CN210036681U - Subreflector pose measuring system of large radio telescope - Google Patents
Subreflector pose measuring system of large radio telescope Download PDFInfo
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- CN210036681U CN210036681U CN201920862589.4U CN201920862589U CN210036681U CN 210036681 U CN210036681 U CN 210036681U CN 201920862589 U CN201920862589 U CN 201920862589U CN 210036681 U CN210036681 U CN 210036681U
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Abstract
The utility model provides a large-scale radio telescope's subreflector position appearance measurement system, including main reflecting surface and subreflector, main reflecting surface's center department is equipped with feed source storehouse, and first laser instrument is installed to subreflector's border department, and feed source storehouse's top is the plane, installs feed horn, black dash receiver and long distance laser rangefinder on the plane, and feed horn's side-mounting has the alignment the camera of black dash receiver, the camera measures the two-dimensional position of the facula that first laser instrument fell on the black dash receiver, and long distance laser rangefinder measures its distance to between the subreflector. The utility model discloses an subreflector position appearance measurement system adopts PSD to replace power detection, can acquire the three-dimensional displacement data of subreflector under the imperfect condition of large-scale radio telescope construction initial stage link system, founds the three-dimensional gravity model of subreflector to carry out quantitative qualitative analysis to the influence of temperature, wind load and this kind of unstable factors of instantaneous start-stop to the subreflector position appearance.
Description
Technical Field
The utility model belongs to the radio telescope field, concretely relates to subreflector position appearance measurement system of large-scale radio telescope.
Background
The pointing error is one of the important factors influencing the efficiency of the antenna of the large radio telescope. During the operation of the radio telescope, along with the change of the azimuth angle of pitch, the comprehensive influence of gravity, sunlight, wind load and the like on the auxiliary reflecting surface support rod can cause the change of the pose of the auxiliary reflecting surface of the telescope, thereby causing the increase of pointing error.
Among the many factors, gravity is the most influential and stable factor. At present, a gravity model of an auxiliary reflecting surface is constructed by using a radio-electric method to correct the pose change of the auxiliary reflecting surface caused by gravity. The radio method determines the optimal position of the subreflector corresponding to different pitching positions by searching the maximum power point and the maximum antenna efficiency point of the telescope at different pitching positions, thereby constructing a gravity model of the subreflector. The method combines the existing main reflecting surface correction technology and the pointing correction technology, so that the telescope can meet the requirement of pointing accuracy in the working process.
However, the radio-frequency method has defects, and the method needs to stop observation for scanning detection; the telescope can be carried out only under the condition that the whole signal receiving system and the link transmission system of the telescope are complete; because real-time monitoring cannot be achieved, only modeling can be performed on the inherent factor of gravity, and the change conditions of the positions and the postures of the sub-reflecting surfaces during temperature, wind load and instantaneous start and stop of the antenna cannot be quantitatively and qualitatively analyzed.
SUMMERY OF THE UTILITY MODEL
An object of the utility model is to provide a large-scale radio telescope's subreflector position appearance measurement system to found the gravity model of subreflector, quantitative qualitative analysis temperature, wind carried and antenna instantaneous start-stop are to the influence of subreflector position appearance.
In order to achieve the above object, the utility model provides a large-scale radio telescope's subreflector position appearance measurement system, including main reflecting surface and subreflector, main reflecting surface's center department is equipped with a feed storehouse, a first laser instrument is installed to subreflector's border department, the top in feed storehouse is a plane, install feed loudspeaker on this plane, one with black dash receiver and a long distance laser rangefinder that first laser instrument aligns each other, the side-mounting of feed loudspeaker has an alignment the camera of black dash receiver, the camera measures the two-dimensional position of the facula that first laser instrument fell on the black dash receiver, long distance laser rangefinder measures its distance to between the subreflector.
And a network switch connected with a computer terminal device is arranged in the feed source bin.
The camera is communicatively coupled to the network switch via a network interface.
The long-distance laser ranging equipment comprises an RS422 serial port and is in communication connection with the network switch through the RS422 serial port.
The long-distance laser ranging device comprises a second laser, and the emission direction of the second laser is aligned with the middle ring of the auxiliary reflecting surface.
The first laser is adjusted in position through a universal support and fixed at the edge of the subreflector through a stainless steel square tube.
The first laser is covered by a stainless steel cover.
The black receiving plate is fixed at the top end of the feed source bin through an adhesive tape.
