CN111538149A - A telescope control device, system, method, storage medium, program and application - Google Patents

Abstract

The invention belongs to the technical field of observation of astronomical transient sources, and discloses a telescope control device, system, method, storage medium, program and application. Eight sets of optical telescope systems are uniformly fixed on a multifunctional turntable to realize 360° rotation. Achieve uninterrupted scanning of the entire sky area. 4 sets of telescope systems realize low-elevation and broadband scanning and searching for transient source celestial objects. For high-elevation and zenith scanning and searching for transient sources, 4 sets (2 sets of each) optical telescopes placed on base 2 It is completed by means of pitch scanning; by optimizing the control and image processing software, and using the layout of the telescope device, the real-time monitoring and searching of the transient source celestial bodies in the whole sky can be carried out. Compared with the previous 20 independent systems, the centralized control method adopted by the present invention is convenient for centralized control of the system, and the response processing speed is also faster.

Description

A telescope control device, system, method, storage medium, program and application

technical field

The invention belongs to the technical field of observation of astronomical transient sources, and in particular relates to a telescope control device, system, method, storage medium, program and application.

Background technique

In recent years, the observation and research of astronomical transient sources have played an increasingly important role in the research of modern time-domain astronomy. A transient source refers to an occasional, short-lived, non-periodic astronomical phenomenon. Observationally, its duration time scale ranges from seconds to weeks or even months. At present, the known transient sources mainly include astronomical events such as supernovae, gamma-ray bursts, microlensing, black holes disintegrating stars, and the electromagnetic counterparts of gravitational waves. Gamma-ray burst (GRB), referred to as gamma-ray burst, is a typical transient source object. It is a sudden intensification of short-scale gamma rays from the depths of the universe, and it is also the most violent explosion since the Big Bang. According to the duration of the time scale T90 (the time when the photon count is from 5% to 95%), it can be divided into two types: long bursts (T90>2s) and short bursts (T90<2s). It is generally believed that long bursts originate from the collapse of massive stars, while short bursts originate from the merger of double compact stars. In addition, in addition to the instantaneous gamma-ray burst radiation, there are afterglow phenomena in the X-ray band, optical band, and radio band after the eruption. Therefore, by studying gamma-ray bursts and their post-burst afterglow phenomena, we can further explore the production process of compact celestial bodies, gravitational wave radiation, relativistic shock waves, and extremely high-energy cosmic rays, as well as high-precision testing of basic physical principles. Since gamma-ray bursts are difficult to predict in time and space, in order to capture signals in time, optical telescopes with large fields of view are required for high-frequency all-sky monitoring. With the development of modern astronomical observation technology and data processing technology, more and more transient source celestial bodies have been detected, which also makes the sky survey observation and research of transient source become the focus of the astronomical circle.

At present, the ground-based wide-angle camera array (GWAC) of the wide-field transient source survey equipment at the Xinglong Base of the National Astronomical Observatory of my country is constructed for the survey observation and research of transient source celestial bodies. GWAC is mainly used to observe the radiation in the optical band within 5 minutes before and 15 minutes after the eruption of GRB. The system consists of 40 wide-angle telescopes with a diameter of 18 cm. The field of view of each telescope can reach 150 square degrees. They are all equipped with scientific-grade CCD cameras with a large target area (4k*4k), and the total field of view can reach 5000 square meters. Spend. It can be seen that 2 telescopes are installed on each rack, and 40 telescopes require a total of 20 racks. Compared with the overall system, although this structure improves the flexibility of the system, it increases the difficulty of the control system. At the same time, the system cost is greatly increased. Therefore, it is particularly important to devise a new construction method for telescope groups.

In order to conduct sky survey observation and research of transient source celestial bodies, Chinese researchers have proposed to use wide-angle camera arrays to carry out related research. One of the related technologies, "The mini-GWAC optical follow-up of gravitationalwave alerts-results from the O2campaign and prospects for the upcoming O3run", Res.Astron.Astrophys, 20(1),13(2020). my country National Astronomical Observatory Xinglong Base A ground-based wide-angle camera array (GWAC) of the wide-field transient source sky survey equipment is proposed to be used for related work research. GWAC is mainly used to observe the radiation in the optical band 5 minutes before and 15 minutes after the eruption of GRB. The system consists of 40 wide-angle telescopes with a diameter of 18 cm. The field of view of each telescope can reach 150 square degrees. They are all equipped with scientific-grade CCD cameras with a large target area (4k*4k), and the total field of view can reach 5000 square. Spend. At present, relevant research data have been obtained using this system.

