CN115829916B - Method and system for rapid target identification and pointing correction of high-dispersion optical fiber spectrometer - Google Patents
Method and system for rapid target identification and pointing correction of high-dispersion optical fiber spectrometer Download PDFInfo
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Abstract
The invention discloses a method and a system for rapid target identification and pointing correction of a high-dispersion optical fiber spectrometer, wherein the method comprises the following steps: the observation target rapidly confirms the imaging position of the locking target in the telescope pointing view field; the telescope orientation is quickly corrected to quickly align the observed target star to the fiber hole. The invention can avoid the situations of low efficiency of manual identification, false identification and low efficiency of manual pointing correction of the telescope, and improves the observation efficiency.
Description
Technical Field
The invention belongs to the technical field of astronomical observation, and particularly relates to a method and a system for rapid target identification and pointing correction of a high-dispersion optical fiber spectrometer.
Background
The high-dispersion optical fiber spectrometer is used for carrying out spectroscopic observation on a single star and is generally arranged on a large telescope with medium and large calibers in astronomy. The number of high-dispersion optical fiber spectrometers which are applied to astronomical observation at present in China is not large, and only 4 high-dispersion optical fiber spectrometers are arranged on a 2.4-meter telescope of Lijiang Gaomen, a 2.16-meter telescope of Xinglong, a 1.8-meter telescope of Lijiang Gaomen and a 1-meter telescope of Wisea school area of Shandong university respectively. With the further development of domestic astronomical observation research, candidates of a high-dispersion spectrum observation target extend to a darker target, and the cost of astronomical instruments and observation time is rapidly increased nowadays, so that the extremely improved telescope observation efficiency and instrument utilization rate are important for scientific observation.
Before high-dispersion spectrum observation is carried out, a target is needed to be found in a view field, the pointing direction of a telescope is corrected, and the current target identification process of the high-dispersion spectrum observation is as follows: 1) Telescope pointing, namely inputting the coordinates of the observed celestial object into a telescope control system, and pointing the telescope to the position of the sky according to the coordinates. 2) Target authentication: and (3) carrying out short exposure shooting on the position of the sky by using a camera of a CCD detector, and carrying out artificial verification by combining an observation target verification graph to find out the target. 3) Pointing correction: after the target is located in the CCD image, the target is manually moved into the fiber hole of the pinhole mirror by moving the telescope. The three steps are used for completing target identification and pointing correction before observation, and spectroscopic observation of celestial objects can be started. The process is easily affected by objective factors, such as telescope orientation, weather conditions, pinhole mirror reflection efficiency and the like, and the efficiency of target identification and orientation correction links is very low when a dark and weak target is observed, for example: the number of bright stars in the CCD field of view is very small, and the naked eyes can hardly find the target in the contrast standard identification graph, so that the difficulty of target identification is increased; even if a target is found, in the process of correcting the pointing direction of the telescope, the CCD needs long exposure (more than 20 seconds) to visually see the updated and moved position of the target, then the moving step length of the telescope is manually adjusted, and the telescope is gradually moved in the pointing direction through the button, so that the efficiency is extremely low.
Under the unbalanced condition that the demands of domestic astronomical observation research are growing and observation resources are scarce, how to furthest improve the observation efficiency and the equipment utilization rate and the scientific output is the basic starting point of the invention. A set of rapid star guiding and pointing correction method and system for the high-dispersion optical fiber spectrometer are designed, so that the problems of difficulty in identifying a dark target by people and low pointing efficiency of a single-step correction telescope are solved, the observation efficiency is improved, the equipment utilization rate is improved, and the scientific output is improved.
Therefore, there is a need for a method and system for rapid identification and pointing correction of an observation target.
Disclosure of Invention
In view of the above, the invention provides a method and a system for rapid target identification and pointing correction of a high-dispersion optical fiber spectrometer, aiming at the problems that the manual identification of an observation target by the high-dispersion optical fiber spectrometer is time-consuming, the identification efficiency is low, and even the situation of target identification error occurs, so that the waste of the observation time is caused.
