right ascension correction coefficient and the declination correction coefficient, and the equatorial telescope is accurately corrected:
(1) during the nth observation, calculating the right ascension coordinate Ra of the moon at the moment according to the moon position formulanAnd declination coordinate DecnWherein n is an integer greater than or equal to 2;
(2) adjusting declination coordinates of the equatorial telescope to enable the lunar spectral image to be positioned at the center of the view field of the slit type spectrometer, and calculating the central position M of the lunar spectral image at the momentnAnd recording the moon spectral image width L at the momentn；
(3) Calculating the right ascension error compensation dra at this timenAnd declination error compensation ddecn：
dran＝pra*(Lmax-Ln)
ddecn＝pdec(Mn-M0)
(4) Calculating to obtain the accurate right ascension coordinate Ra of the moon at the momentn is repairedAnd precise declination coordinate Decn is repaired：
Ran is repaired＝Ran+dRan-1+dran
Decn is repaired＝Decn+dDecn-1+ddecn
Wherein, when n is more than 2,
dRan-1＝dRan-2+dran-2
dDecn-1＝dDecn-2+ddecn-2；
wherein, dRan-1The accumulated right ascension error of the equatorial telescope is observed for the first n-1 times; dRan-2The accumulated right ascension error of the equatorial telescope is observed for the first n-2 times; dDecn-1The accumulated declination error of the equatorial telescope is observed for the first n-1 times; dDecn-2The accumulated declination error of the equatorial telescope is observed for the first n-2 times;
when n is equal to 2, the compound is,
dRan-1＝dran-1
dDecn-1＝ddecn-1；
according to the precise right ascension coordinate Ran is repairedAnd precise declination coordinate Decn is repairedAnd correcting the right ascension coordinates and the declination coordinates of the equatorial telescope to finish positioning.
Because the errors of the rough right ascension coordinates and declination coordinates calculated by the lunar position formula and the real position are larger and larger, the moon can not be seen by only using the lunar position formula. Therefore, in each observation, the deviation compensation calculated in the previous observation is added, and the moon can be ensured to appear in the field of view by taking the deviation compensation as the initial position of the observation, which is a process of error accumulation compensation.
The following is an example of actual observation using the method of the invention for monthly positioning:
manually controlling the equatorial telescope to move the lunar spectral image to the center of the image to enable the width of the lunar spectral image to reach the maximum state, wherein the slit is positioned at the widest position of the moon, and the right ascension coordinate ra of the equatorial telescopemax7.6639. Integrating the moon spectral image in the spectral dimension direction to obtain an integral curve, and then deriving the integral curve to obtain a derivative maximum value DleftAnd derivative minimum DrightThen, then
Figure BDA0002653262950000061
Calculating to obtain M0At the same time, the moon spectral image width L is recorded at 250 deg.fmax＝260。
The right ascension coordinate of the equatorial telescope is adjusted to make the width of the lunar spectral image about one fifth of the widest time, and the width L of the lunar spectral image is adjustedmin60, in this caseRight ascension coordinate ramin＝7.6906。
According to
Figure BDA0002653262950000071
Calculated pra is 1.334e-4。
Adjusting the declination coordinate of the equatorial telescope to move the lunar spectrum image from the left edge as shown in figure 5 to the right edge as shown in figure 5, and recording the declination coordinate dec of the equatorial telescope when the lunar spectrum image is positioned at the left edge1And the equatorial declination coordinate dec of the moon spectral image at the right edge2Calculating the center position M of the moon spectral image at the left edge1And the center position M of the moon spectral image at the right edge2；
Wherein, the center position M of the moon spectrum image when being positioned at the left edge1And the center position M of the moon spectral image at the right edge2The specific calculation method is as follows:
integrating the moon spectral image positioned at the left edge in the spectral dimension direction to obtain an integral curve, then deriving the integral curve to obtain a derivative maximum value and a derivative minimum value, and averaging the derivative maximum value and the derivative minimum value to obtain the central position M of the moon spectral image positioned at the left edge1；
Integrating the moon spectral image positioned at the right edge in the spectral dimension direction to obtain an integral curve as shown in fig. 3, then deriving the integral curve to obtain a derivative maximum value and a derivative minimum value as shown in fig. 4, and averaging the derivative maximum value and the derivative minimum value to obtain the central position M of the moon spectral image positioned at the right edge2；
The calculated pdec is 2.74e-3。
In the 5 th formal observation, the right ascension coordinate Ra of the moon at the moment is calculated according to the moon position formula57.7856 and declination coordinate Dec5Adjusting the declination coordinate of the equatorial telescope to 22.5833 to obtain a lunar spectrum imageIs positioned at the center of the field of view of the slit type spectrometer, and calculates the center position M of the moon spectral image at the moment5255 f, and recording the moon spectral image width L at this time5246; obtaining dRa through the first 4 times of observation4＝0.0184，dDec40.1423; calculating the right ascension error compensation dra at this time50.0019, compensating ddec for declination error5＝0.0137。
At this moment, the precise right ascension coordinate Ra of the moonRepair 5：
RaRepair 5＝Ra5+dRa4+dra5＝7.7856+0.0184+0.0019＝7.8059
Precise declination coordinates of the moon:
Decrepair 5＝Dec5+dDec4+ddec5＝22.5833+0.1423+0.0137＝22.7393
The equatorial telescope is adjusted in turn so that it points precisely towards the moon.
