CN117606511A - Pointing model correction method, system, equipment and medium for horizon telescope - Google Patents
Pointing model correction method, system, equipment and medium for horizon telescope Download PDFInfo
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Abstract
The invention provides a pointing model correction method, a pointing model correction system, pointing model correction equipment and pointing model correction media for a horizontal telescope, and relates to the field of horizontal telescopes. It comprises the following steps: and selecting uniformly distributed star targets from a preset star table to obtain a target test object. Recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data. Based on the preset matrix data, corresponding coefficient item data are calculated. The coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on preset matrix data. The scheme can improve the pointing precision of the horizontal telescope, and further improve the operation efficiency of the telescope.
Description
Technical Field
The invention relates to the field of horizon telescopes, in particular to a method, a system, equipment and a medium for correcting a pointing model of a horizon telescope.
Background
Along with the continuous innovation of the modern manufacturing level, the processing and assembling process of the optical telescope is continuously improved, and the assembling error is continuously reduced, but the pointing deviation of the telescope is still one of important indexes for measuring a telescope. Therefore, in the prior art, a scheme of correcting the pointing error of the optical telescope by software is proposed, that is, by analyzing various error factors and repeatability rules affecting the operation of the telescope, the position change of the observed celestial body on the detector is recorded, and the functional relationship and model between the azimuth and the pitching of the observed celestial body are established. After the solved telescope pointing model coefficient is imported into a telescope control system through computer software, the pointing precision of an observation target is improved.
Common methods of correcting pointing errors of optical telescopes by software include error correction using spherical harmonic models or basic parametric models. Although the spherical harmonic model can reflect the distribution rule of the star targets on the sphere, the spherical harmonic is a pure mathematical model, the correlation between model coefficients under different collected samples is poor, the model is unstable, and the pointing model coefficients need to be recalibrated after the telescope is observed and operated for a period of time. In addition, although each coefficient item in the basic parameter model has clear physical meaning, the azimuth axis residual error data of the basic parameter model has obvious system error trend.
Disclosure of Invention
The invention aims to provide a pointing model correction method, a pointing model correction system, pointing model correction equipment and a pointing model correction medium for a horizontal telescope, which can improve the pointing precision of the horizontal telescope and further improve the operation efficiency of the telescope.
The invention is realized in the following way:
in a first aspect, the present application provides a method for correcting an orientation model of a horizontal telescope, including the following steps:
and selecting uniformly distributed star targets from a preset star table to obtain a target test object. And recording preset matrix data of the target test object in the CCD view field, wherein the preset matrix data comprise the actual azimuth position of the target test object in the CCD view field, the actual elevation position of the target test object in the CCD view field, the azimuth position of the target test object in the center of the CCD view field, the elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data. And calculating corresponding coefficient item data based on the preset matrix data. The coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on the preset matrix data.
Further, based on the foregoing scheme, the step of bringing the coefficient term data into the gantry pointing model to correct the telescope specifically includes: the coefficient item data are brought into a frame pointing model, and the conformity is verified; if the verification result is not in conformity, adding a target test object, and transferring to a step of recording preset matrix data of the target test object in the CCD field of view; otherwise, correcting the telescope based on the coefficient item data.
Further, based on the foregoing scheme, the step of bringing the coefficient item data into the gantry pointing model and verifying the conformity includes:
and the coefficient item data are brought into a frame pointing model, and the precision value of the azimuth axis and the precision value of the pitching axis are calculated. And judging whether the coefficient item data meets the preset coincidence degree requirement or not based on the comparison relation between the precision value of the azimuth axis and the first threshold value and the comparison relation between the precision value of the elevation axis and the second threshold value.