The camera is covered by a stainless steel cover.
The long-distance laser ranging equipment is fixed to the top end of the feed source bin through a vertical mounting frame.
The utility model discloses a large-scale radio telescope's subreflector Position appearance measurement system adopts laser instrument and the black dash receiver of aiming at each other, and adopt a camera to aim at this black dash receiver and receive the change of laser facula Position, and combine a long distance laser rangefinder, thereby adopt PSD (Position Sensing Device Position sensor Device) to replace power detection, can acquire the three-dimensional displacement data of subreflector under the imperfect condition of large-scale radio telescope construction initial stage link system, can be used for constructing the three-dimensional gravity model of subreflector fast, help revising the influence of gravity to the subreflector Position appearance, and can real-time supervision subreflector Position appearance state after the gravity model is constructed, can carry out qualitative analysis to temperature, wind-load and the influence of opening and stopping this kind of unstable factor to the subreflector Position appearance.
Drawings
Fig. 1 is a schematic structural diagram of an auxiliary reflection surface pose measurement system of a large radio telescope according to an embodiment of the present invention.
Fig. 2 is a measurement schematic diagram of the method for measuring the pose of the secondary reflecting surface of the large radio telescope according to the utility model.
Fig. 3 is a schematic view of the measurement result of the gravity model obtained by the method for measuring the pose of the subreflector of the large-scale radio telescope according to the utility model.
Fig. 4 is a schematic diagram showing the result of the influence of the temperature on the pose of the subreflector, which is obtained by the method for measuring the pose of the subreflector of the large-sized radio telescope according to the present invention.
Fig. 5 is a schematic diagram showing the result of the influence of wind load on the pose of the subreflector obtained by the method for measuring the pose of the subreflector of the large-sized radio telescope according to the present invention.
Detailed Description
Fig. 1 shows an auxiliary reflection surface pose measurement system of a large radio telescope according to an embodiment of the present invention, which is based on PSD and includes a main reflection surface 1 and an auxiliary reflection surface 2 fixed directly above a feed bin at the center of a cylinder of the main reflection surface 1 by four supporting legs 101.
A first laser 21 is mounted at the edge of the sub-reflecting surface 2. The position of the first laser 21 is adjusted by a gimbal so that the emitting direction of the first laser 21 is aligned with the black receiving plate 5 at the top end of the feed bin 3, and is fixed at the edge of the sub-reflecting surface 2 by a 304 stainless steel square tube. In addition, the first laser 21 is covered by a stainless steel cover and is provided with a dedicated power supply.
The center of the main reflecting surface 1 is provided with a feed source bin 3, a network switch 31 connected with a computer terminal device 7 is arranged in the feed source bin 3, the top end of the feed source bin is a plane, a plurality of wave band feed source horns are arranged on the plane, one of the feed source horns is an L wave band feed source horn 4, a black receiving plate 5 and a long-distance laser ranging device 6. The feed source loudspeaker 4 is a part of the current telescope system and is not a part of the PSD measuring system, and a camera in the PSD measuring system is installed and fixed by means of the position of the existing feed source loudspeaker 4.
The black receiving plate 5 is fixed on the top end of the feed bin 3 through an adhesive tape and is aligned with the first laser 21, so that the laser emitted by the first laser 21 can be received and the facula of the laser can be displayed. The black receiving plate 5 is used to reduce the probability that the camera 41 erroneously captures a field point at the time of gray level recognition.
Wherein a camera 41 is mounted on the side of the feed horn 4. The industrial camera is preferably a CCD camera which is directed at the black receiving plate 5 to measure the two-dimensional position of the spot of the first laser 21 falling on the black receiving plate 5 based on gray level recognition. The camera 41 is in communication connection with the network switch 31 through a network interface 411, and is configured to send the acquired data to the computer terminal device 7 through the network interface 411 via the network switch 31 of the feed bin 3, so as to obtain the x-direction and y-direction displacements of the sub-reflecting surface 2 in real time according to the acquired two-dimensional data of the light spot. The first laser 21 and the camera 41 thus form part of a PSD measurement system, enabling measurement of x and y displacements of the sub-reflector 2. In addition, the camera 41 is covered by a stainless steel cover to prevent the network interface thereof from being corroded by rainwater.