In the case of the first observation, the accumulated error does not need to be considered, and in the case of the second observation, the accumulated error of the first observation only needs to be considered.
The equatorial telescope can adopt an equatorial telescope with the maximum load of 50kg, the polar axis and the declination axis are both provided with synchronous motors, the automatic control of double axes can be realized, in addition, an ascom standard astronomy interface is adopted, and the synchronization and the pointing of the equatorial telescope can be controlled by inputting the absolute coordinates of the right ascension and the declination.
By verification, the moon can be accurately observed by adopting the moon positioning method, the accumulated error can be fully considered, and the result is accurate.
The above description is only an embodiment of the present invention, and is not intended to limit the scope of the present invention, and all equivalent structural changes made by using the contents of the present specification and the drawings, or applied directly or indirectly to other related technical fields, are included in the scope of the present invention.

Claims (6)

1.一种狭缝型光谱仪对月定位方法，其特征在于，包括以下步骤：1. a slit type spectrometer to the moon positioning method, is characterized in that, comprises the following steps: S1，根据月球位置公式计算当前时刻月球赤经坐标Ra和赤纬坐标Dec；S1, calculate the moon's right ascension coordinate Ra and declination coordinate Dec at the current moment according to the lunar position formula; S2，以赤道仪作为狭缝型光谱仪对月观测的转台；根据当前时刻月球赤经坐标Ra和赤纬坐标Dec，控制赤道仪指向月球，作为粗定位；S2, use the equatorial mount as the turntable for the slit spectrometer to observe the moon; control the equatorial mount to point to the moon according to the moon's right ascension coordinate Ra and declination coordinate Dec at the current moment, as a rough positioning; S3，调整赤道仪的赤经坐标和赤纬坐标，使月球光谱图像完全出现在狭缝型光谱仪的视场内；S3, adjust the right ascension and declination coordinates of the equatorial mount, so that the lunar spectral image completely appears in the field of view of the slit spectrometer; S4，调整赤道仪的赤纬坐标，使月球光谱图像位于狭缝型光谱仪的视场中心处，计算此时月球光谱图像中心位置M0；调整赤道仪赤经坐标使月球光谱图像达到最宽，计算此时月球光谱图像宽度Lmax，再调整赤道仪的赤经坐标，使月球光谱图像由最宽变为最宽的五分之一，计算此时月球光谱图像宽度Lmin，同时，记录月球光谱图像最宽时的赤道仪赤经坐标ramax和月球光谱图像为最宽的五分之一时的赤道仪赤经坐标ramin；S4, adjust the declination coordinates of the equatorial mount so that the lunar spectral image is located at the center of the field of view of the slit spectrometer, and calculate the center position M 0 of the lunar spectral image at this time; adjust the right ascension coordinates of the equatorial mount to make the lunar spectral image reach the widest Calculate the width L max of the lunar spectral image at this time, and then adjust the right ascension coordinates of the equatorial mount to make the lunar spectral image change from the widest to one-fifth of the widest, calculate the lunar spectral image width L min at this time, and record the lunar spectral image at this time. The equatorial mount right ascension coordinate ra max when the spectral image is the widest and the equatorial mount right ascension coordinate ra min when the lunar spectral image is the widest one-fifth; S5，计算赤道仪赤经坐标与月球光谱图像坐标之间的赤经修正系数pra：S5, calculate the right ascension correction coefficient pra between the equatorial mount right ascension coordinates and the lunar spectral image coordinates:
Figure FDA0002653262940000011
Figure FDA0002653262940000011
 S6，调整赤道仪的赤纬坐标，使月球光谱图像由左侧边缘移动至右侧边缘，记录月球光谱图像位于左侧边缘时的赤道仪赤纬坐标dec1和月球光谱图像位于右侧边缘时的赤道仪赤纬坐标dec2，计算得到月球光谱图像位于左侧边缘时的中心位置M1和月球光谱图像位于右侧边缘时的中心位置M2；S6, adjust the declination coordinates of the equatorial mount so that the lunar spectral image moves from the left edge to the right edge, and record the declination coordinates dec 1 of the equatorial mount when the lunar spectral image is located on the left edge and when the lunar spectral image is located on the right edge the declination coordinates dec 2 of the equatorial mount, and calculate the center position M 1 when the lunar spectral image is located on the left edge and the center position M 2 when the lunar spectral image is located on the right edge; S7，计算得到赤道仪赤纬坐标与月球光谱图像坐标之间的赤纬修正系数pdec：S7, calculate the declination correction coefficient pdec between the declination coordinates of the equatorial mount and the lunar spectral image coordinates:
Figure FDA0002653262940000012
Figure FDA0002653262940000012
 S8，每次观测时，根据经步骤S5得到的赤经修正系数pra和经步骤S7计算得到的赤纬修正系数pdec，修正赤道仪赤经坐标和赤纬坐标，完成定位。S8 , correct the right ascension coordinates and declination coordinates of the equatorial mount according to the right ascension correction coefficient pra obtained through step S5 and the declination correction coefficient pdec obtained through step S7 for each observation to complete the positioning. 2.如权利要求1所述一种狭缝型光谱仪对月定位方法，其特征在于，所述步骤S1之前还包括步骤S0，对赤道仪进行极轴校准和一星校正。2 . The method for locating the moon with a slit spectrometer according to claim 1 , wherein, before the step S1 , it further comprises a step S0 of performing polar axis calibration and one-star calibration on the equatorial mount. 3 . 3.如权利要求1所述一种狭缝型光谱仪对月定位方法，其特征在于，步骤S2中，所述当前时刻月球赤经坐标Ra和赤纬坐标Dec具体是通过SAMPA算法计算得到的。3. a kind of slit type spectrometer as claimed in claim 1 is characterized in that, in step S2, described current moment lunar right ascension coordinate Ra and declination coordinate Dec are specifically calculated by SAMPA algorithm. 4.如权利要求1所述一种狭缝型光谱仪对月定位方法，其特征在于，步骤S4中，所述计算此时月球光谱图像中心位置M0具体为，对此时月球光谱图像在光谱维方向进行积分，得到积分曲线，再对所述积分曲线求导，得到导数最大值Dleft和导数最小值Dright，则4. a kind of slit-type spectrometer as claimed in claim 1 is characterized in that, in step S4, described calculating this moment lunar spectral image center position M 0 is specifically, to this moment lunar spectral image is in spectrum. Integrate in the dimensional direction to obtain the integral curve, and then derive the integral curve to obtain the maximum derivative D left and the minimum derivative D right , then
Figure FDA0002653262940000021
Figure FDA0002653262940000021
 5.如权利要求1所述一种狭缝型光谱仪对月定位方法，其特征在于，步骤S6中，所述计算得到月球光谱图像位于左侧边缘时的中心位置M1和月球光谱图像位于右侧边缘时的中心位置M2的具体方法为：5. a kind of slit type spectrometer as claimed in claim 1 to the moon positioning method, it is characterised in that in step S6, described calculation obtains that the central position M when the lunar spectral image is positioned on the left edge and the lunar spectral image is positioned on the right side. The specific method of the center position M 2 when the side edge is: 对位于左侧边缘时的月球光谱图像在光谱维方向进行积分，得到积分曲线，再对所述积分曲线求导，得到导数最大值和导数最小值，对导数最大值和导数最小值求均值，即得到月球光谱图像位于左侧边缘时的中心位置M1；Integrate the lunar spectral image at the left edge in the spectral dimension to obtain an integral curve, and then derive the integral curve to obtain the maximum derivative value and the minimum derivative value, and average the maximum derivative value and the minimum derivative value, That is, the center position M 1 when the lunar spectral image is located at the left edge is obtained; 对位于右侧边缘时的月球光谱图像在光谱维方向进行积分，得到积分曲线，再对所述积分曲线求导，得到导数最大值和导数最小值，对导数最大值和导数最小值求均值，即得到月球光谱图像位于右侧边缘时的中心位置M2。