CN114860196A - Telescope main light path guide star device and calculation method of guide star offset - Google Patents
Telescope main light path guide star device and calculation method of guide star offset Download PDFInfo
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Abstract
The invention relates to a telescope main optical path guide star device, which comprises a telescope main focus detector and a guide star detector, wherein the telescope main focus detector is positioned on a telescope focal plane, and the telescope main focus detector comprises: the guide star detector is arranged near the telescope prime focus detector, is in a focal plane with the prime focus detector, and shares the same optical path with the telescope prime focus detector. The invention realizes the guiding of the main light path, so as to eliminate the position and angle errors of the guiding detector and the main detector and improve the guiding and tracking precision of the telescope. The invention also discloses an algorithm of the vector offset, the vector camera sends the formed image to a program for processing in a certain exposure time, the program finds a star body in the image data by using a method in the field of image processing, and obtains XY (row and column) offset according to the historical record of the star body position, and then the offset is returned to a moving mechanism of the telescope to make the telescope perform correction movement, thereby achieving the purpose of compensation and forming a more reliable closed-loop control system.
Description
Technical Field
The invention belongs to the technical field of telescopes, and particularly relates to a telescope main optical path guide star device and a guide star offset calculation method, wherein a guide star detector is designed on a main optical path of a telescope, and a plurality of bright stars in a guide star image are solved by using algorithms such as image processing and the like to obtain the position offset of the bright stars so as to correct the movement of a right ascension declination or horizontal pitching axis of the telescope.
Background
The guide star of the astronomical telescope is a function during observation, and the guide star is mainly used in the following occasions: (1) and observing while tracking the stars, and performing long-time tracking continuous imaging shooting or long-time exposure imaging shooting on the stars. Due to the earth's autobiography, if the telescope is stationary, the stars will move from east to west on the celestial coordinate system at 15 ʺ/s along an axis parallel to the earth's equator, with the equatorial axis of the equatorial telescope parallel to the earth's axis of rotation. To counteract the effects of earth rotation, the right ascension axis should be moved from east to west at 15 ʺ/s, with the image of the target celestial body fixed in the field of view. In the same way, in order to counteract the rotation of the earth and ensure that the observed target is fixed in the field of view, the horizontal and pitching angles of the horizontal telescope need to be corrected and adjusted when the target is exposed for a long time or is subjected to tracking shooting for a long time, so that the phenomenon that the target is smeared in the image is avoided.
(2) For the targets of fast moving celestial bodies such as solar asteroid, comet and low-orbit satellite, because the target moving speed is fast, although the trailing phenomenon is easy to generate under the condition of short-time exposure, the correction quantity of the telescope pointing direction must be calculated by means of the star guide equipment of the telescope, and the control of the telescope (equator or horizontal type) frame is guided to offset the relative movement between the telescope and the fast moving celestial body.
The guide star camera is an imaging device arranged on an optical axis of a telescope, most of guide star imaging detectors are positioned outside a main focus at present, and some guide star imaging detectors are arranged near a lens cone of the telescope and are called as offset guide stars. That is, the star finder is not located on the main optical axis of the telescope, as shown in fig. 1 by taking a reflective main telescope and a refractive star finder as an example. The guide star camera system is designed to be parallel to a main light path outside a main lens cone, and is equivalent to an independent small telescope system. The method has the advantages that the independent guide telescope system is easy to install and debug, but because the guide light path and the telescope light path are separated from each other, the light path inevitably generates position and angle errors, and the guide and tracking precision of the telescope is influenced.
Disclosure of Invention
The invention provides a telescope main optical path guide star device and a method for calculating the guide star offset, which effectively solve the problems.
In order to achieve the purpose, the invention adopts the following technical scheme:
the utility model provides a telescope main light path guide star device, includes telescope principal focal detector and leads star detector, and telescope principal focal detector is located the telescope focal plane, wherein: the guide star detector is arranged near the telescope main focus detector, is positioned on a focal plane with the main focus detector, and shares the same optical path with the telescope main focus detector.