Further, based on the foregoing scheme, the mathematical formula of the gantry pointing model includes:
ΔAcosE＝d 1 -d 3 cosAtanE-d 4 sinAtanE+d 5 secE-d 6 tanE+d 7 sinA+d 8 cosA+d 12 (A/2π)+d 14 sin2A+d 15 cos2A+d 20 sin2AsecE+d 21 cos2AsecE
ΔE＝d 2 +d 3 sinA-d 4 cosA+d 9 sinE+d 11 cotE+d 13 (E/2π)+d 16 sinA+d 17 cosA+d 18 EsinA+d 19 EcosA+d 22 sin2A+d 23 cos2A
wherein A is the actual azimuth position of the target test object in the CCD field of view, E is the actual pitching position of the target test object in the CCD field of view, d 1 Zero point of azimuth encoder, d 2 For pitch encoder zero, d 3 Is inclined to the north and south of the azimuth axis, d 4 Is the azimuth axisEast-west inclination, d 5 D is the visual axis difference 6 Is non-orthogonal to the azimuth axis and the elevation axis, d 7 For the first azimuth axis ellipticity, d 8 Ellipticity of second azimuth axis, d 9 For a first pitch axis ellipticity, d 10 Ellipticity of second pitch axis, d 11 D is gravity bending of telescope lens cone 12 Line error for azimuth axis encoder, d 13 Score error for pitch axis encoder, d 14 Is a periodic term in a first azimuth, d 15 Is the periodic term in the second azimuth angle, d 16 For the first pitch axis encoder stiction, d 17 For the second pitch axis encoder stiction, d 18 For the first pitch axis static resistance, d 19 Is the second pitching axis static resistance, d 20 For the first azimuthal cycle ratio, d 21 Is a second azimuthal period ratio.
Further, based on the foregoing scheme, the step of recording the preset matrix data of the target test object in the field of view of the CCD specifically includes:
extracting the right ascension value and the right ascension value of a target test object so as to point to a corresponding target position by using a telescope; the target position is a position determined by the right ascent value and the right ascent value of the target test object. And acquiring the position information of the target test object in the azimuth encoder and the pitch encoder and the off-center position information to obtain and record preset matrix data of the target test object in the CCD field of view.
Further, based on the foregoing solution, the selecting the star targets uniformly distributed in the predetermined star table, and the selecting the star targets in the step of obtaining the target test object includes: in the direction of the azimuth axis 0-360 degrees, selecting a group of fixed star targets at intervals of 30 degrees, selecting azimuth positions along the azimuth axis, and selecting a group of fixed star targets at intervals of 20 degrees in the direction of the pitching axis 0-90 degrees.
In a second aspect, the present application provides a pointing model correction system for a horizon telescope, comprising:
an acquisition module configured to: and selecting uniformly distributed star targets from a preset star table to obtain a target test object. A recording module configured to: and recording preset matrix data of the target test object in the CCD view field, wherein the preset matrix data comprise the actual azimuth position of the target test object in the CCD view field, the actual elevation position of the target test object in the CCD view field, the azimuth position of the target test object in the center of the CCD view field, the elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data. A computing module configured to: and calculating corresponding coefficient item data based on the preset matrix data. A correction module configured to: the coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on the preset matrix data.
In a third aspect, the present application provides an electronic device comprising at least one processor, at least one memory, and a data bus; wherein: the processor and the memory complete communication with each other through the data bus; the memory stores program instructions for execution by the processor, the processor invoking the program instructions to perform the method of any of the first aspects.
In a fourth aspect, the present application provides a computer readable storage medium having stored thereon a computer program which, when executed by a processor, implements a method as in any of the first aspects above.
Compared with the prior art, the invention has at least the following advantages or beneficial effects:
the invention provides a correcting method of a pointing model of a horizon telescope, which is characterized in that on the basis of a basic parameter model, the actual azimuth position of a target test object in a CCD view field, the actual elevation position of the target test object in the CCD view field, the azimuth position of the target test object in the center of the CCD view field, the elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data are introduced, so that a corresponding frame pointing model can be constructed, the telescope is corrected by the model, the pointing precision of the horizon telescope can be effectively improved, and the operating efficiency of the telescope is further improved.
Drawings
In order to more clearly illustrate the technical solutions of the embodiments of the present invention, the drawings that are needed in the embodiments will be briefly described below, it being understood that the following drawings only illustrate some embodiments of the present invention and therefore should not be considered as limiting the scope, and other related drawings may be obtained according to these drawings without inventive effort for a person skilled in the art.
FIG. 1 is a schematic diagram of residual distribution conditions under different acquisition targets when correction is performed by using a basic parameter model;
FIG. 2 is a flow chart of an embodiment of a method for correcting a pointing model of a horizontal telescope according to the present invention;
FIG. 3 is a diagram illustrating residual distribution and azimuth axis accuracy in an embodiment of the present invention;
FIG. 4 is a diagram illustrating residual distribution and pitch-and-yaw accuracy in an embodiment of the present invention;
FIG. 5 is a block diagram illustrating an embodiment of a pointing model correction system for a horizontal telescope according to the present invention;
fig. 6 is a block diagram of an electronic device according to an embodiment of the present invention.