The first implementation scheme of the prior art: The Ground Wide Angle Camera (GWAC) consists of 40 wide-angle telescopes with a diameter of 18 cm. The field of view of each telescope can reach 150 square degrees, and each is equipped with a large target surface. (4k*4k) scientific-grade CCD camera, the total field of view can reach 5000 square degrees. The observation plan is distributed through the main control system, and each observation subsystem (single telescope) is activated to observe different sky areas and obtain original images. After data processing of the collected images, the obtained images are identified according to the dynamic threshold variation range. If the dynamic threshold variation range does not exceed the set value, it is considered that no new target is found, and the image is collected again; if the dynamic threshold exceeds the set value, it is regarded as a candidate target, and multi-frame acquisition of the target will be obtained. The images are sent to the science center for further identification and judgment, and the matching target images are stored in the database to facilitate the development of subsequent scientific research.

Disadvantage of the prior art 1 In order to realize a telescope array system with a large field of view and an all-sky area, the system selects a structure in which every two telescopes are placed on one rack, and the whole system has a total of 20 rack devices. Although the flexibility of a single device has increased, it still has the following shortcomings: the overall control of the control system is more difficult, the performance requirements of the main control device are higher, and the system response time is longer; the system cost is higher;

Through the above analysis, the existing problems and defects in the prior art are: the current telescope has high difficulty in controlling the system, the system response time is long, and the cost of the system is high.

The difficulty of solving the above problems and defects is: the above-mentioned GWAC system is mainly composed of 20 sets of sub-systems, the system composition is relatively cumbersome, the 20 sets of sub-systems need to respond separately, and the system response time is long; Easy system centralized control. How to improve the system response speed and achieve centralized control is difficult.

The overall cost of the system is relatively high, and the cost is at least 1-2 times higher than that of the technical solution.

The significance of solving the above problems and defects is: for the transient source celestial body, it has extremely high requirements on the response speed of the system. The structure is more compact (the floor space is less than 20m ² ), the automatic search function of the system can be turned on with only one command signal, and there is no need for separate operation of each sub-system, which reduces the response time of the system and simplifies the structure of the system. The cost of the system is greatly reduced.

SUMMARY OF THE INVENTION

In view of the problems existing in the prior art, the present invention provides a telescope control device, system, method, storage medium, program and application.

The present invention is realized in this way, a telescope control method, the telescope control method includes:

In the first step, 8 sets of optical telescope systems are uniformly fixed on the multi-function turntable to achieve 360° rotation and uninterrupted scanning of the entire sky area.

In the second step, 4 sets of telescope systems can scan and search for transient source celestial bodies with low elevation angle and wide band. (station) optical telescope is completed by means of pitch scanning;

In the third step, by optimizing the control and image processing software, and using the layout of the telescope device, the real-time monitoring and searching of the transient source celestial bodies in the whole sky area is realized.

Image processing process:

There are two observation modes: if the lens remains stationary, for the position information of a transient source, the difference map of two consecutive frames of pictures will change significantly at this position, denoted as a, while the second and third frames will change significantly. The difference value map of the picture will not have a difference value -a that offsets this change at this position; however, due to the random appearance of noise, if there is a significant difference value b in two consecutive frames of pictures, the difference between the second and third frames of pictures A value near -b appears, indicating that the third frame and the first frame have the same value at this position, then the change represented in the second frame is likely to be a noise rather than a transient source. Using this property, it is possible to determine whether it is a noise or a transient source object by observing several frames consecutively after a significant difference. If the lens moves to track a moving target, before making a difference between the two frames, the translation length of the second frame along the horizontal and vertical directions needs to be considered, and the images need to be realigned first, and then the difference is processed. For the pixels that exist in the second frame of pictures but do not exist in the first frame, they need to wait for processing together with the next frame of pictures. At this time, the images observed by the first set of telescopes are saved, and the images obtained by the second set of telescopes are compared with the images obtained by the first set. Through this optimization method, the operation of repeated observation of a single set of telescopes is omitted, the observation time is shortened, and the speed of target recognition is improved.