In order to solve the technical problems, the invention discloses a method for rapidly identifying and correcting the target of a high-dispersion optical fiber spectrometer, which comprises the following steps:
step 1, rapidly identifying and locking an imaging position of an observation target in a pointing view field of a telescope;
and 2, quickly correcting the pointing direction of the telescope, and quickly aligning the observation target star with the optical fiber hole.
Optionally, the quickly identifying and locking the imaging position of the target in the telescope pointing field of view by the observation target in the step 1 specifically includes:
step 1.1, obtaining a target standard identification chart: automatically acquiring a target identification chart through a network open source star chart by manually giving input or inputting target coordinates and related parameters;
step 1.2, acquiring a current field imaging diagram of a star-guiding camera telescope: controlling the star-guiding camera to expose and image according to a software development kit (soft develop keil, SDK) provided by a camera manufacturer, and obtaining a current field imaging image of the telescope;
step 1.3, performing image matching on a target standard identification image and a current view field imaging image of the star-guiding camera telescope;
step 1.4, determining a target position: and matching the target identification image with the current field imaging image of the telescope by using an image matching algorithm, finding out the position of the target at the current pointing imaging image of the telescope, and marking out the position.
Optionally, in the step 1.4, the image matching algorithm is used to match the target identification map with the current field imaging map of the telescope, and the position of the target in the current pointing imaging map of the telescope is found and marked, which specifically includes:
step 1.4.1, confirming the size of a view field of a verification image, wherein the view field of the verification image is larger than the imaging view field of a star-guiding camera by 2 times, so that the image can be conveniently matched;
step 1.4.2, performing image matching on an image shot by a star guiding camera and a verification image, finally marking the position of a target star, and obtaining a pixel position (xobj, yobj) where the target is located; and finally, the accurate and quick identification process of the observation target is completed.
Optionally, the telescope orientation in the step 2 is quickly corrected, and the observation target star is quickly aligned to the optical fiber hole, specifically:
step 2.1, establishing a relation between a telescope motion coordinate system and a star guiding camera view field coordinate system;
step 2.2, determining the position of the optical fiber hole in the CCD imaging image, and calculating the imaging center coordinate of the optical fiber hole;
step 2.3, calculating the central coordinate (x o ，y o )；
Step 2.4, calculating the deviation between the central coordinate of the CCD imaging position of the observation target and the central coordinate of the optical fiber hole position;
step 2.5, judging whether the deviation is in an allowable range, if so, ending the pointing correction, and if so, carrying out the pointing deviation correction; where l=square ((dx) 2 +(dy) 2 ) I.e. square sum of x and y coordinate deviation, and then opening root number;
step 2.6, calculating the movement step length of the telescope in the movement axial direction according to the relation between the pointing deviation and the telescope movement and the star-guiding CCD imaging coordinates;
step 2.7, transmitting the step length into a telescope control system to carry out pointing correction according to the step length;
and 2.8, repeating the pointing deviation calculating step 2.4 until the pointing is corrected to be within the set range.