Icon: 1. an acquisition module; 2. a recording module; 3. a computing module; 4. a correction module; 5. a processor; 6. a memory; 7. a data bus.
Detailed Description
For the purposes of making the objects, technical solutions and advantages of the embodiments of the present application more clear, the technical solutions of the embodiments of the present application will be clearly and completely described below with reference to the drawings in the embodiments of the present application, and it is apparent that the described embodiments are some embodiments of the present application, but not all embodiments. The components of the embodiments of the present application, which are generally described and illustrated in the figures herein, may be arranged and designed in a wide variety of different configurations.
Some embodiments of the present application are described in detail below with reference to the accompanying drawings. The various embodiments and features of the embodiments described below may be combined with one another without conflict.
Example 1
The conventional optical telescope pointing model is corrected by a spherical harmonic model, a basic parameter model and the like, and although the schemes can be adequate for most application scenes, the situation that model coefficients are unstable in the spherical harmonic model and the situation that system differences cannot be completely eliminated in the basic parameter model exist.
For ease of understanding, the following scheme for error correction of spherical harmonic models and basic parameter models is briefly described as follows:
(1) The scheme of correcting by utilizing spherical harmonic function model:
the sidereal targets observed by the optical telescope are celestial bodies defined on a spherical surface. Some telescope devices adopt a spherical harmonic model pointing model to correct pointing deviation of a telescope according to the distribution condition of an observed celestial body, and the spherical harmonic model has no specific physical meaning as a mathematical model. Therefore, when a spherical harmonic model fitting pointing model formula is adopted, high-order fitting is needed to reflect the characteristic that residual distribution has no obvious regional property. The fourth-order band harmonic term and the first-order field harmonic term are generally taken. Unfolding a model formula through Legend polynomials:
ΔAcosE＝m 0 +m 1 sinE+m 2 cosAcosE+m 3 sinAcosE+m 4 sin 2 E+m 5 cosAsinEcosE+m 6 sinAsinEcosE+m 7 sin 3 E+m 8 cosAsin 2 EcosE+m 9 sinAsin 2 EcosE+m 10 sin 4 E+m 11 cosAsin 3 EcosE+m 12 sinAsin 3 EcosE
ΔE＝n 0 +n 1 sinE+n 2 cosAcosE+n 3 sinAcosE+n 4 sin 2 E+n 5 cosAsinEcosE+n 6 sinAsisnEcosE+n 7 sin 3 E+n 8 cosAsin 2 EcosE+n 9 sinAsin 2 EcosE+n 10 sin4E+n 11 cosAsin 3 EcosE+n 12 sinAsin 3 EcosE
wherein m is 0 To m 12 Respectively corresponding azimuth axis model coefficients, n 0 To n 12 Respectively corresponding pitch axis model coefficients, wherein A is an actual azimuth value of a target source, E is an actual pitching value of the target source, delta A is azimuth axis deviation, and delta E is pitching axis deviation.
In the scheme, although the spherical harmonic function model can reflect the distribution rule of the star targets on the sphere, the spherical harmonic function is a pure mathematical model, the correlation between model coefficients under different collected samples is poor, the model is unstable, and the pointing model coefficients need to be recalibrated after the telescope is observed and operated for a period of time. Model coefficients calculated from three different sets of target numbers collected (table 1) can be more clearly reflected in a relatively large variation between coefficients.
TABLE 1
(2) The scheme of correcting by using the basic parameter model is as follows:
the basic parameter model is obtained by carrying out regression analysis on various shafting errors of the telescope and system errors of the telescope. Wherein each parameter has a definite physical meaning. The pointing model expression can be obtained by analyzing the shafting error and the system error of the telescope, and is as follows:
ΔAcosE＝d 1 +d 4 tanE+d 5 secE+d 6 cosAtanE+d 7 tanEsinA
ΔE＝d 2 +d 3 cosE+d 6 sinA+d 7 cosA
wherein d 1 Is the azimuth zero point difference, d 2 Is the height zero point difference, d 3 D is the gravity deformation of the lens barrel 4 Is that the azimuth axis is not orthogonal to the pitching axis, d 5 Is that the visual axis and the pitching axis do not intersect 6 Is the east-west inclination difference of azimuth axis, d 7 And (3) the azimuth axis north-south inclination difference is obtained, A is the actual azimuth value of the target source, and E is the actual pitching value of the target source.