In addition, the observation strategy of the telescope plays a very important role in the detection of the target. The vertical "M-type" scanning and the horizontal "Z-type" scanning will be used to conduct wide-area monitoring of the entire sky area. The scanning path diagram is shown. By studying the rotation parameters of the telescope's turntable, the pitch parameters, and the exposure time of the camera, the telescope control parameters and camera parameters that are suitable for the whole-sky monitoring of the gamma-ray burst transient source objects are obtained. detection probability. Figure 8 is a schematic diagram of observation using the "M" type and "Z" type observation strategies, respectively. The classic transient source search process is shown in Figure 9.

Further, the telescope control method realizes telescope optical systems with different monitoring fields of view by changing the size, material and structure of the optical lens of the telescope; and changing the number of telescopes realizes the adjustment of the monitoring sky area of a single set of telescopes.

Further, the field of view of the two optical telescopes in the telescope control method is 14°*14°.

Another object of the present invention is to provide a computer device, the computer device includes a memory and a processor, the memory stores a computer program, and when the computer program is executed by the processor, the processor executes the following step:

In the first step, 8 sets of optical telescope systems are uniformly fixed on the multi-function turntable to achieve 360° rotation and uninterrupted scanning of the entire sky area.

In the second step, 4 sets of telescope systems realize the work of scanning and searching for transient source celestial bodies with low elevation angle and wide band. For the scanning and searching for transient sources at high elevation angle and zenith, the two optical telescopes placed on the base will scan through pitching. done in a way;

In the third step, by optimizing the control and image processing software, and using the layout of the telescope device, the real-time monitoring and searching of the transient source celestial bodies in the whole sky area is realized.

Another object of the present invention is to provide a computer-readable storage medium, which stores a computer program, and when the computer program is executed by a processor, causes the processor to perform the following steps:

In the first step, 8 sets of optical telescope systems are uniformly fixed on the multi-function turntable to achieve 360° rotation and uninterrupted scanning of the entire sky area.

In the second step, 4 sets of telescope systems realize the work of scanning and searching for transient source celestial bodies with low elevation angle and wide band. For the scanning and searching for transient sources at high elevation angle and zenith, the two optical telescopes placed on the base will scan through pitching. done in a way;

In the third step, by optimizing the control and image processing software, and using the layout of the telescope device, the real-time monitoring and searching of the transient source celestial bodies in the whole sky area is realized.

Another object of the present invention is to provide a telescope control system for operating the telescope control method, the telescope control system comprising:

Telescope system module, used to realize surveillance and search in different surveillance fields of view;

The control system module is used to realize the search speed of the surveillance target by adjusting the rotation speed and rotation direction/azimuth of the telescope;

The image data processing module is used to realize target recognition by optimizing the algorithm of the image processing software.

Another object of the present invention is to provide a telescope control device equipped with the telescope control system, and the telescope control device is provided with:

pedestal;

A multifunctional turntable is rotatably fixed on the base, a first equatorial mount bracket and a second equatorial mount bracket are rotatably fixed on the multifunctional turntable, and the second equatorial mount bracket is arranged inside the first equatorial mount bracket, so the The first equatorial mount bracket and the second equatorial mount bracket are provided with four, and they are evenly arranged at 90 degrees;

The height of the second equatorial mount bracket is higher than that of the first equatorial mount bracket, and both the first equatorial mount bracket and the second equatorial mount bracket are provided with telescopes.

Further, the number of telescopes on the first equatorial mount bracket or the second equatorial mount bracket is 1-4.

Further, the telescope is provided with a lens barrel, and an optical lens is clamped at the inner front end of the lens barrel;

The diameter of the telescope is 15cm, the matrix of the optical lens is K9 glass, quartz glass or fluoride glass, and the number of optical lenses is 1-10 pieces; the optical field of view of the telescope is 14°*14°.

