CN112097907A - Moon positioning method of slit type spectrometer - Google Patents
Moon positioning method of slit type spectrometer Download PDFInfo
- Publication number
- CN112097907A CN112097907A CN202010878151.2A CN202010878151A CN112097907A CN 112097907 A CN112097907 A CN 112097907A CN 202010878151 A CN202010878151 A CN 202010878151A CN 112097907 A CN112097907 A CN 112097907A
- Authority
- CN
- China
- Prior art keywords
- moon
- coordinate
- declination
- spectral image
- lunar
- Prior art date
- Legal status (The legal status is an assumption and is not a legal conclusion. Google has not performed a legal analysis and makes no representation as to the accuracy of the status listed.)
- Granted
Links
- PEDCQBHIVMGVHV-UHFFFAOYSA-N Glycerine Chemical compound OCC(O)CO PEDCQBHIVMGVHV-UHFFFAOYSA-N 0.000 title claims abstract description 118
- 238000000034 method Methods 0.000 title claims abstract description 26
- 230000003595 spectral effect Effects 0.000 claims abstract description 81
- 238000001228 spectrum Methods 0.000 claims description 32
- 238000012937 correction Methods 0.000 claims description 18
- 238000012935 Averaging Methods 0.000 claims description 6
- 238000004422 calculation algorithm Methods 0.000 claims description 6
- 150000001875 compounds Chemical class 0.000 claims description 3
- 230000009466 transformation Effects 0.000 abstract description 6
- 238000010586 diagram Methods 0.000 description 5
- 238000004364 calculation method Methods 0.000 description 3
- 230000005855 radiation Effects 0.000 description 3
- 238000009825 accumulation Methods 0.000 description 1
- 230000009286 beneficial effect Effects 0.000 description 1
- 238000009795 derivation Methods 0.000 description 1
- 238000011161 development Methods 0.000 description 1
- 238000003384 imaging method Methods 0.000 description 1
- 239000002105 nanoparticle Substances 0.000 description 1
- 230000003287 optical effect Effects 0.000 description 1
- 238000011160 research Methods 0.000 description 1
- 230000001360 synchronised effect Effects 0.000 description 1
- 238000012795 verification Methods 0.000 description 1
Images
Classifications
-
- G—PHYSICS
- G01—MEASURING; TESTING
- G01J—MEASUREMENT OF INTENSITY, VELOCITY, SPECTRAL CONTENT, POLARISATION, PHASE OR PULSE CHARACTERISTICS OF INFRARED, VISIBLE OR ULTRAVIOLET LIGHT; COLORIMETRY; RADIATION PYROMETRY
- G01J3/00—Spectrometry; Spectrophotometry; Monochromators; Measuring colours
- G01J3/28—Investigating the spectrum
-
- G—PHYSICS
- G06—COMPUTING; CALCULATING OR COUNTING
- G06F—ELECTRIC DIGITAL DATA PROCESSING
- G06F17/00—Digital computing or data processing equipment or methods, specially adapted for specific functions
- G06F17/10—Complex mathematical operations
Landscapes
- Physics & Mathematics (AREA)
- Engineering & Computer Science (AREA)
- General Physics & Mathematics (AREA)
- Mathematical Physics (AREA)
- Data Mining & Analysis (AREA)
- Theoretical Computer Science (AREA)
- Spectroscopy & Molecular Physics (AREA)
- Computational Mathematics (AREA)
- Mathematical Analysis (AREA)
- Mathematical Optimization (AREA)
- Algebra (AREA)
- Pure & Applied Mathematics (AREA)
- Databases & Information Systems (AREA)
- Software Systems (AREA)
- General Engineering & Computer Science (AREA)
- Spectrometry And Color Measurement (AREA)
Abstract
The invention relates to a moon calibration method, aiming at solving the technical problems that when a slit type spectrometer, an equatorial telescope and a star finder are matched for carrying out ground-based moon calibration, spectral image transformation is established, and the corresponding relation of equatorial telescope red longitude and red latitude coordinate transformation is difficult, so that the observation error is large.