In the scheme, although each coefficient term in the basic parameter model has clear physical meaning, the basic parameter model is fitted with a basic parameter model formula to find that under three groups of acquisition targets with different numbers, azimuth axis residual data in the model has obvious systematic error trend (shown in figure 1), which indicates that some errors of the basic parameter model are not covered and cannot completely reflect all errors.
Referring to fig. 2, the method for correcting the pointing model of the horizon telescope includes the following steps:
step S101: selecting uniformly distributed star targets from a preset star table to obtain target test objects;
step S102: recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data;
step S103: based on the preset matrix data, calculating corresponding coefficient item data;
step S104: the coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on the preset matrix data.
In the installation process of the telescope, the telescope is limited by the mechanical processing precision, the on-site adjustment, the system calibration and other horizontal limitations, and various errors can be introduced after the installation is completed. Various errors can bring serious influence to the observation of the telescope after accumulated and transferred. The inventor discovers that various interference factors influencing telescope pointing mainly comprise the following errors in two aspects: systematic errors and occasional errors (random errors).
Wherein the systematic error includes: the triaxial non-orthogonal error of the horizontal telescope, namely the misalignment deviation of the azimuth axis and the plumb line, the non-orthogonal deviation of the azimuth axis and the pitching axis, and the non-orthogonal deviation of the telescope visual axis and the pitching axis. The azimuth axis of the telescope is zero-point-difference with the axis encoder of the pitching axis. The telescope main optical axis (visual axis) is not coincident with the center of the CCD detector camera. And the telescope frame is deformed by gravity. Accidental errors include: temperature, humidity, wind load, etc. When the celestial coordinates are calculated, mongolian difference in the atmospheric model, station coordinates errors, errors introduced by software calculation, turbulence factors and the like are also considered. Thus, the key core for correcting the telescope is to determine the mapping relation between the central position of the observed celestial body in the visual axis (collimation axis) of the telescope and the actual position.
For this reason, in the above embodiment, on the basis of the basic parameter model, other unknown errors affecting telescope pointing are further analyzed to construct a new gantry pointing model, that is, the gantry pointing model is constructed based on the actual azimuth position of the target test object in the CCD field of view, the actual elevation position of the target test object in the CCD field of view, the azimuth position of the target test object in the center of the CCD field of view, the elevation position of the target test object in the center of the CCD field of view, azimuth axis deviation data, and elevation deviation data. The horizon telescope can then be corrected based on the gantry pointing model. Specifically, the method comprises the steps of obtaining uniformly distributed fixed star targets to record azimuth, pitching and deviation data of the fixed star targets in a CCD field of view, solving and calculating coefficient items in a frame pointing model through matrix calculation, and then bringing the coefficient item data into the frame pointing model to correct a telescope.
By introducing the specific preset matrix data, the system error of the azimuth axis can be eliminated, and the introduced preset matrix data can construct stable coefficient item data, so that the time for calibrating and pointing the telescope is greatly prolonged.
Based on the foregoing, in some embodiments of the present invention, the step of bringing the coefficient term data into the gantry pointing model to correct the telescope specifically includes: the coefficient item data are brought into a frame pointing model, and the conformity is verified; if the verification result is not in conformity, adding a target test object, and transferring to a step of recording preset matrix data of the target test object in the CCD field of view; otherwise, correcting the telescope based on the coefficient item data.
That is, after the coefficient term data is calculated, firstly verifying whether the precision meets the preset requirement, including verifying whether the azimuth axis precision is smaller than the preset corresponding threshold value and verifying whether the pitch axis precision is preset corresponding threshold value; and if the target test object is not met, further adding the target test object, carrying out corresponding calculation and solving on the preset matrix data again to obtain new coefficient item data, and carrying out verification again until the precision meets the preset requirement.