Another object of the present invention is to provide an observation terminal for an astronomical transient source, where the telescope control device is installed on the observation terminal for an astronomical transient source.

Combined with all the above-mentioned technical solutions, the advantages and positive effects possessed by the present invention are:

FIG. 10 is an actual photograph of the transient source search carried out by using the technical solution.

Table 1 Technical comparison between this scheme and the GWAC project

project This technical solution GWAC surveillance sky area 6600 square degrees 5000 square degrees Number of lens barrels 16 40 Number of racks 8 20 cost valuation <10 million >40 million floor space &lt;20m² &gt;100m²

The initial test system of this technical solution is used to take pictures of real objects in the all-sky survey of transient sources. The entire response and shooting process takes about 20s, which greatly improves the response speed of the system and facilitates the search and detection of transient source celestial objects. Table 1 shows the technical comparison between the technical solution and the GWAC project. The technical solution reduces the cost and also reduces the system space under the condition of the same performance.

The invention can realize a transient source monitoring system with a larger monitoring sky area while reducing the system complexity and cost. The invention has high practical value to meet the needs of fast search for transient source celestial bodies. Through the telescope layout of the above scheme, the overall system layout is more compact, which is convenient for the realization of overall control; at the same time, the speed of target search and scanning in the whole sky area can also be improved; more importantly, through the modification of the scheme, the number of telescopes is reduced, and the To 1/2 to 1/3 of the original number of equipment.

In the case of the same monitoring sky area, the present invention reduces the cost. The number of telescopes required by the system of the present invention is 16, which greatly reduces the system cost compared with the 40 telescopes of the previous GWAC system. The system integration is higher and the processing speed is faster. Compared with the previous 20 independent systems, the centralized control method adopted by the present invention is convenient for the centralized control of the system, and the response processing speed is also faster.

Description of drawings

In order to explain the technical solutions of the embodiments of the present application more clearly, the following will briefly introduce the drawings that need to be used in the embodiments of the present application. Obviously, the drawings described below are only some embodiments of the present application. For those of ordinary skill in the art, other drawings can also be obtained from these drawings without creative effort.

FIG. 1 is a flowchart of a method for controlling a telescope according to an embodiment of the present invention.

FIG. 2 is a schematic structural diagram of a telescope control system provided by an embodiment of the present invention.

3 is a schematic structural diagram of a telescope device for rapid identification of transient celestial bodies provided by an embodiment of the present invention;

4 is a schematic structural diagram of another side of a telescope device for fast identification of transient celestial objects provided by an embodiment of the present invention;

5 is a schematic structural diagram of Embodiment 3 provided by an embodiment of the present invention;

In the figure: 1. Multifunctional turntable; 2. The first equatorial mount; 3. The second equatorial mount; 4. The lens barrel; 5. The base; 6. The optical lens.

FIG. 6 is a schematic diagram of a method for constructing a telescope system for rapid identification of transient celestial objects provided by an embodiment of the present invention.

FIG. 7 is a schematic diagram of a scanning sky area range provided by an embodiment of the present invention.

FIG. 8 is a schematic diagram of an observation using an “M” type and a “Z” type observation strategy provided by an embodiment of the present invention.

FIG. 9 is a diagram illustrating an example of processing of a transient source search image subtraction method provided by an embodiment of the present invention.

FIG. 10 is an actual photograph of using the present invention to search for a transient source provided by an embodiment of the present invention.

Detailed ways

In order to make the objectives, technical solutions and advantages of the present invention clearer, the present invention will be further described in detail below with reference to the embodiments. It should be understood that the specific embodiments described herein are only used to explain the present invention, but not to limit the present invention.

In view of the problems existing in the prior art, the present invention provides a telescope control device, system, method, storage medium, program and application. The present invention is described in detail below with reference to the accompanying drawings.

As shown in Figure 1, the telescope control method provided by the present invention comprises the following steps:

S101: 8 sets of optical telescope systems are uniformly fixed on the multi-function turntable to achieve 360° rotation and uninterrupted scanning of the entire sky area.