The long range laser ranging device 6 is fixed to the top of the feed bin 3 by a vertical mount (which is also part of the telescope system currently available) for measuring its distance to the subreflector 2. Which comprises a second laser 61 and an RS422 serial port 62, the emitting direction of the second laser 61 is aligned with the middle ring of the sub-reflecting surface 2, wherein the sub-reflecting surface 2 is composed of three-turn panels so as to emit visible light beams with different frequencies to the middle-turn position of the sub-reflecting surface 2, the long-distance laser ranging device 6 receives scattered laser returned from the sub-reflecting surface 2, compares the phase of the received laser signal with that of a reference signal, and the distance value of the z-direction displacement of the sub-reflecting surface 2 corresponding to the phase offset is calculated according to the principle of the phase comparison method, the long-distance laser ranging device 6 is in communication connection with the network switch 31 through the RS422 serial port 62, and the distance value is sent to the computer terminal device 7 through the network switch in the feed bin (namely, the long-distance laser ranging device 7 directly provides a distance value to be sent to a user through the serial port by adopting the principle of the phase comparison method). Thereby, measurement of z-directional displacement of the sub-reflecting surface 2 is achieved.
Therefore, the utility model discloses a large-scale radio telescope's subreflector position appearance measurement system can acquire the three-dimensional displacement data of subreflector in real time.
According to the position and posture measuring system of the auxiliary reflecting surface of the large radio telescope, the position and posture measuring method of the auxiliary reflecting surface of the large radio telescope comprises the following steps:
step S1: constructing the position and orientation measuring system of the auxiliary reflecting surface of the large radio telescope;
step S2: changing the pitch angle of the telescope for many times, respectively driving the subreflector 2 to generate x-direction displacement and y-direction displacement under each different pitch angle through software, and acquiring two-dimensional data xpsd and ypsd of the spot displacement of the laser of the first laser 21 under different x-direction displacement xsub and y-direction displacement ysub by adopting a camera 41 to obtain calibration data.
The step S2 is performed when the temperature and the wind load are constant and the influence of the temperature and the wind load on the pose of the sub-reflecting surface 2 is small (for example, at a sunny and windless night). The temperature difference change at night is small, the situation that direct sunlight does not exist or the steel building is slowly cooled after being heated after the steel building is set in the mountains in the evening is generally selected, the temperature difference of the temperature is approximately within 2 ℃, and the wind speed is generally the situation that the wind cannot be felt, for example, the wind speed is less than 1 m/s. However, the two values have no hard requirement, and the measurement accuracy is as high as possible by selecting temperature and good weather with little wind influence when the measurement is carried out by a radio method or other high-accuracy measurements of a large radio telescope. Since calibration is performed to obtain the relationship between the change of the light spot collected by the camera 41 and the change of the displacement of the sub-reflecting surface, and the instability of wind and temperature itself causes errors, the sub-reflecting surface of the antenna should be affected by gravity as much as possible when the calibration data is collected.
The utility model discloses an its subreflector of large-scale radio telescope possess six connecting rod regulatory function, consequently in step S2, can change the x and the y displacement of subreflector through the software drive, the working range of the angle of pitch (EL, elevation) of telescope is 7 to 88, and the interval of selecting the angle of pitch among the calibration process is 5.
Because the coordinate origin of the sub-reflecting surface 2 and the camera 41 are not defined the same, there is an angle θ between the first direction of spot displacement (corresponding to the two-dimensional data xpsd) and the x-directionaAn included angle theta exists between the second direction (corresponding to the two-dimensional data ypsd) of the light spot displacement and the y directionbAnd since the camera 41 itself has a focal length setting, there is a zoom, for example, the sub-reflecting surface 2 is displaced by 1mm, and the corresponding spot may be displaced by 1.5mm, which is a zoom amount of 1.5 times. The two-dimensional spot data acquired by the camera 41 is zoomed, translated and rotated to obtain two-dimensional data of pose change of the sub-reflecting surface in the sub-reflecting surface displacement process.
In step S2, the scaling data includes: a pitch angle EL (when the pitch angle is 88 °, that is, when the telescope is placed close to the sky, and the four supporting legs of the sub-reflecting surface are uniformly stressed), two-dimensional data offx and offy of the spot position, two-dimensional data xpsd and ypsd of the spot displacement, fitting slopes kx and ky, and an included angle θ between the x direction and the first direction of the spot displacement (corresponding to the two-dimensional data xpsd) acquired by the camera 41 when the sub-reflecting surface 2 is in the initial stateaAnd an angle theta between the y direction and a second direction of the spot displacement (corresponding to the two-dimensional data ypsd)b。
Wherein the offx and offy can be obtained by acquiring two-dimensional data of the spot position with the camera 41 when the pitch angle of the sub-reflecting surface is set to be close to 90 ° (to be 88 °).