Optionally, the establishing a relationship between the telescope motion coordinate system and the view field coordinate system of the star guiding camera in the step 2.1 specifically includes: the telescope has two motion shafting, supposing X and Y, most of the time because of CCD adjustment precision problem, when the telescope moves along the axis, the satellite-guiding view field does not strictly follow the horizontal and vertical pixel direction to move;
the telescope moves along X direction for 1 angular second, and the horizontal and vertical pixels of CCD have motion components of X respectively 1 ，y 1 The method comprises the steps of carrying out a first treatment on the surface of the The method comprises the following steps: x=x 1 +y 1 Similarly, the Y axis is the same, y=x 2 +y 2 Wherein x is 1 ,y 1 ,x 2 ,y 2 Directly measuring, therefore, if the pixel deviation of the target in the CCD image is dx, dy, if the telescope needs to travel for A-angle seconds in the X direction and B-angle seconds in the Y direction, A is X 1 +B*x 2 ＝dx；A*y 1 +B*y 2 =dy; directly solving A and B;
then: a= (y) 2 dx-x 2 dy)/(x 1 y 2 -x 2 y 1 )；B＝(y 1 dx-x 1 dy)/(x 2 y 1 -x 1 y 2 )(1)。
Optionally, the determining the position of the fiber hole in the step 2.2 in the CCD imaging image, and calculating the center coordinates of the fiber hole imaging specifically includes: carrying out Gaussian filtering noise reduction treatment on the image, and carrying out self-adaptive binarization treatment on the image to obtain a binarized image with values of 0 and 1; the binarization is turned over (0 is changed to 1,1 is changed to 0), the position of the optical fiber hole is turned over to 1, the rest is changed to 0,60 x 100 pixels are taken near the imaging position of the optical fiber hole, wherein the x axis is 600 to 660 pixels, and the y axis is 600 to 700 pixels, namely [600:660,600:700]The method comprises the steps of carrying out a first treatment on the surface of the Directly obtaining the fiber Kong Zhixin coordinates (x f ,y f ) And a radius r; the fiber hole location is accomplished by marking the fiber hole location with the circle of OpenCV.
Optionally, the deviation formula in step 2.4 is: (dx, dy) = (x) o -x f ,y o -y f )。
Optionally, the moving step length of the telescope in the moving axial direction in the step 2.6 is as follows: a= (y) 2 dx-x 2 dy)/(x 1 y 2 -x 2 y 1 )；B＝(y 1 dx-x 1 dy)/(x 2 y 1 -x 1 y 2 ) The method comprises the steps of carrying out a first treatment on the surface of the A. B is the movement step length of the telescope in two movement directions.
The invention also discloses a system for rapidly identifying and correcting the target and directing of the high-dispersion optical fiber spectrometer, which comprises an image acquisition module, a control module and a telescope module; the image acquisition module and the telescope module are connected with the control module through an Ethernet or USB communication interface; the control module is installed in a computer.
Compared with the prior art, the invention can obtain the following technical effects:
1) And inputting a verification graph, quickly performing target verification, marking a target star, and providing a user for re-checking. 2) The position coordinates of the fiber holes in the slit monitor can be obtained. 3) The center coordinates of the target star can be obtained. 4) The position offset of the target star from the fiber hole position can be obtained. 5) The correspondence between the telescope axis motion coordinates and the slit monitor image pixel coordinates can be obtained. 6) The telescope can be quickly pointed for correction.
Of course, it is not necessary for any of the products embodying the invention to achieve all of the technical effects described above at the same time.
Drawings
The accompanying drawings, which are included to provide a further understanding of the invention and are incorporated in and constitute a part of this specification, illustrate embodiments of the invention and together with the description serve to explain the invention and do not constitute a limitation on the invention. In the drawings:
FIG. 1 is a flow chart of the present invention for the observation target to quickly identify the imaging position of the locked target in the telescope pointing field of view;
FIG. 2 is a flow chart of the invention for quick correction of telescope orientation, quick alignment of an observation target star to an optical fiber hole;
FIG. 3 is a schematic diagram of a system for rapid target verification and pointing correction of a high dispersion fiber optic spectrometer of the present invention.
Detailed Description
The following will describe embodiments of the present invention in detail by referring to examples, so that the implementation process of how to apply the technical means to solve the technical problems and achieve the technical effects of the present invention can be fully understood and implemented.