S102: 4 sets of telescope systems can realize the work of scanning and searching for transient source celestial bodies with low elevation angle and broadband. For the work of scanning and searching for transient sources at high elevation angle and zenith, two optical telescopes are placed on the base marked 2. Completed by tilting scan;

S103: By optimizing the control and image processing software and using the layout of the telescope device, it is possible to carry out real-time monitoring and searching for transient source celestial bodies in the entire sky area.

As shown in Figure 2, the telescope control system provided by the present invention includes:

The telescope system module is used to realize surveillance and search in different surveillance fields of view.

The control system module is used to realize the search speed of the surveillance target by adjusting the rotation speed and rotation direction/azimuth of the telescope.

The image data processing module is used to realize target recognition by optimizing the algorithm of the image processing software.

The technical solutions of the present invention will be further described below with reference to the accompanying drawings.

1. Transient source: refers to an occasional, short-lived non-periodic astronomical phenomenon. Its duration time scale ranges from seconds to weeks or even months. At present, the known transient sources mainly include astronomical events such as supernovae, gamma-ray bursts, microlensing, black holes disintegrating stars, and the electromagnetic counterparts of gravitational waves.

2. Gamma-ray burst (GRB), referred to as gamma-ray burst, is a typical transient source celestial body. It is a sudden intensification of short-scale gamma rays from the depths of the universe, and it is also the most violent explosion since the Big Bang. The transient source mentioned in the present invention will be described by taking a gamma burst as an example.

3. Sky area: In the field of astronomy, for the convenience of identification, according to the orientation of the stars, it is divided into stellar sky areas, referred to as sky areas or star areas.

4. Field of View: (Field of View, FOV) is an astronomical term that refers to the extent of the sky that can be seen through a telescope. The field of view represents the maximum range that can be observed, usually expressed in degrees, and the larger the field of view, the larger the observation range.

As shown in FIG. 3 to FIG. 5 , the telescope device for rapid identification of transient source celestial bodies provided by the embodiment of the present invention includes: a multifunctional turntable 1 , a first equatorial mount bracket 2 , a second equatorial mount bracket 3 , and a lens barrel 4 , base 5, optical lens 6.

Example 1

The base 5 in this embodiment is rotatably fixed with a multi-function stage changer 1, and the multi-function stage changer 1 is rotatably fixed with a first equatorial mount bracket 2 and a second equatorial mount bracket 3, and the second equatorial mount bracket 3 is arranged on the first equatorial mount bracket 3. On the inner side of the equatorial mount bracket 2, there are four first equatorial mount brackets 2 and second equatorial mount brackets 3, and they are evenly arranged at 90 degrees; the height of the second equatorial mount bracket 3 is higher than that of the first equatorial mount bracket 2, and the first Telescopes are installed on the equatorial mount bracket 2 and the second equatorial mount bracket 3; the equatorial mount bracket can rotate 360° to ensure uninterrupted scanning of the whole sky area. The rotation of the function changer 1 can realize 360° rotation in the horizontal direction. In addition, each set of telescope equipment can be rotated independently, which has better tracking flexibility.

The number of telescopes on the equatorial mount or the second equatorial mount 3 is 1-4. The telescope is provided with a lens barrel 4, and the inner front end of the lens barrel 4 is clamped with an optical lens 6. The diameter of the telescope is 15cm, the matrix of the optical lens 6 is K9 glass, quartz glass or fluoride glass, and the number of the optical lens 6 is 1-10 pieces; the optical field of view of the telescope is 14°*14°. The system layout of the invention is more compact, which is convenient for the realization of the overall control; at the same time, the speed of searching and scanning the target in the whole sky area can also be improved; the cost of the system.

Example 2

On the basis of Embodiment 1, the diameter of the telescope in this embodiment is 15cm, the matrix of the optical lens 6 is K9 glass, the number of optical lenses 6 is 6, and the optical field of view of a single telescope can reach 14°*14°. Two above-mentioned telescopes are placed on each of the four first equatorial mount supports 2, and two above-mentioned telescopes are placed on each of the second equatorial mount supports 3 to carry out the construction of the transient source target search system. By controlling the main control system and starting the observation system, the multi-functional platform 1 mainly rotates 360° in the horizontal azimuth. Monitoring; the monitoring work in the 33°-90° sky area is monitored by the telescope placed on the second equatorial mount 3 by means of pitch scanning. Both sets of telescope systems rotate with the turntable to monitor and search the entire sky area within a 360° range. Multiple telescopes acquire observation data at the same time. Each telescope is matched with a graphics workstation to process the acquired observation data in real time. For change monitoring, after multi-frame identification of eligible observation images, they are stored in the database, and then the collection of observation data is continued. If the observed image does not conform to the target characteristics, no data processing is required, and the data acquisition work is carried out directly.

