CN103206964A - Spectrum weight tunable weak light star simulation system - Google Patents

Abstract

The invention relates to a simulation system for weak light stars with adjustable spectral weight. The system includes a spectral simulation subsystem with adjustable spectral weight and a large-aperture stray light elimination device arranged on the outgoing light path of the spectral simulation subsystem with adjustable spectral weight. Star simulator subsystem. The invention proposes a large-aperture, stray light elimination and high measurement precision tunable spectral weight simulation system for weak light stars and the like.

Description

Spectral Weight Tunable Faint Magnitude Simulation System

technical field

The invention belongs to the technical field of optical detection, and relates to a magnitude simulator system, in particular to a large-aperture, stray light-eliminating, faint-light star magnitude simulation system with adjustable spectral weight.

Background technique

In deep space exploration and astronomical observation, in order to detect stars with weak brightness or farther away from the earth, it is necessary to develop some high-sensitivity detection cameras, and this detection camera has a strong detection ability, and there is no effective standard test in China equipment to calibrate its detection capabilities. For conventional detection cameras, the following two methods are usually used in China to calibrate the detection capabilities of detection cameras: one is to take pictures of internationally recognized stars with known magnitudes in the mountains far away from the city, and then the collected data Perform processing to complete the calibration and calibration of the detection camera. The disadvantages of this method are: ① affected by natural conditions and weather, sometimes waiting for dozens of days may not necessarily wait for the weather to meet the experimental conditions; ② affected by the absorption of the spectrum by the atmosphere, the measurement accuracy of atmospheric density and the atmospheric transmittance ③ due to the non-uniform absorption of the star radiation spectrum by the atmosphere, the spectral distribution received by the detection camera is different from the actual radiation spectral distribution of the star; Stray light makes the background of the detection camera brighter, and the faint target information is submerged in the dark background; another calibration method is to use a star simulator to simulate an infinite star point in the laboratory to complete the calibration of the detection capability of the detection camera. Not affected by weather conditions, the implementation is relatively simple, but this method also has many shortcomings: ①Since the stray light of the star simulator itself is difficult to eliminate, it cannot simulate higher magnitude stars; ②At present, the effective aperture of the star simulator in China is small , cannot complete the calibration task of the large-aperture detection camera; ③The simulated spectrum is single, that is, the laboratory can only simulate the radiance of the star, but cannot simulate the radiation spectrum distribution of the star, resulting in inaccurate calibration of the detection camera.

Therefore, the calibration of the detection capability of the detection camera should not only consider the submersion of the faint target information by stray light, but also consider the mismatch between the simulated star point spectrum and the actual star radiation spectrum, which leads to wrong calibration results. In order to solve many shortcomings and deficiencies in the detection capabilities of domestic calibration detection cameras at the present stage, the present invention designs and develops a large-aperture, stray light elimination, and adjustable spectral weight faint light star simulation system. In order to meet the high-precision calibration of the detection ability of the detection camera under various spectral curve distribution conditions.

Contents of the invention

In order to solve the above-mentioned technical problems in the background technology, the present invention proposes a large-aperture, stray light-eliminating and high-accuracy spectral weight tunable weak light star simulation system.

The technical solution of the present invention is: the present invention provides a simulation system for faint light stars with adjustable spectral weights, which is special in that: the simulated system for faint stars with adjustable spectral weights includes adjustable spectral weights type spectrum simulation subsystem and a large-aperture stray-light star simulator subsystem arranged on the exit light path of the spectrum weight-adjustable spectrum simulation subsystem.

The spectrum weight adjustable spectrum simulation subsystem includes a light source system, a light splitting system, a light intensity adjustment system, a spectrum mixing and monitoring system, and a control system; The outgoing light path of the system; the control system is respectively connected with the light source system, the light intensity adjustment system and the spectrum mixing and monitoring system.