Furthermore, the star guide detector consists of a plurality of star guide cameras, the telescope main focus detector comprises a plurality of main focus scientific imaging detectors and a wavefront imaging detector, the star guide cameras are installed around the main focus scientific imaging detectors, and the wavefront imaging detectors are also arranged around the main focus scientific imaging detectors.
Furthermore, the number of the satellite guiding cameras is four, and the satellite guiding cameras are installed around the main focus scientific imaging detector at equal intervals.
Furthermore, the main focus scientific imaging detector is a large-target-surface high-resolution spliced CCD and is used for accurately and scientifically imaging an astronomical scientific target.
The method for calculating the guide star offset applies a telescope main optical path guide star device and comprises the following steps:
step one, when the telescope works, the guide star detector continuously acquires image data from the optical path of the telescope,
step two, selecting a predetermined number of brightest stars in the first frame image data as the guide stars, determining the coordinates, brightness, Full Width Half Maximum (FWHM) and time information of the guide stars,
step three, extracting the brightest star bodies with the preset number in the next frame image as the updated guide star, determining the coordinate, the brightness, the FWHM and the time information of the updated guide star,
matching the updated guide star with the guide star of the previous frame, calculating the offset on the guide star coordinate, and returning the offset to the motion mechanism of the telescope to make the telescope perform correction motion;
and step five, repeating the step three and the step four until the guide process is finished.
In image data acquired by a guide star detector, a star body used as a guide star is a bright star, when the guide star coordinate is determined, the center of the bright star is taken as the guide star coordinate, before the guide star coordinate is extracted, whether the point spread function PSF and the FWHM of an image are within a preset range or not is detected, if the point spread function PSF and the FWHM are within the preset range, the image is judged to be properly focused, the guide star coordinate is extracted, if the point spread function PSF and the FWHM are beyond the preset range, the image is judged to be improperly focused, and a picture is discarded and a warning is sent.
And step four, when the updated guide star is matched with the guide star of the previous frame, if the offset of the coordinate of a certain updated guide star exceeds the offset threshold, judging that a new bright star is added, abandoning the image of the previous frame, and taking the current frame image as the first frame, and executing the step two.
Selecting three brightest stars as guide stars, correspondingly, in the fourth step, judging the offset of the three bright stars in the current frame and the three bright stars in the previous frame in the X and Y directions as six quantities, namely star 0_ X, star 0_ Y, star 1_ X, star 1_ Y, star 2_ X and star 2_ Y, if the offset exceeding the offset threshold is calculated in the six quantities, determining that one or more stars brighter than the three bright stars in the previous frame are contained in the newly shot image, and performing the second step by taking the current frame image as the first frame.
The invention has the beneficial effects that:
1. the invention directly designs the guide star on the main focus detector of the telescope, and the guide star and the main light path are the same light path, thereby realizing the guide star of the main light path, eliminating the position and angle errors of the guide star detector and the main detector, and improving the guide star and tracking accuracy of the telescope.
2. The invention also discloses an algorithm program of the guide star offset, a guide star camera carries out target imaging according to the optical design (including a target surface, a focal length, a visual field and the like) of the guide star camera and the telescope pointing direction within a certain period of exposure time, the formed image is sent to a program for processing, the program finds a star body in image data by using a method in the field of image processing, XY (row and column) offset is obtained according to the historical record of the star body position, and then the offset is returned to a moving mechanism of the telescope to guide the telescope to carry out correction movement, so that the compensation purpose is achieved, and a more reliable closed-loop control system is formed.
3. The invention also solves two important problems in the algorithm program of the guide star offset: (1) the focusing problem of the image, in the process of extracting the central coordinate of the bright star, the quality of the image has great influence on the accuracy of the central extraction, before the central coordinate is extracted, judging the quality of the image and the quality of focusing, adopting the FWHM (full width at half maximum) value of PSF (point spread function) as the judgment basis for judging whether the image focusing is proper or not to ensure the accuracy of the leading star coordinate, (2) after processing one image and extracting the brightness of three bright stars and the respective coordinates, a bright star is newly captured when the next image is processed, and the brightness of the bright star is located in the first three digits in the image, this is a very special but existing situation, and the present invention, by adding the offset threshold, can determine whether there is a new brightest star added, by invalidating the last image and not participating in the calculation, a new operation is started with the current image (containing the newly added bright star) as the first frame. The method is a safe working mode, and the correctness of image matching is ensured.