Thus, in one implementation of the present invention, the step of bringing the coefficient item data into a gantry pointing model and verifying compliance includes:
the coefficient item data are brought into a frame pointing model, and an accuracy value of an azimuth axis and an accuracy value of a pitching axis are obtained through calculation; and judging whether the coefficient item data meets the preset coincidence degree requirement or not based on the comparison relation between the precision value of the azimuth axis and the first threshold value and the comparison relation between the precision value of the elevation axis and the second threshold value. It should be noted that the predetermined compliance requirement may be set according to the actual situation. For example, if the accuracy value of the azimuth axis is smaller than the first threshold (or the accuracy value of the pitch axis is smaller than the second threshold), it may be determined that the compliance requirement is satisfied, and if the accuracy value of the azimuth axis is not smaller than the second threshold, the compliance requirement is not satisfied. And if the precision value of the azimuth axis is smaller than the first threshold value and the precision value of the elevation axis is smaller than the second threshold value, the satisfaction requirement is judged to be met, otherwise, the satisfaction requirement is not met.
Based on the foregoing, in some embodiments of the invention, the mathematical formula of the gantry pointing model includes:
ΔAcosE＝d 1 -d 3 cosAtanE-d 4 sinAtanE+d 5 secE-d 6 tanE+d 7 sinA+d 8 cosA+d 12 (A/2π)+d 14 sin2A+d 15 cos2A+d 20 sin2AsecE+d 21 cos2AsecE
ΔE＝d 2 +d 3 sinA-d 4 cosA+d 9 sinE+d 11 cotE+d 13 (E/2π)+d 16 sinA+d 17 cosA+d 18 EsinA+d 19 EcosA+d 22 sin2A+d 23 cos2A
wherein A is the actual azimuth position of the target test object in the CCD field of view, E is the actual pitching position of the target test object in the CCD field of view, d 1 Zero point of azimuth encoder, d 2 For pitch encoder zero, d 3 Is inclined to the north and south of the azimuth axis, d 4 Is inclined to azimuth axis east-west, d 5 D is the visual axis difference 6 Is non-orthogonal to the azimuth axis and the elevation axis, d 7 For the first azimuth axis ellipticity, d 8 Ellipticity of second azimuth axis, d 9 For a first pitch axis ellipticity, d 10 Ellipticity of second pitch axis, d 11 D is gravity bending of telescope lens cone 12 Line error for azimuth axis encoder, d 13 Score error for pitch axis encoder, d 14 Is a periodic term in a first azimuth, d 15 Is the periodic term in the second azimuth angle, d 16 For the first pitch axis encoder stiction, d 17 For the second pitch axis encoder stiction, d 18 For the first pitch axis static resistance, d 19 Is the second pitching axis static resistance, d 20 For the first azimuthal cycle ratio, d 21 Is a second azimuthal period ratio.
In the above embodiment, other unknown errors affecting the pointing direction of the telescope are further analyzed on the basis of the basic parameter model, and after regression analysis and calculation of various errors, corresponding coefficient items are added, so as to obtain the frame pointing model with 23 parameters.
Based on the foregoing, in some embodiments of the present invention, the step of recording the preset matrix data of the target test object in the field of view of the CCD specifically includes:
extracting the right ascension value and the right ascension value of a target test object so as to point to a corresponding target position by using a telescope; the target position is a position determined by the right ascension value and the right ascension value of the target test object;
and acquiring the position information of the target test object in the azimuth encoder and the pitch encoder and the off-center position information to obtain and record preset matrix data of the target test object in the CCD field of view.
Illustratively, the right and left warp values of the target test object may be extracted by the TheSky6 software, and then inputted on the computer integrated control software. Click tracking after input is completed, and the telescope points to the target position. The azimuth and elevation of the target test object displayed on the control software at this time are recorded. The encoder values recorded at this time are the actual positions of the target test object in the CCD market. After the recording is completed, the off-target quantity information of the target test object, which is far from the center of the CCD field of view, is recorded. Azimuth axis Δa, pitch axis Δe. After the four rows of data are collected, the azimuth angle value and the pitch angle value of the star target in the center of the CCD field of view can be obtained through the following formulas. Then by the formula: the true value = measured value-deviation, after calculating the true value, the corresponding data can be placed in a table to form the corresponding matrix data, and the fitting solution of coefficient item data is convenient to follow.