Integrate the lunar spectral image at the right edge in the spectral dimension to obtain an integral curve, and then derive the integral curve to obtain the maximum derivative value and the minimum derivative value, and average the maximum derivative value and the minimum derivative value, That is, the center position M 2 of the lunar spectral image at the right edge is obtained. 6.如权利要求1所述一种狭缝型光谱仪对月定位方法，其特征在于，步骤S8具体为：6. a kind of slit spectrometer as claimed in claim 1 is characterized in that, step S8 is specifically: S8.1，第n次观测时，根据月球位置公式计算此时月球的赤经坐标Ran和赤纬坐标Decn，其中，n为大于等于2的整数；S8.1, during the nth observation, calculate the right ascension coordinate Ra n and the declination coordinate Dec n of the moon at this time according to the moon position formula, where n is an integer greater than or equal to 2; S8.2，调整赤道仪的赤纬坐标，使月球光谱图像位于狭缝型光谱仪的视场中心处，计算此时月球光谱图像中心位置Mn，并记录此时月球光谱图像宽度Ln；S8.2, adjust the declination coordinates of the equatorial mount so that the lunar spectral image is located at the center of the field of view of the slit spectrometer, calculate the center position M n of the lunar spectral image at this time, and record the width L n of the lunar spectral image at this time; S8.3，计算此时的赤经误差补偿dran和赤纬误差补偿ddecn：S8.3, calculate the right ascension error compensation dran and declination error compensation ddec n at this time: dran＝pra*(Lmax-Ln)dra n =pra*(L max -L n ) ddecn＝pdec(Mn-M0)ddec n =pdec(M n -M 0 ) S8.4，计算得到此时月球的精准赤经坐标Ran修和精准赤纬坐标Decn修：In S8.4, the precise right ascension coordinates Ra n and the precise declination coordinates Dec n of the moon at this time are calculated and obtained: Ran修＝Ran+dRan-1+dran Ra n repair = Ra n +dRa n -1 +dran Decn修＝Decn+dDecn-1+ddecn Dec n repair = Dec n +dDec n-1 +ddec n 其中，当n＞2时，Among them, when n>2, dRan-1＝dRan-2+dran-2 dRa n-1 =dRa n-2 +dra n-2 dDecn-1＝dDecn-2+ddecn-2；dDec n-1 =dDec n-2 +ddec n-2 ; 其中，dRan-1为前n-1次观测赤道仪的累积赤经误差；dRan-2为前n-2次观测赤道仪的累积赤经误差；dDecn-1为前n-1次观测赤道仪的累积赤纬误差；Among them, dRa n-1 is the accumulated right ascension error of the first n-1 observations of the equatorial mount; dRa n-2 is the accumulated right ascension error of the first n-2 observations of the equatorial mount; dDec n-1 is the first n-1 observations Observing the cumulative declination error of the equatorial mount; dDecn-2为前n-2次观测赤道仪的累积赤纬误差；dDec n-2 is the accumulated declination error of the first n-2 observations of the equatorial mount; 当n＝2时，When n=2, dRan-1＝dran-1 dRa n-1 =dra n-1 dDecn-1＝ddecn-1；dDec n-1 =ddec n-1 ; S8.5，根据精准赤经坐标Ran修和精准赤纬坐标Decn修修正赤道仪的赤经坐标和赤纬坐标，完成定位。S8.5, correct the right ascension coordinates and declination coordinates of the equatorial mount according to the precise right ascension coordinates Ra n and the precise declination coordinates Dec n to complete the positioning.
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