The two-dimensional data xpsd and ypsd of the light spot displacement are respectively as follows:
xpsd＝xpsd_x-offx；ypsd＝ypsd_y-offy，
wherein xpsd _ x and ypsd _ y are two-dimensional data of the spot position acquired by the camera 41 in real time, respectively, and offx and offy are two-dimensional data of the spot position acquired by the camera 41 in the initial state of the sub-reflecting surface 2, respectively.
The fitting slopes kx and ky are slopes obtained by fitting the two-dimensional data xpsd and ypsd of the displacement of the light spot relative to the x-direction displacement and the y-direction displacement respectively.
θaIs the angle between the x-direction and the first direction of spot displacement, thetabIs the angle between the y direction and the second direction of spot displacement, thetaaAnd thetabThe method can be calculated by using an arctangent function, and the calculation formula is as follows:
θa＝arctan(kx)，
where kx and ky are the fitted slopes.
Step S3: and calibrating by using the calibration data to obtain a matrix function relation between the x-direction displacement xsub and the y-direction displacement ysub of the auxiliary reflecting surface 2 and the two-dimensional data xpsd and ypsd of the light spot displacement. From this, according to the matrix function relational expression that obtains the utility model discloses a large-scale radio telescope's subreflector position appearance measuring method can obtain the subreflector two-dimensional position situation of change in real time according to the two-dimensional facula data xpsd _ x and ypsd _ y that obtain in real time through camera 41.
In step S3, for the two-dimensional data xpsd and ypsd of the spot displacement corresponding to the case where the pitch angle is unchanged and the sub-reflecting surface 2 is only displaced in the x direction, the matrix functional relation between the x-direction displacement xsub and the y-direction displacement ysub of the sub-reflecting surface 2 and the two-dimensional data xpsd and ypsd of the spot displacement is as follows:
for the two-dimensional data xpsd and ypsd of the spot displacement corresponding to the unchanged pitch angle and the y-direction displacement of the sub-reflecting surface 2, the matrix function relation between the x-direction displacement xsub and the y-direction displacement ysub of the sub-reflecting surface 2 and the two-dimensional data xpsd and ypsd of the spot displacement is as follows:
in the formulae (1) and (2), sx1,sx2,sy1,sy2Is a scaling factor, θaIs the angle between the x-direction and the first direction of spot displacement, thetabIs the angle between the y-direction and the second direction of spot displacement.
Thus, the values θ of the respective transformation matrix parameters of the matrix function relational expression can be scaled by the scaling data obtained in step S2a,θb,sx1,sx2,sy1,sy2The numerical value of (c).
Step S4: and measuring the vertical distance between the long-distance laser ranging equipment 6 and the subreflector by adopting the long-distance laser ranging equipment 6 under each different pitching angle to obtain the z-direction displacement of the subreflector 2, thereby constructing a three-dimensional gravity model of the subreflector 2 according to the relation between the three-dimensional displacement and the pitching of the subreflector. Wherein the gravity model comprises the variation relation of the x-direction displacement xsub, the y-direction displacement ysub and the z-direction displacement of the auxiliary reflecting surface 2 along with the pitch angle.
When the position of the sub-reflecting surface 2 is changed under the influence of gravity at different pitch angles, the light spot of the second laser 61 used by the long-distance laser ranging apparatus 6 during distance measurement may deviate from the principle position, and since the sub-reflecting surface 2 is a hyperboloid, the hyperbolic relation between the y direction and the z direction of the sub-reflecting surface 2 may cause a component of y direction displacement of the sub-reflecting surface 2 to be superimposed into z direction displacement, a component of z direction change may be introduced into the y direction change according to the curvature of the sub-reflecting surface 2 during the measurement, and the z direction displacement of the sub-reflecting surface 2 may be obtained after correcting the z direction component into the measured data, so the step S4 further includes: and (5) correcting the distance between the long-distance laser ranging device 6 and the sub-reflecting surface by using the two-dimensional data xpsd and ypsd of the light spot displacement in the step (S2) to obtain the z-direction displacement of the sub-reflecting surface 2.