Based on the foregoing, in some embodiments of the present invention, the selecting the star targets in the predetermined star table, where the star targets are uniformly distributed, in the step of obtaining the target test object includes: in the direction of the azimuth axis 0-360 degrees, selecting a group of fixed star targets at intervals of 30 degrees, selecting azimuth positions along the azimuth axis, and selecting a group of fixed star targets at intervals of 20 degrees in the direction of the pitching axis 0-90 degrees. Therefore, the selected data can be ensured to be uniform, and the preset star table can be uniformly covered.
In order to better understand the present invention, a specific example of a method for correcting the pointing model of the horizon telescope will be explained below. It will be appreciated that this is merely an example and that a person skilled in the art may choose to adapt the method according to the actual situation.
Firstly, uniformly distributed star targets are selected through high-precision star table Thesky6 software at night of sunny, and for uniform coverage, a group of test targets are selected every 30 degrees in the direction of the azimuth axis 0-360 degrees, and 12 groups of targets are selected; and selecting azimuth positions along azimuth axes, selecting a group of test targets at intervals of 20 degrees in the direction of 0-90 degrees of pitch axes, starting pitch angles to be 20-70 degrees, and selecting 72 groups of targets for the first time, wherein 6 points are used for the total.
In the table above: object is the sidereal object name, RA is the target right ascension value, and DEC is the target right ascension value.
Then, the right warp RA and right weft DEC of 72 star targets are extracted by the Thesky6 software. And inputting the right ascension RA and the right ascension DEC of the star target into computer comprehensive control software. Click tracking after input is completed, and the telescope points to the target position. The azimuth and pitch of the sidereal target displayed on the control software are recorded. The encoder value recorded at this time is the actual position of the star target in the CCD field of view. After the recording is completed, the off-target information of the star target from the center of the CCD field of view is recorded. Azimuth axis Δa, pitch axis Δe. After the four rows of data are collected, the azimuth angle value and the pitch angle value of the star target in the center of the CCD field of view can be obtained through the following formulas.
True value = measurement value-deviation
After the true value is calculated by the above formula, six columns of data can be put into one table. Forming a matrix data. And the coefficient of the model (coefficient item data corresponding to the frame pointing model) is conveniently fitted and solved in matlab software.
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In the table above: a is the actual azimuth position of the observation target in the CCD field of view, and E is the actual pitching position of the observation target in the CCD field of view. A 'is the azimuth position of the observation target in the center of the CCD view field, and E' is the pitching position of the observation target in the center of the CCD view field. Δa is azimuth axis deviation data, and Δe is pitch axis deviation data.
And then, calculating the model coefficient by matrix operation in matlab software. The system of modified function equations corresponding to the gantry pointing model can be converted into the form of a system of polynary linear equations: a x=b, by matrix operations in matlab x=b/a (note here division left).
Finally, after calculating the frame pointing model coefficient (coefficient item data), writing into the configuration file. And on the basis, whether the deviation of the corrected pointing target of the telescope reaches the pointing requirement or not can be calculated, so that when the pointing requirement is not met, the acquisition number of the test targets is continuously increased, and the subsequent operation is repeated until the recalculated model coefficient meets the corresponding pointing requirement.
As shown in fig. 3-4, the residual distribution and the precision of the telescope under 160 sets (160 sets of acquisition targets are added on the original basis to improve the pointing effect of the telescope) of targets are shown. The corrected residual distribution shows that the telescope has no systematic error trend in the azimuth axis and the pitch axis under the target. The azimuth axis precision is 3.065 angular seconds, the pitch axis precision is.422 angular seconds, and all astronomical observation requirements are met.
Example 2
Referring to fig. 5, an embodiment of the present application provides a pointing model correction system for a horizon telescope, which includes:
an acquisition module 1 configured to: and selecting uniformly distributed star targets from a preset star table to obtain a target test object. A recording module 2 configured to: the method comprises the steps of recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data. A calculation module 3 configured to: and calculating corresponding coefficient item data based on the preset matrix data. A correction module 4 configured to: the coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on the preset matrix data.
The specific implementation process of the above system refers to the method for correcting the pointing model of the horizon telescope provided in embodiment 1, and is not described herein.