Description
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 spectral image widest, and calculating the width L of the lunar spectral image at the momentmaxAnd 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:
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:
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 calculation of the moon spectral image center position M at this time is performed0Specifically, 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
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, according to the position of the moonThe right ascension coordinate Ra of the moon at the moment is calculatednAnd 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:
(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 the center position M of the moon spectral image at the right edge2；
Calculating to obtain a declination correction coefficient pdec between the declination coordinate of the equatorial telescope and the moon spectrum image coordinate:
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 derivativeMaximum value DleftAnd derivative minimum DrightThen, then
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, right ascension coordinate ramin＝7.6906。
According to
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；
For the moon spectral image positioned at the right edge in the spectral dimension directionIntegrating to obtain an integral curve as shown in FIG. 3, 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 a central position M of the moon spectral image 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 Dec522.5833, adjusting the declination coordinate of the equatorial telescope to make the moon spectrum image be positioned at the center of the view field of the slit spectrometer, and calculating the center position M of the moon spectrum 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. A method for positioning moon by 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 spectral image widest, and calculating the width L of the lunar spectral image at the momentmaxAnd 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 ascension coordinate ra when the moon spectral image is one fifth of the widestmin；
And S5, 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:
s6, adjusting the declination coordinate of the equatorial telescope to make the moonMoving the spectrum image from the left edge to the right edge, and recording the equatorial declination coordinate dec of the moon spectrum image 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 pdec between the declination coordinate of the equatorial telescope and the moon spectrum image coordinate:
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.
2. The method for lunar positioning by a slit spectrometer as claimed in claim 1, wherein the step S1 is preceded by a step S0 of polar axis calibration and one-star calibration of the equatorial telescope.
3. The method for locating the moon by using a slit-type spectrometer as claimed in claim 1, wherein in step S2, the lunar right ascension coordinate Ra and the declination coordinate Dec at the current time are calculated by a SAMPA algorithm.
4. The method for locating the moon in a slit spectrometer as claimed in claim 1, wherein the step S4 is performed by calculating the center M of the moon spectral image at the time0Specifically, 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
5. The method for locating the moon in a slit spectrometer as claimed in claim 1, wherein the step S6 is performed by calculating the center position M of the moon spectrum image at the left edge1And the center position M of the moon spectral image at the right edge2The specific method comprises the following steps:
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。
6. The method for lunar positioning by a slit spectrometer as claimed in claim 1, wherein the step S8 specifically comprises:
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.
Priority Applications (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN202010878151.2A CN112097907B (en) | 2020-08-27 | 2020-08-27 | Moon positioning method of slit type spectrometer |
Applications Claiming Priority (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN202010878151.2A CN112097907B (en) | 2020-08-27 | 2020-08-27 | Moon positioning method of slit type spectrometer |
Publications (2)
| Publication Number | Publication Date |
|---|---|
| CN112097907A true CN112097907A (en) | 2020-12-18 |
| CN112097907B CN112097907B (en) | 2021-06-22 |
Family
ID=73757963
Family Applications (1)
| Application Number | Title | Priority Date | Filing Date |
|---|---|---|---|
| CN202010878151.2A Active CN112097907B (en) | 2020-08-27 | 2020-08-27 | Moon positioning method of slit type spectrometer |
Country Status (1)
| Country | Link |
|---|---|
| CN (1) | CN112097907B (en) |
Citations (8)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN101281060A (en) * | 2008-04-30 | 2008-10-08 | 大连理工大学 | Sky polarized light radiation spectrum measuring systems |
| US7671985B1 (en) * | 2006-03-13 | 2010-03-02 | Milan Milosevic | Device for small spot analysis using fiber optic interfaced spectrometers |
| KR20130054021A (en) * | 2011-11-16 | 2013-05-24 | 황인준 | Altitude adjusting apparatus of equatorial mount for astronomical telescope |
| CN105067115A (en) * | 2015-07-15 | 2015-11-18 | 中国科学院长春光学精密机械与物理研究所 | Method for performing ground-based moon observation by means of split type imaging spectrometer |
| CN105092033A (en) * | 2015-07-15 | 2015-11-25 | 中国科学院长春光学精密机械与物理研究所 | Ground-based moon observation apparatus by using slit type imaging spectrometer |