The above-mentioned light source system includes a xenon light source, a parabolic condenser, a slit diaphragm and a collimating lens; the xenon light source is arranged in a concave cavity formed by the parabolic condenser; The outgoing light path after the reflection of the condenser;

The spectroscopic system includes a blazed grating and a converging lens; the blazed grating is set on the outgoing light path after the collimator lens; the converging lens is set on the outgoing light path of the blazed grating; the light intensity adjustment system includes an incident optical fiber array, a light Strong regulator and outgoing fiber array; the incident fiber array is arranged on the outgoing light path after the converging lens, and the incident end of the incident fiber array coincides with the focal plane of the image side of the converging lens; the light intensity adjuster is arranged on The outgoing optical path of the incident optical fiber; the outgoing optical fiber array is arranged on the outgoing optical path of the light intensity adjuster;

The spectrum mixing and monitoring system includes an integrating sphere, a spectral radiance meter probe and a manual iris; the integrating sphere is arranged on the outgoing optical path of the outgoing optical fiber array; the spectral radiance meter probe is arranged on the inner wall of the integrating sphere ; The manual iris is arranged at the exit of the integrating sphere;

The control system includes a xenon lamp controller, a light intensity regulator controller and a spectral radiance meter controller; the xenon lamp controller is connected to the xenon lamp light source; the light intensity regulator controller is connected to the light intensity regulator; the spectrum The radiometer controller is connected with the integrating sphere and is used for monitoring the spectral radiance value and the spectral distribution curve of the output of the integrating sphere.

The above-mentioned light intensity adjuster includes a motorized variable diaphragm and a relay lens; the motorized variable diaphragm and the relay lens are sequentially arranged on the outgoing light path after passing through the incident optical fiber array.

The above-mentioned relay mirror is a lens with a diameter of Φ8mm and a focal length of 5mm; the slit diaphragm is a rectangular diaphragm whose size is 1mm×4mm; the collimating lens has a diameter of Φ50mm and a focal length of 150mm lens; the grating constant of the blazed grating is 3.33×10 ^-3 mm, the blazed wavelength is 0.5 μm, the blazed angle is 4.3°, and the effective depicting area is 64mm×64mm; the converging lens has an aperture of Φ100mm and a focal length of 300mm lens; the incident optical fiber array includes 168 optical fibers; all the optical fibers of the incident optical fiber array are arranged in 4 rows in a regular hexagon; the single fiber diameter of the incident optical fiber array is Φ1.5mm, and the incident optical fiber array The fiber core diameter is Φ1.0mm; the outgoing fiber array includes 168 optical fibers, the diameter of a single fiber in the outgoing fiber array is Φ2mm, and the core diameter of the outgoing fiber array is Φ1.5mm.

The above-mentioned large-aperture star simulator subsystem for eliminating stray light includes a collimator, and the collimator includes a primary mirror, a first reflector, a second reflector, a third reflector and a plane reflector; the plane The reflector is set on the outgoing light path of the spectral weight adjustable spectrum simulation subsystem; the second reflector is set on the reflection light path of the plane reflector and the third reflector; the third reflector and the first reflector The primary mirror is set on the reflection light path of the second reflection mirror; the primary mirror is set on the reflection light path of the first reflection mirror; mirror, second reflector, third reflector, second reflector, first reflector and primary mirror.

The above-mentioned large-aperture stray light elimination star simulator subsystem also includes a stray light elimination component arranged inside the collimator.

The stray light elimination assembly includes a stray light diaphragm arranged between the third reflection mirror and the second reflection mirror and a light extinction cover arranged on the stray light diaphragm; the stray light diaphragm is arranged on the The reflected light path from the third reflector to the second reflector.

The above-mentioned stray light elimination assembly also includes a first stray light elimination tube arranged inside the exit port of the collimator, a shading cover outside the collimator exit port, a second stray light elimination tube arranged outside the main reflector, and a The third stray light elimination tube outside the first reflector and the extinction body arranged on the optical path between the second reflector and the third reflector; the extinction body is spliced by two extinction tubes with different calibers The stray light stop is a Φ1mm clear hole.

The above-mentioned large-aperture stray light elimination star simulator subsystem also includes a star point plate, and the star point plate is arranged on the primary image plane of the collimator.