Example 3

As shown in FIG. 3 , on the basis of Example 1, the diameter of the telescope in this example is 15cm, the matrix of optical lens 6 is K9 glass, the number of lenses is 6, and the optical field of view of a single telescope can reach 14°*14°. Two of the above-mentioned telescopes are placed on the four first equatorial mount supports 2. To save costs, only one of the above-mentioned telescopes is placed on the second equatorial mount support 3 to construct the transient source target search system. By controlling the main control system , start the observation system, the multi-function changer 1 mainly rotates 360° in the horizontal azimuth, the telescope on the first equatorial mount 2 maintains the pitch angle of 25°, and monitors the sky area of 18-32°; 33-90 °The monitoring work in the sky area is monitored by the telescope placed on the second equatorial mount support 3 by means of pitch scanning. Both sets of telescope systems rotate with the turntable to monitor and search the entire sky area within a 360° range. Multiple telescopes acquire observation data at the same time. Each telescope is matched with a graphics workstation to process the acquired observation data in real time. For change monitoring, after multi-frame identification of eligible observation images, they are stored in the database, and then the collection of observation data is continued. If the observed image does not conform to the target characteristics, no data processing is required, and the data acquisition work is carried out directly.

The working principle of the present invention is as follows: by controlling the main control system, the observation system is activated, the multi-function changer 1 mainly rotates 360° in the horizontal azimuth, the telescope on the first equatorial mount 2 keeps the pitch angle at 25°, and the 18- The 32° sky area is monitored; the surveillance work in the 33-90° sky area is monitored by the telescope placed on the second equatorial mount 3 by means of pitch scanning. Both sets of telescope systems rotate with the turntable to monitor and search the entire sky area within a 360° range. Multiple telescopes acquire observation data at the same time. Each telescope is matched with a graphics workstation to process the acquired observation data in real time. For change monitoring, after multi-frame identification of eligible observation images, they are stored in the database, and then the collection of observation data is continued. If the observed image does not conform to the target characteristics, no data processing is required, and the data acquisition work is carried out directly.

The present invention adopts a centralized control method, and the overall layout is shown in Figure 1. There are 8 sets of optical telescope systems, which are uniformly fixed on the multifunctional turntable. The equatorial mount shown in Figure 2 can be rotated 360°, ensuring uninterrupted scanning of the entire sky. The telescope system placed on the multi-function turntable realizes 360° rotation in the horizontal direction with the rotation of the multi-function turntable. In addition, each set of telescope equipment can be rotated independently, which has better tracking flexibility. The base marked 1 is equipped with 2 optical telescopes (field of view is 14°*14°), and the 4 sets of telescope systems can realize low-elevation, broadband scanning and searching for transient source celestial objects. For high elevation angle and zenith scanning and searching for transient sources, two optical telescopes (field of view 14°*14°) placed on the base marked 2 are completed by means of elevation scanning, which scans the sky area. A schematic diagram of the scope is shown in Figure 7. At the same time, by optimizing the control and image processing software and using the layout of the above-mentioned telescope device, it is possible to carry out real-time monitoring and search work for the transient source celestial body in the whole sky area. In the present invention, by increasing the field of view of the telescope, the speed of scanning and searching can be further improved; by increasing the number of telescopes placed on the base 2 and changing the rotation speed, the speed of scanning and searching the sky area can also be improved. The layout structure of the system can be changed by changing the number of telescopes on the base, the diameter of the telescope (changing the field of view), etc., or the overall layout structure can be changed by continuing to increase the number of bases. In addition, change the shape of the turntable, if it is round now, it can be changed into square and so on.