Step S5: under the condition that the influence of temperature, wind load or instantaneous start and stop of an antenna on the pose of the auxiliary reflecting surface 2 is large, the camera 41 is adopted to obtain two-dimensional data xpsd and ypsd of the light spot displacement of the laser of the first laser 21, the long-distance laser ranging equipment 6 is adopted to obtain the distance (namely z-direction data) between the long-distance laser ranging equipment and the auxiliary reflecting surface, and the influence of the temperature, the wind load or the instantaneous start and stop of the antenna on the pose of the auxiliary reflecting surface 2 is analyzed by utilizing the gravity model in the step S4.
Therefore, the utility model discloses a large-scale radio telescope's subreflector position appearance measuring method can acquire the three-dimensional displacement data of subreflector in real time, builds three-dimensional gravity model. As shown in fig. 2, gravity is a fixed factor that affects the pose of the sub-reflecting surface 2, and once determined, a gravity model can be constructed. The temperature is the gradual change process, and it is the uncertain factor that influences the subreflector position appearance the same as wind load and the inertial action of instantaneous start-stop, can't establish the inherent model, through adopting the utility model discloses a subreflector position appearance measuring method of large-scale radio telescope that subreflector position appearance measuring system of large-scale radio telescope realized can real-time supervision sunshine arouse prop the influence of leg local temperature effect, wind load and instantaneous start-stop these factors to the subreflector position appearance. After the three-dimensional displacement of the subreflector is obtained through real-time monitoring, the fixed quantity of the gravity model can be removed, and further, three transient factors of temperature, wind and instantaneous start and stop can be subjected to quantitative and qualitative analysis. Measurement results
The 65 meters astronomical telescope antenna of a cassegrain structure is used as the large radio telescope of the utility model to explain the measurement result of the position and orientation measurement method of the secondary reflection surface of the large radio telescope.
The resulting calibration data is shown in table 1 according to step S2 above.
TABLE 1 calibration data
| EL(°) | θa(rad) | kx | θb(rad) | ky | offx(mm) | offy(mm) |
| 88 | 1.1697 | -2.357 | 0.4049 | 0.4285 | 13.7 | 16.1 |
| 83 | 1.1738 | -2.385 | 0.3910 | 0.4122 | 17.2 | 17.1 |
| 78 | 1.1690 | -2.353 | 0.4058 | 0.4296 | 20.4 | 19 |
| 73 | 1.1856 | -2.466 | 0.4112 | 0.4360 | 23 | 20.6 |
| 68 | 1.1632 | -2.316 | 0.3943 | 0.4160 | 25.7 | 22.5 |
| 63 | 1.1743 | -2.388 | 0.3996 | 0.4223 | 28 | 24.2 |
| 58 | 1.1624 | -2.310 | 0.4116 | 0.4366 | 30 | 26.1 |
| 53 | 1.1586 | -2.286 | 0.4011 | 0.4241 | 32.6 | 27.3 |
| 48 | 1.1770 | -2.406 | 0.3938 | 0.4155 | 34.6 | 29.1 |
| 43 | 1.1683 | -2.348 | 0.3968 | 0.4190 | 36.2 | 30.3 |
| 38 | 1.1614 | -2.304 | 0.3863 | 0.4067 | 37.4 | 31.8 |
| 33 | 1.1690 | -2.353 | 0.4000 | 0.4228 | 38.8 | 33.1 |
| 28 | 1.1858 | -2.467 | 0.3862 | 0.4066 | 39.4 | 34 |
| 23 | 1.1693 | -2.355 | 0.3961 | 0.4182 | 39.7 | 35.1 |
| 18 | 1.1608 | -2.300 | 0.3886 | 0.4095 | 39.4 | 35.7 |
| 13 | 1.1746 | -2.390 | 0.4163 | 0.4421 | 39.3 | 36.4 |
| 8 | 1.1626 | -2.3119 | 0.3911 | 0.4123 | 38.2 | 37.1 |
TABLE 2 transformation matrix parameter values
| θa(rad) | θb(rad) | sx1 | sx2 | sy1 | sy2 |
| 1.1697 | 0.3985 | 0.71 | 0.72 | 1.75 | 0.31 |
The values of the respective transformation matrix parameters according to the matrix function relational expression obtained in step S3 are shown in table 2.
According to step S4, the constructed gravity model is as shown in fig. 3.