The advantages of the present invention are:

The difference between the dim light magnitude simulation system with tunable spectral weights provided by the present invention and the traditional magnitude simulator is: ① the dim light magnitude simulation system with tunable spectral weights proposed by the present invention, in the optical system A secondary image plane is set up to enclose the space between the secondary image plane and the primary image plane into a closed space, and a stray light stop and a light shield are installed on the secondary image plane. In this way, for the light beam emitted from the light source, only the light within the effective solid angle can pass through the hood and exit the stray light diaphragm, while the light beams outside the effective solid angle emitted by the light source are all blocked by the light hood and the stray light diaphragm. Thereby fundamentally solve the shortcoming that the stray light of the traditional star simulator cannot be completely eliminated; ②The spectral weight tunable faint light star simulation system proposed by the present invention, the light source system adopts the spectral curve tunable uniform light source, and this function passes the xenon lamp , blazed gratings, light intensity modifiers and integrating spheres are implemented. Compared with the traditional star simulator, the light source system can simulate the radiation spectral lines of any star, avoiding the inaccurate calibration caused by the error between the simulated spectral lines and the actual star spectral lines. Specifically, the present invention has the following advantages:

1) A faint light star simulation system with tunable spectral weight of the present invention: using a blazed grating as a light splitting element, and then using a converging lens to integrate monochromatic light of various wavelengths into different optical fibers for transmission, reducing Reduce the loss of light energy of the system and reduce the volume of the system;

2) An analog system for weak light stars with adjustable spectral weights of the present invention: using a fiber array with a thick core and a thin cladding layer, and adopting a regular hexagonal arrangement, it has a very high filling factor;

3) A faint light magnitude simulation system with tunable spectral weight according to the present invention: 84 optical fibers are used in the 0.35μm-1.0μm spectral band, and the average spectral resolution is 7.86nm, which has a relatively high spectral simulation resolution. ability;

4) A faint light star simulation system with tunable spectral weight of the present invention: using a motorized iris, the weight of energy of various wavelengths can be automatically changed, and suitable radiation can be easily simulated according to the required spectral distribution curve spectrum;

5) A kind of faint light star simulation system with adjustable spectral weight of the present invention: use the integrating sphere as a spectral mixer, so that the simulated spectrum has very high spectral uniformity, angular uniformity and surface uniformity;

6) A faint light star simulation system with adjustable spectral weight of the present invention: a spectral radiance meter probe is installed on the inner wall of the integrating sphere, which can monitor the radiance and spectral distribution curve of the output spectrum in real time;

7) A faint light magnitude simulation system with tunable spectral weight of the present invention: a manual iris diaphragm is installed at the outlet of the integrating sphere, which can easily change the size of the radiation surface.

8) A dim light magnitude simulation system with tunable spectral weight of the present invention: since a secondary image plane is set in the optical path, a Φ1mm stray light stop and a light shield are set at the secondary image plane, and The system is also equipped with 3 extinction cylinders and 1 extinction body. The stray light extinction device can effectively block the stray light of the system.

The faint light magnitude simulation system with tunable spectral weight of the present invention, because the system has a very high ability to eliminate stray light, can simulate 16th magnitude stars or even higher magnitudes, which solves the problems caused by existing domestic star simulators. The stray light of the system is too large to simulate magnitudes above 10 with high precision; at the same time, the weak light magnitude simulation system of the present invention can provide uniform surface light sources with different spectral weights according to requirements. At present, only xenon lamps or tungsten halogen lamps can be used in China. The light source has a single simulated spectrum, which cannot meet the calibration work of the astronomical detection camera under different spectral energy distributions. Therefore, the present invention fills the blank that cannot simulate any star radiation spectrum in China.