The method for constructing a telescope system for rapid identification of a transient source celestial body of the present invention mainly includes three parts: a telescope system, a control system and an image data processing system, and the specific process is shown in FIG. 6 .

The telescope system of the present invention can realize the telescope optical system of different monitoring fields by changing the size, material and structure of the optical lens of the telescope; change the number of telescopes to realize the adjustment of the monitoring sky area of a single set of telescopes. The size of the optical lens can be 1cm～100cm; the material of the optical lens can be K9 glass, quartz glass and fluoride glass; the number of lenses of the optical system can be 1 to 10; the size, material and quantity of the optical lens used can be One or more of the materials and dimensions mentioned above. The number of telescopes that can be placed on each rack is 1 to 4.

The control system of the present invention can realize the search speed for the monitoring target by adjusting the rotation speed and rotation direction/azimuth of the telescope.

The image data processing system of the present invention can improve the speed of image processing by optimizing the algorithm (artificial intelligence) of the image processing software, and facilitate target recognition.

By integrating the above three parts, a telescope system for rapid identification of transient celestial objects can be obtained.

The present invention is further described below in conjunction with the experimental results.

Figure 8 is a schematic diagram of observation using the "M" type and "Z" type observation strategies, respectively. The classic transient source search process is shown in Figure 9. The main principle is to subtract the observed image (a) and the template image (b). If it is a transient source (ie, a new source), the In the residual image (c) after completion, an image similar to a complete point source will appear, such as o1 and o2 in Figure 9, while other incomplete image spots are noise generated during the subtraction process, as shown in Figure 9 (c). ) in n1, n2 and n3. Therefore, how to automatically and quickly identify the transient source in the residual image from the surrounding noise is one of the key problems to be solved by the technical solution. Will be based on isophotometric measurement of new characteristic parameters such as star image contour, use actual star image contour simulation and build a more realistic training sample algorithm; add noise filtering criteria based on measured data analysis and other methods to achieve an optimized transient source fast Automatic identification system.

Fig. 10 is an actual photograph of the transient source search carried out by the technical solution.

Figure 10 shows the results of scanning and searching for an all-sky area initially observed using this technical solution.

In the description of the present invention, unless otherwise stated, "plurality" means two or more; the terms "upper", "lower", "left", "right", "inner", "outer" The orientation or positional relationship indicated by , "front end", "rear end", "head", "tail", etc. are based on the orientation or positional relationship shown in the accompanying drawings, and are only for the convenience of describing the present invention and simplifying the description, not An indication or implication that the referred device or element must have a particular orientation, be constructed and operate in a particular orientation, is not to be construed as a limitation of the invention. Furthermore, the terms "first," "second," "third," etc. are used for descriptive purposes only and should not be construed to indicate or imply relative importance.

It should be noted that the embodiments of the present invention may be implemented by hardware, software, or a combination of software and hardware. The hardware portion may be implemented using special purpose logic; the software portion may be stored in memory and executed by a suitable instruction execution system, such as a microprocessor or specially designed hardware. Those of ordinary skill in the art will appreciate that the apparatus and methods described above may be implemented using computer-executable instructions and/or embodied in processor control code, for example on a carrier medium such as a disk, CD or DVD-ROM, such as a read-only memory Such code is provided on a programmable memory (firmware) or a data carrier such as an optical or electronic signal carrier. The device and its modules of the present invention can be implemented by hardware circuits such as very large scale integrated circuits or gate arrays, semiconductors such as logic chips, transistors, etc., or programmable hardware devices such as field programmable gate arrays, programmable logic devices, etc., It can also be implemented by software executed by various types of processors, or by a combination of the above-mentioned hardware circuits and software, such as firmware.

The above are only specific embodiments of the present invention, but the protection scope of the present invention is not limited to this. Any person skilled in the art is within the technical scope disclosed by the present invention, and all within the spirit and principle of the present invention Any modifications, equivalent replacements and improvements made within the scope of the present invention should be included within the protection scope of the present invention.