| CN105387996A (en) * | 2015-10-29 | 2016-03-09 | 中国科学院长春光学精密机械与物理研究所 | Optical axis consistency calibration method for multi-optical axis ground star observation system |
| CN207600598U (en) * | 2017-09-21 | 2018-07-10 | 中国科学院云南天文台 | The atmospheric parameter monitoring device of the big visual field sky imaging technique of multiband |
| RU2692350C1 (en) * | 2018-07-19 | 2019-06-24 | Федеральное государственное бюджетное учреждение науки Институт астрономии Российской академии наук | Method for high-accuracy positioning of apparatus on moon surface and device for its implementation |
-
2020
- 2020-08-27 CN CN202010878151.2A patent/CN112097907B/en active Active
Patent Citations (8)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| US7671985B1 (en) * | 2006-03-13 | 2010-03-02 | Milan Milosevic | Device for small spot analysis using fiber optic interfaced spectrometers |
| CN101281060A (en) * | 2008-04-30 | 2008-10-08 | 大连理工大学 | Sky polarized light radiation spectrum measuring systems |
| KR20130054021A (en) * | 2011-11-16 | 2013-05-24 | 황인준 | Altitude adjusting apparatus of equatorial mount for astronomical telescope |
| CN105067115A (en) * | 2015-07-15 | 2015-11-18 | 中国科学院长春光学精密机械与物理研究所 | Method for performing ground-based moon observation by means of split type imaging spectrometer |
| CN105092033A (en) * | 2015-07-15 | 2015-11-25 | 中国科学院长春光学精密机械与物理研究所 | Ground-based moon observation apparatus by using slit type imaging spectrometer |
| CN105387996A (en) * | 2015-10-29 | 2016-03-09 | 中国科学院长春光学精密机械与物理研究所 | Optical axis consistency calibration method for multi-optical axis ground star observation system |
| CN207600598U (en) * | 2017-09-21 | 2018-07-10 | 中国科学院云南天文台 | The atmospheric parameter monitoring device of the big visual field sky imaging technique of multiband |
| RU2692350C1 (en) * | 2018-07-19 | 2019-06-24 | Федеральное государственное бюджетное учреждение науки Институт астрономии Российской академии наук | Method for high-accuracy positioning of apparatus on moon surface and device for its implementation |
Non-Patent Citations (1)
| Title |
|---|
| 王阳等: "利用恒星对天文观测系统光轴平行性检校", 《红外与激光工程》 * |
Also Published As
| Publication number | Publication date |
|---|---|
| CN112097907B (en) | 2021-06-22 |
Similar Documents
| Publication | Publication Date | Title |
|---|---|---|
| EP2472471B1 (en) | System and method for automatically aligning a telescope without requiring user intervention | |
| CN113900125B (en) | Satellite-ground combined linear array imaging remote sensing satellite full-autonomous geometric calibration method and system | |
| CN111238485B (en) | System error self-compensation method for shooting Mars image based on navigation sensor | |
| CN105698766A (en) | Satellite image RFM model block adjustment method with orientation parameter precision information taken into consideration | |
| CN112097907B (en) | Moon positioning method of slit type spectrometer | |
| CN114838740A (en) | Satellite image geometric calibration method considering different longitude and latitude areas | |
| CN115311365A (en) | High-precision on-orbit geometric positioning method for long-linear-array swinging camera | |
| Cheng et al. | New on-orbit geometric interior parameters self-calibration approach based on three-view stereoscopic images from high-resolution multi-TDI-CCD optical satellites | |
| CN112097794B (en) | Calibration method and system for remote sensing satellite load platform | |
| Yang et al. | Joint estimation of stellar atmospheric refraction and star tracker attitude | |
| CN116465432A (en) | Course error-based four-position horizontal gyro zero bias residual error compensation method | |
| Wallace et al. | Alignment, pointing accuracy and field rotation of the UK 1.2-m Schmidt telescope | |
| CN116718182A (en) | Satellite attitude determination method based on extended Kalman filtering | |
| CN115689915A (en) | Method for realizing geometric distortion correction of on-orbit star map based on two-dimensional Legendre neural network and star sensor | |
| CN112378372B (en) | Star radius curvature correction method for meridian weft measurement of multifunctional astronomical theodolite | |
| CN109443380B (en) | Thermal deformation error correction method for optical camera with geostationary orbit | |
| CN109506645B (en) | Star sensor mounting matrix ground accurate measurement method | |
| CN114838739A (en) | Satellite image geometric calibration method considering complete regression cycle | |
| CN113776560A (en) | Gyro scale factor testing method based on high-precision three-axis turntable | |
| Colditz et al. | Boresight calibration of FIFI-LS: in theory, in the lab and on sky | |
| CN112070822B (en) | Synchronization method for equatorial telescope for lunar observation of foundation | |
| CN114280773B (en) | Astronomical telescope calibration method and device | |
| CN115371669A (en) | Calibration method, system and storage medium of laser inertial navigation | |
| CN115586640B (en) | Mounting and adjusting method and device for step-by-step calculation of coaxial two-inverse system | |
| CN117572463A (en) | Geometric calibration method for low-orbit area array imaging satellite with two-dimensional turntable |
Legal Events
| Date | Code | Title | Description |
|---|---|---|---|
| PB01 | Publication | ||
| PB01 | Publication | ||
| SE01 | Entry into force of request for substantive examination | ||
| SE01 | Entry into force of request for substantive examination | ||
| GR01 | Patent grant | ||
| GR01 | Patent grant |