4. The invention uses star-like brightness as standard to sort and identify celestial body targets in the guide star on the basis of astronomical image processing algorithm, and matches and calculates the position offset of the guide star target in a plurality of images by extracting the center coordinate, FWHM (full width at half maximum) and brightness information of image spots. The algorithm can meet the requirement that the director corrects the pointing direction of the telescope in real time, is quick and accurate, and the final offset result can be quickly returned to a telescope control system for processing and correction.
Drawings
Fig. 1 is a schematic diagram of a prior art device using a reflective main telescope and a refractive star finder as a star finder.
FIG. 2 is a diagram of the main light path guiding star type light path of the present invention (to)Cassegrain systemFor example);
FIG. 3 is a schematic view of the focal plane distribution of the telescope prime focus detector;
FIG. 4 is a schematic diagram of bright stars in a set of guide star images;
FIG. 5 is a graph of FWHM (last term in the series of values) and profile for an imperfect focus;
FIG. 6 is a plot of FWHM (last term in the series of values) and profile for an ideal focusing;
FIG. 7 is a diagram illustrating a bright star match error;
FIG. 8 is a flowchart of a program for calculating the amount of shift of the guide star image.
Wherein the reference numerals are: the device comprises a telescope main focus detector 1, a wavefront imaging detector 2, a guide star detector 3, a guide star camera 31 and a main focus scientific imaging detector 4.
Detailed Description
The invention will be further described with reference to the accompanying drawings.
As shown in fig. 2-3, the telescope main optical path star guide device of the present invention includes a telescope main focus detector 1 and a star guide detector 3, the telescope main focus detector 1 is located on the telescope focal plane, wherein: the guide star detector 3 is arranged near the telescope main focus detector 1, is positioned on a focal plane with the main focus detector, and shares the same optical path with the telescope main focus detector 1.
The guide star detector 3 is composed of a plurality of guide star cameras 31, the telescope main focus detector 1 comprises a plurality of main focus scientific imaging detectors 4 and a wave front imaging detector 2, the guide star cameras 31 are installed around the main focus scientific imaging detectors 4, and the wave front detector 2 is also arranged around the main focus scientific imaging detectors 4.
The number of the guide star cameras 31 is four, and the guide star cameras 31 are installed around the main focus scientific imaging detector 4 at equal intervals.
The main focus scientific imaging detector 4 is a spliced CCD with a large target surface and high resolution, and is used for accurately and scientifically imaging an astronomical scientific target, and the wave front imaging detector (2) (four in design) is a technology for imaging in wave front in order to realize active optical adjustment of a main mirror. The objective of active optics is that the telescope system can maintain its primary mirror in an optimal imaging condition to resist the effects of environmental forces such as wind, sag, thermal expansion, and deformation of the telescope axis. The wavefront detector can measure the pupil-surface wavefront error of the imaging system in real time, then converts the measured data into a control signal of the active optical system, and controls the optical characteristics of the imaging system in real time. The purpose of the star finder is to perform real-time correction and guidance on a motion axis of a telescope when the telescope performs perpetual motion or performs quick tracking on a shooting target or performs long-time exposure shooting.