In step S5, thermal deformation of the sub-reflecting surface leg support caused by temperature is also an important factor causing a change in the pose of the sub-reflecting surface 2, fig. 4 shows the influence of temperature on the pose of the sub-reflecting surface 2 in the x-direction and the y-direction, a clear day is selected, the 65 m astronomical telescope is placed in the sky, the sun rises in the morning, the temperature of the leg support facing the sun rises rapidly, the pose change speed of the sub-reflecting surface 2 is high, the temperature drop speed is low in the afternoon sun landing process, and the pose change speed of the sub-reflecting surface 2 is slower than that in the morning. In the case of breeze at night, the influence of wind load on the pose of the auxiliary reflecting surface 2 in the x direction and the y direction is monitored, as shown in fig. 5, the situation that the pose of the auxiliary reflecting surface 2 changes by less than 1mm after the temperature is completely cooled at 9 o' clock half night can be found, and in such a night in fine weather, after the influence on the pose of the auxiliary reflecting surface 2 is corrected by using a gravity model in the process of tracking the telescope, the pose change is small, and the direction of the telescope is correct, so that the high-precision pointing requirement of high-frequency observation is met. The utility model discloses can also be used for monitoring the influence of the appearance of aerial to subreflector 2 because of the overshoot that the inertial action of big mass arouses and the back pendulum phenomenon when the instantaneous start-stop.
What has been described above is only the preferred embodiment of the present invention, not for limiting the scope of the present invention, but various changes can be made to the above-mentioned embodiment of the present invention. All the simple and equivalent changes and modifications made according to the claims and the content of the specification of the present invention fall within the scope of the claims of the present invention. The present invention is not described in detail in the conventional technical content.
Claims (10)
1. An auxiliary reflecting surface pose measuring system of a large radio telescope comprises a main reflecting surface (1) and an auxiliary reflecting surface (2), wherein a feed bin (3) is arranged at the center of the main reflecting surface (1), it is characterized in that a first laser (21) is arranged at the edge of the sub-reflecting surface (2), the top end of the feed bin (3) is a plane, the plane is provided with a feed source horn (4), a black receiving plate (5) aligned with the first laser (21) and a long-distance laser distance measuring device (6), a camera (41) aligned with the black receiving plate (5) is arranged on the side surface of the feed source loudspeaker (4), the camera (41) measures the two-dimensional position of the spot of the first laser (21) falling on the black receiving plate (5), the long-distance laser ranging device (6) measures the distance between the long-distance laser ranging device and the auxiliary reflecting surface (2).
2. The system for measuring the pose of an auxiliary reflecting surface of a large-scale radio telescope according to claim 1, wherein a network switch (31) connected with a computer terminal device (7) is arranged in the feed bin (3).
3. The system for measuring the pose of a secondary reflecting surface of a large-sized radio telescope according to claim 2, wherein the camera (41) is communicatively connected to the network switch (31) through a network interface (411).
4. The system for measuring the pose of the subreflector of the large-scale radio telescope according to claim 2, wherein the long-distance laser ranging device (6) comprises an RS422 serial port (62), and is in communication connection with the network switch (31) through the RS422 serial port (62).
5. The system for measuring the pose of an auxiliary reflecting surface of a large-scale radio telescope according to claim 1, wherein the long-distance laser ranging device (6) comprises a second laser (61), and the emission direction of the second laser (61) is aligned with the middle circle of the auxiliary reflecting surface (2).
6. The system for measuring the pose of the subreflector of a large-scale radio telescope according to claim 1, wherein the first laser (21) is adjusted in position by a gimbal and fixed at the edge of the subreflector (2) by a stainless steel square tube.
7. The system for measuring the pose of a subreflector of a large-sized radio telescope according to claim 1, wherein the first laser (21) is covered with a stainless steel cover.
8. The position and orientation measurement system of the secondary reflecting surface of the large-scale radio telescope according to claim 1, wherein the black receiving plate (5) is fixed at the top end of the feed bin (3) by an adhesive tape.
9. The system for measuring the pose of an auxiliary reflecting surface of a large-sized radio telescope according to claim 1, wherein the camera (41) is covered with a stainless steel cover.
10. The system for measuring the pose of the subreflector of a large-scale radio telescope according to claim 1, wherein the long-distance laser ranging device (6) is fixed to the top end of the feed bin (3) through a vertical mounting bracket.
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