Claims (10)

1. A telescope control method, characterized in that the telescope control method comprises:

firstly, uniformly fixing a plurality of sets of optical telescope systems on a multifunctional turntable, realizing 360-degree rotation and realizing uninterrupted scanning of a whole day area;

secondly, the multiple sets of telescope systems realize the work of scanning and searching the transient source celestial body at a low elevation angle and a broadband, and the work of scanning and searching the transient source at a high elevation angle and a zenith is finished by multiple sets of optical telescopes arranged on a base in a pitching scanning mode;

and thirdly, realizing real-time monitoring and searching work of the whole day area on the transient source celestial body by optimizing control and image processing software and utilizing the layout of the telescope device.

2. The telescope control method according to claim 1, wherein the telescope control method is used for realizing telescope optical systems with different monitoring fields of view by changing the size, the material and the structure of optical lenses of the telescope; the adjustment of the monitoring sky area of a single set of telescope is realized by changing the number of the telescopes.

3. The telescope control method as recited in claim 1, wherein the field of view of the 2 optical telescopes is 14 ° by 14 °.

4. A computer device, characterized in that the computer device comprises a memory and a processor, the memory storing a computer program which, when executed by the processor, causes the processor to carry out the steps of:

step one, 8 sets of optical telescope systems are uniformly fixed on a multifunctional turntable, 360-degree rotation is realized, and uninterrupted scanning of a whole day area is realized;

secondly, 4 sets of telescope systems realize the work of scanning and searching the transient source celestial body at a low elevation angle and a broadband, and the work of scanning and searching the transient source at a high elevation angle and a zenith is finished by 4 sets of optical telescopes arranged on a base in a pitching scanning mode;

and thirdly, realizing real-time monitoring and searching work of the whole day area on the transient source celestial body by optimizing control and image processing software and utilizing the layout of the telescope device.

5. A computer-readable storage medium storing a computer program which, when executed by a processor, causes the processor to perform the steps of:

step one, 8 sets of optical telescope systems are uniformly fixed on a multifunctional turntable, 360-degree rotation is realized, and uninterrupted scanning of a whole day area is realized;

secondly, 4 sets of telescope systems realize the work of scanning and searching the transient source celestial body at a low elevation angle and a broadband, and the work of scanning and searching the transient source at a high elevation angle and a zenith is finished by 4 sets of optical telescopes arranged on a base in a pitching scanning mode;

and thirdly, realizing real-time monitoring and searching work of the whole day area on the transient source celestial body by optimizing control and image processing software and utilizing the layout of the telescope device.

6. A telescope control system for operating the telescope control method according to any one of claims 1 to 3, the telescope control system comprising:

the telescope system module is used for realizing monitoring and searching of different monitoring fields;

the control system module is used for realizing the searching speed of the monitored target by adjusting the rotating speed and the rotating direction/direction of the telescope;

and the image data processing module is used for realizing target identification by optimizing the algorithm of the image processing software.

7. A telescope control apparatus equipped with the telescope control system according to claim 6, wherein the telescope control apparatus is provided with:

a base;

the multifunctional turntable is rotationally fixed on the base, a first equatorial instrument support and a second equatorial instrument support are rotationally fixed on the multifunctional turntable, the second equatorial instrument support is arranged on the inner side of the first equatorial instrument support, and the number of the first equatorial instrument support and the number of the second equatorial instrument support are four and are uniformly arranged at 90 degrees;

the second equatorial telescope support is higher than the first equatorial telescope support, and the first equatorial telescope support and the second equatorial telescope support are both provided with a telescope.

8. The telescope control apparatus according to claim 7, wherein the number of telescopes on the first equatorial mount or the second equatorial mount is 1-4.

9. The telescope control apparatus according to claim 1, wherein the telescope is provided with a lens barrel, and an optical lens is engaged with a front end of an inner side of the lens barrel;

the aperture of the telescope is 15cm, the optical lens substrate is K9 glass, quartz glass or fluoride glass, and the number of the optical lenses is 1-10; the optical field of view of the telescope is 14 degrees or 14 degrees; the aperture and the view field of the telescope are both variable, and the change of the view field changes along with the change of the aperture.

10. An observation terminal of an astronomical transient source, characterized in that the observation terminal of the astronomical transient source is provided with the telescope control device of any one of claims 7-9.

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