The invention is practically applied to a 2.5m large-view-field telescope (WFST) of the Arnica astrology platform of the Chinese academy of sciences. The WFST telescope is a ground-level large-view-field telescope, the focal plane detector of which consists of 9 main-focus scientific imaging detectors, 8 wavefront imaging detectors and 4 guide star detectors (the guide star detectors are shown as a dashed line frame in figure 3), the aperture of the main mirror of the telescope is 2.5 meters, the effective focal length of the system is 6.2 meters, and the focal ratio is f/2.48. The main focus detector adopts a CCD290-99 detector, and the single-chip imaging target surface is 92.2 mmx92.4mm. The guide star detector adopts a CCD47-20 detector, the single-chip imaging target surface is 13.3mmx13.3mm, the view field of the main focus scientific camera obtained by combining the focal length of the system is about 3 < x > 3 ℃, the imaging view field of the single-chip guide star detector is 7.4 ʹ < x > 7.4 ʹ, and the spatial pixel resolution is 0.43 ʺ/pixel. Different from the common telescope, the guide star of the WFST telescope related to the invention is directly positioned near the main focus detector and is designed with four CCD frame transfer detectors on the periphery, and the design of the plurality of guide star detectors increases the probability that the guide star can capture the bright star and comprehensively calculates the data of the four guide stars, so that the data for calculating the offset of the guide star is more accurate.
The invention relates to a specific algorithm of the guide star offset besides the guide star optical equipment of the main optical path.
The image of the guide star is a group of continuous multi-frame images generally taken when the telescope tracks, and the image processed by the experiment is a group of continuous 5-frame exposure images. The image name is:
HT0001316-2.fits,HT0001317-2.fits,HT0001318-2.fits,HT0001319-2.fits,HT0001320-2.fits，
the exposure time for each image was 30 seconds and the time interval between images was also approximately 30 seconds.
The general idea of the method for extracting the guide star offset is to use a sexfractor tool to extract the bright source of a fits image through programming, and arrange the images according to the bright source after extraction, in order to reduce the time consumed by the image algorithm, only the brightest three stars in the images are arranged in the program, so as to determine the brightest three stars in the five images as star0, star1 and star2 (the brightness is sequentially reduced), as shown in fig. 4. After the three best bright stars are determined, star0 in the multiple graphs can be determined to be the same star, star1 and star2 are the same, the central coordinates of star0, star1 and star2 in the graphs are extracted according to a central coordinate extraction method, and time information and the XY coordinate values of the bright stars are extracted from the header file of each of the fists format files and recorded. The program is written in python language, and finally time-position values and two-dimensional motion tracks of three bright stars are formed.
There are two particular cases in this approach that require special handling:
(1) focusing of images and extraction of bright star centers
After the paired target star is determined, extracting the center position coordinates of the star is another problem. The image spots (circles) of the guide targets in the CCD image are different in size due to the difference in the star number, distance, etc. of the guide targets, and therefore, it is necessary to accurately extract the center position coordinates of the entire image spots as the position information thereof for processing.
In the process of extracting the center coordinates of the bright stars, the quality of the image has a great influence on the accuracy of the center extraction, so that the quality of the image and the quality of focusing need to be judged before extracting the center coordinates. Fig. 5 and 6 are profile curves of FWHM and its flux for sub-optimal and optimal focus, respectively.
The present invention adopts the FWHM (full width at half maximum) value of the PSF (point spread function) as a criterion for judging whether image focusing is appropriate. The larger FWHM value indicates that the focusing is not required, and at this time, the calculation program is stopped to remind the operator of focusing. When the FWHM value is in a reasonable range, the program continues to extract information of the next image for processing. The present invention sets the FWHM range as a threshold variable in the program, which can be set and modified to accommodate different detectors and optical systems.