The invention discloses a method for rapidly identifying and correcting the target of a high-dispersion optical fiber spectrometer, which comprises the following steps:
step 1, rapidly identifying an imaging position of a locking target in a telescope pointing view field by an observation target:
step 1.1, obtaining a target standard identification chart: obtaining a target certification graph through artificially given input or inputting target coordinates and related parameters through a network open-source star table (the star table is an internationally disclosed star table, such as the downloading of Alatin and simpad to a local computer);
step 1.2, acquiring a current field imaging diagram of a star-guiding camera telescope: controlling the star-guiding camera to expose and image according to a software development kit (soft develop keil, SDK) provided by a camera manufacturer, and obtaining a current field imaging image of the telescope;
step 1.3, performing image matching on a target standard identification image and a current view field imaging image of the star-guiding camera telescope;
step 1.4, determining a target position: matching the target identification image with the current field imaging image of the telescope by using an image matching algorithm, finding out the position of the target in the current pointing imaging image of the telescope, and marking out the position;
step 1.4.1, confirming the size of the view field of the evidence-obtaining and confirming view field, wherein the view field of the evidence-obtaining and confirming view field is larger than the imaging view field of the star-guiding camera by about 2 times, so that the image matching is facilitated, for example: the star guiding view field is 5 degrees, the verification view field is larger than 10 degrees, and the purpose is to prevent the telescope from excessively deviating, and if the star guiding view field is smaller, the star guiding view field cannot be matched if the star guiding view field is not in the verification view area.
Step 1.4.2, performing image matching on an image shot by a star guiding camera and a verification image, marking the position of a target star, and obtaining a pixel position (xobj, yobj) where the target is located; and finally, the accurate and quick identification process of the observation target is completed.
And 2, quickly correcting the pointing direction of the telescope, and quickly aligning the observation target star to the optical fiber hole, wherein the specific process is shown in fig. 2.
Step 2.1, establishing a relation between a telescope motion coordinate system and a star guiding camera view field coordinate system:
the telescope has two motion axes, assuming X and Y, most often due to CCD alignment accuracy problems, and the satellite field of view does not follow exactly the horizontal and vertical pixel directions as the telescope moves along the axis.
Thus, the telescope is moved in the X direction for 1 angular second, with a motion component X at each of the CCD horizontal and vertical pixels 1 ，y 1 . We can obtain: x=x 1 +y 1 Similarly, the Y axis is the same, y=x 2 +y 2 Wherein x is 1 ,y 1 ,x 2 ,y 2 Can be directly measured, so if the pixel deviation of the target in the CCD image is dx, dy, if the telescope needs to walk A-angle seconds in the X direction and B-angle seconds in the Y direction, A is X 1 +B*x 2 ＝dx；A*y 1 +B*y 2 =dy. A and B can be directly obtained;
then: a= (y) 2 dx-x 2 dy)/(x 1 y 2 -x 2 y 1 )；B＝(y 1 dx-x 1 dy)/(x 2 y 1 -x 1 y 2 )
And 2.2, determining the position of the optical fiber hole in the CCD imaging image, and calculating the center coordinate of the optical fiber hole image.
And carrying out Gaussian filtering noise reduction processing on the image. And performing self-adaptive binarization processing on the image to obtain a binarized image with values of 0 and 1. The binarization was flipped (0 to 1,1 to 0), the fiber hole position was flipped to 1, and the rest was 0. Taking a 60 x 100 pixel range around the fiber optic aperture imaging location, where the x-axis is 600 to 660 pixels and the y-axis is 600 to 700 pixels, i.e., [600:660,600:700 ]]. The coordinates (x) of the fiber Kong Zhixin can be obtained directly from the movements of OpenCV f ,y f ) And a radius r. Fiber hole locations can be marked using the circle of OpenCV, which completes fiber hole positioning.
Step 2.3, calculating the central coordinate (x o ，y o ) The method comprises the steps of carrying out a first treatment on the surface of the In step 1.4.2, it is mentioned that the position of the target star can be located and marked by the image matching algorithm, so that the center coordinate of the target can be obtained.
Step 2.4, calculating the deviation between the CCD imaging position coordinates and the optical fiber hole position coordinates of the observation target, wherein a deviation formula is as follows: (dx, dy) = (x) o -x f ,y o -y f )；
Step 2.5, judging whether the deviation is in an allowable range, for example: l=square ((dx) 2 +(dy) 2 ) The distance (sum of squares of x and y coordinate deviations, and root number of the deviation) is smaller than 0.2 optical fiber hole radius, if yes, the pointing correction is finished, and if the deviation is larger than the set range, the pointing deviation correction is carried out.