Example 3
Referring to fig. 6, an embodiment of the present application provides an electronic device comprising at least one processor 5, at least one memory 6 and a data bus 7; wherein: the processor 5 and the memory 6 complete the communication with each other through the data bus 7; the memory 6 stores program instructions executable by the processor 5, which the processor 5 invokes to perform a pointing model correction method for a horizon telescope. For example, implementation:
and selecting uniformly distributed star targets from a preset star table to obtain a target test object. Recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data. Based on the preset matrix data, corresponding coefficient item data are calculated. The coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on preset matrix data.
The Memory 6 may be, but is not limited to, a random access Memory (Random Access Memory, RAM), a Read Only Memory (ROM), a programmable Read Only Memory (Programmable Read-Only Memory, PROM), an erasable Read Only Memory (Erasable Programmable Read-Only Memory, EPROM), an electrically erasable Read Only Memory (Electric Erasable Programmable Read-Only Memory, EEPROM), etc.
The processor 5 may be an integrated circuit chip with signal processing capabilities. The processor 5 may be a general-purpose processor including a central processing unit (Central Processing Unit, CPU), a network processor (Network Processor, NP), etc.; but also digital signal processors (Digital Signal Processing, DSP), application specific integrated circuits (Application Specific Integrated Circuit, ASIC), field programmable gate arrays (Field-Programmable Gate Array, FPGA) or other programmable logic devices, discrete gate or transistor logic devices, discrete hardware components.
It will be appreciated that the configuration shown in fig. 6 is merely illustrative, and that the electronic device may also include more or fewer components than shown in fig. 6, or have a different configuration than shown in fig. 6. The components shown in fig. 6 may be implemented in hardware, software, or a combination thereof.
Example 4
The present invention provides a computer readable storage medium having stored thereon a computer program which, when executed by a processor 5, implements a method for correcting a pointing model of a horizon telescope.
For example, implementation:
and selecting uniformly distributed star targets from a preset star table to obtain a target test object. Recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data. Based on the preset matrix data, corresponding coefficient item data are calculated. The coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on preset matrix data.
The above functions, if implemented in the form of software functional modules and sold or used as a stand-alone product, may be stored in a computer readable storage medium. Based on such understanding, the technical solution of the present application may be embodied essentially or in a part contributing to the prior art or in a part of the technical solution, in the form of a software product stored in a storage medium, including several instructions for causing a computer device (which may be a personal computer, a server, or a network device, etc.) to perform all or part of the steps of the methods described in the embodiments of the present application. And the aforementioned storage medium includes: a U-disk, a removable hard disk, a Read-Only Memory (ROM), a random access Memory (RAM, random Access Memory), a magnetic disk, or an optical disk, or other various media capable of storing program codes.
It will be evident to those skilled in the art that the present application is not limited to the details of the foregoing illustrative embodiments, and that the present application may be embodied in other specific forms without departing from the spirit or essential characteristics thereof. The present embodiments are, therefore, to be considered in all respects as illustrative and not restrictive, the scope of the application being indicated by the appended claims rather than by the foregoing description, and all changes which come within the meaning and range of equivalency of the claims are therefore intended to be embraced therein. Any reference sign in a claim should not be construed as limiting the claim concerned.
Claims (9)
1. The pointing model correction method of the horizon telescope is characterized by comprising the following steps of:
selecting uniformly distributed star targets from a preset star table to obtain target test objects;
recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data;
based on the preset matrix data, calculating corresponding coefficient item data;
the coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on the preset matrix data.
2. The method for correcting the pointing model of the horizontal telescope as claimed in claim 1, wherein the step of bringing the coefficient term data into the frame pointing model to correct the telescope comprises:
the coefficient item data are brought into a frame pointing model, and the conformity is verified; if the verification result is not in conformity, adding a target test object, and transferring to a step of recording preset matrix data of the target test object in the CCD field of view; otherwise, correcting the telescope based on the coefficient item data.
3. The method for correcting the pointing model of the horizontal telescope according to claim 2, wherein the step of bringing the coefficient item data into the gantry pointing model and verifying the conformity comprises:
the coefficient item data are brought into a frame pointing model, and an accuracy value of an azimuth axis and an accuracy value of a pitching axis are obtained through calculation;
and judging whether the coefficient item data meets the preset coincidence degree requirement or not based on the comparison relation between the precision value of the azimuth axis and the first threshold value and the comparison relation between the precision value of the elevation axis and the second threshold value.