(2) A special target match error condition
After the extraction of the brightness of three bright stars and the extraction of the respective coordinates after processing one image, a new bright star is shot when processing the next image, and the brightness of this bright star is located in the first three digits in this image, which is a very special case. As shown in fig. 7, if a new brightest star (star D') is added to the image 2. According to the flow of the program, the first three light stars in image 2 have been changed to D ', A ' and B ' in sequence, and the offsets calculated for their pairing with image 1 have been changed to AD ' _ X, AD ' -Y, BA ' _ X BA ' _ Y, CB ' _ X and CB ' _ Y, which is obviously a wrong pairing, and the offsets calculated therefrom are also wrong due to a matching error. To correct for this false match, the program sets another threshold that determines the X and Y offsets of the current three bright stars in the frame from the previous three bright stars in the previous frame as six total amounts, star 0_ X, star 0_ Y, star 1_ X, star 1_ Y, star 2_ X, and star 2_ Y. According to the setting of the 2.5m WFST exposure time, for example, 5 second exposure is set, and the position change of the target is 75 arc seconds if the telescope does not follow the shooting. Given that the spatial resolution of the star finder is 0.43 "/pixel, the variation of the stars in the CCD coordinate system within 5 seconds is 175 pixels, i.e. the maximum variation of the above six quantities is 175, if a larger offset than 175 is found in the six quantities, it is possible that one or more stars brighter than the last three bright stars are included in the newly captured image, as in the above figure if AD ' _ x and AD ' _ y are calculated to be significantly larger than AA ' _ x and AA ' _ y, D ' is a newly added bright star. At this time, the program will suggest to the observer to check whether there is an obvious bright star newly added to the image queue, and to restart the calculation, and to invalidate the last image without participating in the calculation, and start a new operation with the current image (containing the newly added bright star) as the first frame. The method is a safe working mode, and the correctness of image matching is ensured. If the newly shot image contains the new bright star, but the new bright star is not bright as the last three bright stars, the newly added bright star has no influence on the calculation result of the program, the influence can be ignored, and the program continues to run. The program sets the maximum variation value of the above six quantities as a threshold variable that can be modified, possibly calculated and set according to the exposure time or the spatial resolution of the detector.
(3) Speed of program operation
The purpose of the guide star is to correct the pointing direction of the telescope in real time, so that the algorithm and processing requirements on the guide star are fast and accurate, and the final offset result can be fast returned to the telescope control system for processing and correction.
In order to meet the requirements, the invention uses star-like brightness as a standard to sort and identify celestial body objects in the guide stars on the basis of an astronomical image processing algorithm, uses a SExtractor tool to extract the center coordinates, FWHM (full width at half maximum) and brightness information of image spots, and matches and calculates the position offset of the guide star objects in a plurality of images through Python programming.
Compared with the method of resolving the WCS (world coordinate system) coordinates of each image and then extracting the coordinates of the stars under the coordinate system, the method of sorting according to the brightness and extracting the centers avoids the process of a star table, greatly shortens the time consumed by calculation and improves the real-time property of the calculation result.
The data processing program calls a mature and widely-used photometric data processing software Source Extractor (sextagactor) to perform photometry on the image, including Source detection and positioning, Source flow calculation and the like. Compare image processing toolkit IRAF that tradition was used commonly, the sextramtor calls conveniently, and is fast, is convenient for integrate to the data processing procedure, and sextramtor can once only accomplish source detection and photometry in addition, need not divide multistep to go on, can also carry out multiple mode, multiple aperture photometry simultaneously, and efficiency is higher.
As shown in fig. 8, when all the images are processed, the program directly prints and outputs a scatter diagram of XY coordinates and time of the first three brightest stars in each frame of image.
The above is only a preferred embodiment of the present invention, and the protection scope of the present invention is not limited to the above-mentioned embodiments, and all technical solutions belonging to the idea of the present invention belong to the protection scope of the present invention. It should be noted that modifications and embellishments within the scope of the invention may be made by those skilled in the art without departing from the principle of the invention.
Claims (8)
1. The utility model provides a telescope main light path guide star device, includes telescope principal focus detector (1) and leads star detector (3), and telescope principal focus detector (1) is located telescope focal plane, characterized by: the guide star detector (3) is arranged near the telescope main focus detector (1), is positioned on a focal plane with the main focus detector, and shares the same optical path with the telescope main focus detector (1).
2. A telescope main light path guide star device according to claim 1, characterized in that: the telescope main focus detector (1) comprises a plurality of star guide cameras (31), the telescope main focus detector (1) comprises a plurality of main focus scientific imaging detectors (4) and a wave front imaging detector (2), the star guide cameras (31) are installed around the main focus scientific imaging detectors (4), and the wave front detector (2) is also arranged around the main focus scientific imaging detectors (4).