And 2.6, calculating the movement step length of the telescope in the movement axial direction according to the relation between the pointing deviation and the telescope movement and the star-guiding CCD imaging coordinates.
A＝(y 2 dx-x 2 dy)/(x 1 y 2 -x 2 y 1 )；B＝(y 1 dx-x 1 dy)/(x 2 y 1 -x 1 y 2 ) A, B is the step size of the telescope in both directions of motion.
And 2.7, transmitting the step length into a telescope control system to carry out pointing correction according to the step length.
And 2.8, repeating the pointing deviation calculating step 2.4 until the pointing is corrected to be within the set range.
The invention discloses a system for rapid target identification and pointing correction of a high-dispersion optical fiber spectrometer, which is shown in fig. 3 and comprises an image acquisition module 1, a control module 2 and a telescope module 3; the image acquisition module 1 and the telescope module 3 are connected with the control module 2 through Ethernet or USB communication interfaces; the control module 2 is installed in a computer.
Before spectrum observation, the actual star-guiding CCD imaging and verification images have larger difference due to the factors of telescope pointing deviation, star-guiding CCD performance, view field rotation, mirror image and the like, and the invention can rapidly and automatically position and observe the target star through 3 modules of the telescope, and the image acquisition module 1 reads images from the star-guiding CCD; calculating the offset of the target star from the imaging position of the optical fiber hole, converting the offset of the CCD pixel coordinate into the offset of the telescope motion coordinate system, transmitting the offset to the control module 2 through network communication, and driving the telescope to carry out pointing correction by the control module 2 according to the offset. Finally, the accurate verification target is achieved, the effect of quick telescope pointing correction is achieved, the situations of low human verification efficiency, false verification and low telescope pointing correction efficiency are avoided, and the observation efficiency is improved.
While the foregoing description illustrates and describes several preferred embodiments of the invention, it is to be understood that the invention is not limited to the forms disclosed herein, but is not to be construed as limited to other embodiments, and is capable of use in various other combinations, modifications and environments and is capable of changes or modifications within the spirit of the invention described herein, either as a result of the foregoing teachings or as a result of the knowledge or skill of the relevant art. And that modifications and variations which do not depart from the spirit and scope of the invention are intended to be within the scope of the appended claims.
Claims (7)
1. The method for rapidly identifying and correcting the target and the direction of the high-dispersion optical fiber spectrometer is characterized by comprising the following steps:
step 1, rapidly identifying and locking an imaging position of an observation target in a pointing view field of a telescope;
step 2, quickly correcting the pointing direction of the telescope, and quickly aligning the observation target star with the optical fiber hole;
the observation target in the step 1 rapidly identifies and locks the imaging position of the target in the telescope pointing view field, specifically:
step 1.1, obtaining a target standard identification chart: automatically acquiring a target identification chart through a network open source star chart by manually giving input or inputting target coordinates and related parameters;
step 1.2, acquiring a current field imaging diagram of a star-guiding camera telescope: controlling exposure imaging of the star-guiding camera according to a Software Development Kit (SDK) provided by a camera manufacturer to obtain a current field imaging image of the telescope;
step 1.3, performing image matching on a target standard identification image and a current view field imaging image of the star-guiding camera telescope;
step 1.4, determining a target position: and matching the target identification image with the current field imaging image of the telescope by using an image matching algorithm, finding out the position of the target at the current pointing imaging image of the telescope, and marking out the position.
2. The method according to claim 1, wherein the matching of the target identification map and the current field imaging map of the telescope by using the image matching algorithm in step 1.4 finds out the position of the target in the current pointing imaging map of the telescope, and marks out, specifically:
step 1.4.1, confirming the size of a view field of a verification image, wherein the view field of the verification image is larger than the imaging view field of a star-guiding camera by 2 times, so that the image can be conveniently matched;
step 1.4.2, performing image matching on an image shot by a star guiding camera and a verification image, finally marking the position of a target star, and obtaining a pixel position (xobj, yobj) where the target is located; and finally, the accurate and quick identification process of the observation target is completed.