4. The method for correcting the pointing model of the horizontal telescope according to claim 1, wherein the mathematical formula of the gantry pointing model comprises:
ΔAcosE＝d 1 -d 3 cosAtanE-d 4 sinAtanE+d 5 secE-d 6 tanE+d 7 sinA+d 8 cosA+d 12 (
A/2π)+d 14 sin2A+d 15 cos2A+d 20 sin2AsecE+d 21 cos2AsecE
ΔE＝d 2 +d 3 sinA-d 4 cosA+d 9 sinE+d 11 cotE+d 13 (E/2π)+d 16 sinA+d 17 cosA+d 18 E
sinA+d 19 EcosA+d 22 sin2A+d 23 cos2A
wherein A is the actual azimuth position of the target test object in the CCD field of view, E is the actual pitching position of the target test object in the CCD field of view, d 1 Zero point of azimuth encoder, d 2 For pitch encoder zero, d 3 Is inclined to the north and south of the azimuth axis, d 4 Is inclined to azimuth axis east-west, d 5 D is the visual axis difference 6 Is non-orthogonal to the azimuth axis and the elevation axis, d 7 For the first azimuth axis ellipticity, d 8 Ellipticity of second azimuth axis, d 9 For a first pitch axis ellipticity, d 10 Ellipticity of second pitch axis, d 11 D is gravity bending of telescope lens cone 12 Line error for azimuth axis encoder, d 13 Score error for pitch axis encoder, d 14 Is a periodic term in a first azimuth, d 15 Is the periodic term in the second azimuth angle, d 16 For the first pitch axis encoder stiction, d 17 For the second pitch axis encoder stiction, d 18 For the first pitch axis static resistance, d 19 Is the second pitching axis static resistance, d 20 For the first azimuthal cycle ratio, d 21 Is a second azimuthal period ratio.
5. The method for correcting the pointing model of the horizon telescope according to claim 1, wherein the step of recording the preset matrix data of the target test object in the field of view of the CCD specifically comprises:
extracting the right ascension value and the right ascension value of a target test object so as to point to a corresponding target position by using a telescope; the target position is a position determined by the right ascension value and the right ascension value of the target test object;
and acquiring the position information of the target test object in the azimuth encoder and the pitch encoder and the off-center position information to obtain and record preset matrix data of the target test object in the CCD field of view.
6. The method for correcting the pointing model of the horizon telescope according to claim 1, wherein the selecting of the star targets with uniform distribution in the predetermined star table, the selecting of the star targets in the step of obtaining the target test object, comprises: in the direction of the azimuth axis 0-360 degrees, selecting a group of fixed star targets at intervals of 30 degrees, selecting azimuth positions along the azimuth axis, and selecting a group of fixed star targets at intervals of 20 degrees in the direction of the pitching axis 0-90 degrees.
7. A pointing model correction system for a horizon telescope, comprising:
an acquisition module configured to: selecting uniformly distributed star targets from a preset star table to obtain target test objects;
a recording module configured to: recording preset matrix data of a target test object in a CCD view field, wherein the preset matrix data comprise an actual azimuth position of the target test object in the CCD view field, an actual elevation position of the target test object in the CCD view field, an azimuth position of the target test object in the center of the CCD view field, an elevation position of the target test object in the center of the CCD view field, azimuth axis deviation data and elevation deviation data;
a computing module configured to: based on the preset matrix data, calculating corresponding coefficient item data;
a correction module configured to: the coefficient item data are brought into a frame pointing model to correct the telescope; the frame pointing model is a model which is built in advance based on the preset matrix data.
8. An electronic device comprising at least one processor, at least one memory, and a data bus; wherein: the processor and the memory complete communication with each other through the data bus; the memory stores program instructions for execution by the processor, the processor invoking the program instructions to perform the method of any of claims 1-6.
9. A computer readable storage medium, on which a computer program is stored, which computer program, when being executed by a processor, implements the method according to any of claims 1-6.
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| CN202311472597.5A CN117606511A (en) | 2023-11-06 | 2023-11-06 | Pointing model correction method, system, equipment and medium for horizon telescope |
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| CN202311472597.5A CN117606511A (en) | 2023-11-06 | 2023-11-06 | Pointing model correction method, system, equipment and medium for horizon telescope |
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