3. A telescope main optical path guide star device according to claim 2, characterised by: the number of the guide star cameras (31) is four, and the guide star cameras (31) are installed around the main focus scientific imaging detector (4) at equal intervals.
4. A telescope main optical path guide star device according to claim 3, characterised by: the main focus scientific imaging detector (4) is a large-target-surface high-resolution spliced CCD and is used for accurately and scientifically imaging an astronomical scientific target.
5. The method for calculating the guide star offset is characterized by comprising the following steps: the telescope main optical path guiding star device as claimed in claim 1, wherein the following steps are carried out:
step one, when the telescope works, the guide star detector (3) continuously acquires image data from the optical path of the telescope,
step two, selecting a preset number of brightest stars in the first frame image data as the guide stars, determining the coordinates, the brightness, the full width half maximum value FWHM and the time information of the guide stars,
step three, extracting the brightest star bodies with the preset number in the next frame image as the updated guide star, determining the coordinate, the brightness, the FWHM and the time information of the updated guide star,
matching the updated guide star with the guide star of the previous frame, calculating the offset on the guide star coordinate, and returning the offset to the motion mechanism of the telescope to make the telescope perform correction motion;
and step five, repeating the step three and the step four until the guide process is finished.
6. The method of claim 5, wherein: in the image data acquired by the guide star detector (3), a star body used as a guide star is a bright star, when the guide star coordinate is determined, the center of the bright star is taken as the guide star coordinate, before the guide star coordinate is extracted, whether the point spread function PSF and the FWHM of the image are within a preset range or not is detected, if the point spread function PSF and the FWHM are within the preset range, the image is judged to be properly focused, the guide star coordinate is extracted, if the point spread function PSF and the FWHM are beyond the preset range, the image is judged to be improperly focused, and the image is discarded and a warning is sent.
7. The method of claim 6, wherein: and step four, when the updated guide star is matched with the guide star of the previous frame, if the offset of the coordinate of a certain updated guide star exceeds the offset threshold, judging that a new bright star is added, abandoning the image of the previous frame, and taking the current frame image as the first frame, and executing the step two.
8. The method of claim 7, wherein: selecting three brightest stars as guide stars, correspondingly, in the fourth step, judging the offset amounts of the three bright stars in the current frame and the three bright stars in the previous frame in the X and Y directions to be recorded as six amounts of star 0_ X, star 0_ Y, star 1_ X, star 1_ Y, star 2_ X and star 2_ Y, if the offset amount exceeding the offset threshold value is solved, determining that one or more stars brighter than the three bright stars in the previous frame are included in the newly shot image, invalidating the image of the previous frame, and executing the second step by taking the current frame image as the first frame.
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Cited By (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN115437030A (en) * | 2022-08-23 | 2022-12-06 | 中国科学院云南天文台 | Guide star closed-loop tracking method and system for high-dispersion optical fiber spectrometer |
| CN115829916A (en) * | 2023-02-20 | 2023-03-21 | 中国科学院云南天文台 | Method and system for rapid target identification and pointing correction of high-dispersion optical fiber spectrometer |
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Cited By (4)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN115437030A (en) * | 2022-08-23 | 2022-12-06 | 中国科学院云南天文台 | Guide star closed-loop tracking method and system for high-dispersion optical fiber spectrometer |
| CN115437030B (en) * | 2022-08-23 | 2024-01-30 | 中国科学院云南天文台 | Star-guiding closed-loop tracking method and system for high-dispersion optical fiber spectrometer |
| CN115829916A (en) * | 2023-02-20 | 2023-03-21 | 中国科学院云南天文台 | Method and system for rapid target identification and pointing correction of high-dispersion optical fiber spectrometer |
| CN115829916B (en) * | 2023-02-20 | 2023-08-11 | 中国科学院云南天文台 | Method and system for rapid target identification and pointing correction of high-dispersion optical fiber spectrometer |
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