3. The method according to claim 1, wherein the telescope pointing direction in step 2 is quickly corrected, and the observation target star is quickly aligned to the optical fiber hole, specifically:
step 2.1, establishing a relation between a telescope motion coordinate system and a star guiding camera view field coordinate system;
step 2.2, determining the position of the optical fiber hole in the CCD imaging image, and calculating the central coordinate of the optical fiber hole imaging;
step 2.3, calculating the central coordinate (x o ，y o )；
Step 2.4, calculating the deviation between the central coordinate of the CCD imaging position of the observation target and the central coordinate of the optical fiber hole position;
step 2.5, judging whether the deviation is in an allowable range, if so, ending the pointing correction, and if the deviation is large, the distance L is smaller than 0.2 optical fiber hole radiusIn the set range, correcting the pointing deviation; where l=square ((dx) 2 +(dy) 2 ) I.e. square sum of x and y coordinate deviation, and then opening root number;
step 2.6, calculating the movement step length of the telescope in the movement axial direction according to the relation between the pointing deviation and the telescope movement and the star-guiding CCD imaging coordinates;
step 2.7, transmitting the step length into a telescope control system to carry out pointing correction according to the step length;
and 2.8, repeating the pointing deviation calculating step 2.4 until the pointing is corrected to be within the set range.
4. A method according to claim 3, wherein the relationship between the telescope motion coordinate system and the satellite guide camera field of view coordinate system is established in step 2.1, specifically: the telescope has two motion shafting, supposing X and Y, most of the time because of CCD adjustment precision problem, when the telescope moves along the axis, the satellite-guiding view field does not strictly follow the horizontal and vertical pixel direction to move;
the telescope moves along X direction for 1 angular second, and the horizontal and vertical pixels of CCD have motion components of X respectively 1 ，y 1 The method comprises the steps of carrying out a first treatment on the surface of the The method comprises the following steps: x=x 1 +y 1 Similarly, the Y axis is the same, y=x 2 +y 2 Wherein x is 1 ,y 1 ,x 2 ,y 2 Directly measuring, therefore, if the pixel deviation of the target in the CCD image is dx, dy, if the telescope needs to travel for A-angle seconds in the X direction and B-angle seconds in the Y direction, A is X 1 +B*x 2 ＝dx；A*y 1 +B*y 2 =dy; directly solving A and B;
then: a= (y) 2 dx-x 2 dy)/(x 1 y 2 -x 2 y 1 )；B＝(y 1 dx-x 1 dy)/(x 2 y 1 -x 1 y 2 )(1)。
5. A method according to claim 3, wherein the position of the fiber hole in the CCD image is determined in step 2.2 and calculatedThe center coordinates of the optical fiber hole imaging are specifically as follows: carrying out Gaussian filtering noise reduction treatment on the image, and carrying out self-adaptive binarization treatment on the image to obtain a binarized image with values of 0 and 1; the binarization is turned over, specifically, 0 is changed to 1,1 is changed to 0, the position of the optical fiber hole is turned over to 1, the rest is changed to 0,60 x 100 pixels are taken near the imaging position of the optical fiber hole, wherein the x axis is 600 to 660 pixels, and the y axis is 600 to 700 pixels, namely [600:660,600:700]The method comprises the steps of carrying out a first treatment on the surface of the Directly obtaining the fiber Kong Zhixin coordinates (x f ,y f ) And a radius r; the fiber hole location is accomplished by marking the fiber hole location with the circle of OpenCV.
6. A method according to claim 3, wherein the deviation formula in step 2.4 is: (dx, dy) = (x) o -x f ,y o -y f )。
7. A method according to claim 3, wherein the moving step length of the telescope in the moving axial direction in step 2.6 is:
A＝(y 2 dx-x 2 dy)/(x 1 y 2 -x 2 y 1 )；B＝(y 1 dx-x 1 dy)/(x 2 y 1 -x 1 y 2 ) The method comprises the steps of carrying out a first treatment on the surface of the A. B is the movement step length of the telescope in two movement directions.
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