Description of drawings

Fig. 1 is the structural representation of the system provided by the present invention;

Fig. 2 is the enlarged schematic view of the incident optical fiber array structure adopted in the present invention;

Fig. 3 is the enlarged schematic view of the light intensity regulator adopted in the present invention;

Fig. 4 is the enlarged schematic view of the stray light stop used in the present invention;

1-xenon light source, 2-parabolic condenser, 3-slit diaphragm, 4-collimator lens, 5-blazed grating, 6-converging lens, 7-incident fiber array, 8-light intensity adjuster, 81-motorized Diaphragm, 82-relay lens, 9-exit fiber array, 10-integrating sphere, 11-manual iris, 12-probe, 13-light intensity regulator controller, 14-spectral radiance meter, 15 -Xenon lamp light source controller, 16-main reflector, 17-first reflector, 18-second reflector, 19-third reflector, 20-plane reflector, 21-stray light elimination diaphragm, 22-light extinction cover, 23-first extinction cylinder, 24-second extinction cylinder, 25-third extinction cylinder, 26-extinction body, 27-light hood, 28-star point board.

Detailed ways

Referring to Fig. 1 , a kind of spectral weight tunable faint light star simulation system of the present invention includes a xenon lamp light source 1, a parabolic condenser lens 2, a slit diaphragm 3, a collimating lens 4, a blazed grating 5, a converging lens 6, an incident Optical fiber array 7, light intensity adjuster 8, motorized iris diaphragm 81, relay lens 82, exit fiber array 9, integrating sphere 10, manual iris diaphragm 11, probe 12, light intensity adjuster controller 13, spectrum Radiance meter 14, xenon lamp light source controller 15, main reflector 16, first reflector 17, second reflector 18, third reflector 19, plane reflector 20, stray light stop 21, extinction Cover 22, the first extinction tube 23, the second extinction tube 24, the third extinction tube 25, the extinction body 26, the shading cover 27, the star point plate 28; It is arranged on the outgoing light path of the parabolic condenser 2, the collimator lens 4 is arranged on the outgoing light path of the slit diaphragm 3, and its focus is located on the slit diaphragm 4, and the blazed grating 5 is arranged on the outgoing light path of the collimating lens 4 , to make the incident light wave diffract, the converging lens 6 is arranged on the outgoing optical path of the blazed grating 5, so that the diffracted waves of different wavelengths converge on the focal plane and interfere, thereby separating the spectra of different wavelengths to realize light splitting, and the incident optical fiber array 7 The incident end of the optical fiber array 9 is arranged on the focal plane of the converging lens 6, and the outgoing ends are respectively arranged on the entrance of the light intensity adjuster 8. On the integrating sphere 10, the manual iris 11 is arranged on the outlet of the integrating sphere 10, the probe 12 is arranged on the inner wall of the integrating sphere 10, and the main reflector 16 is arranged on the outgoing light path of the simulation system such as faint light stars, the first The secondary reflector 17, the second reflector 18, the third reflector 19 and the plane reflector 20 are arranged on the optical path between the collimator main mirror 16 and the focal plane, and the plane reflector 20 is used to deflect the system In the optical path, the stray light stop 21 is set on the secondary image plane of the star simulator, the light extinction cover 22 is set on the outside of the stray light stop 21 (see Fig. 4 ), and the second stray light tube 3 is set with a star simulation In the light exit port of the device, the second stray light elimination cylinder 4 is outside the main reflector 16, the second stray light elimination cylinder 5 is arranged outside the second reflection mirror 18, and the light extinguishing body 26 is provided with the secondary image surface of the star simulator And on the optical path in the middle of the primary image plane, the shading cover 27 is arranged outside the exit port of the weak light star magnitude simulation system, the star point plate 28 is arranged on the focal plane of the star simulator, the light intensity adjuster controller 13, the spectral radiance meter 14 and the xenon lamp controller 15 are arranged outside the system, and are used to control the radiance value and spectral distribution output by the entire analog system.

The spectrum emitted by the xenon lamp light source 1 is converged on the slit diaphragm 3 through the parabolic condenser 2, and after being modulated by the slit diaphragm 3, the collimated beam is formed by the collimating lens 4 and incident on the blazed grating 5, and the polychromatic collimated beam passes through After the blazed grating 5 diffracts, the exit angles of different wavelength spectra are different with respect to the normal line of the grating surface, and after being converged by the converging lens 6, interference is emitted on the focal plane of the converging lens 6 to form colored interference fringes, which enter the optical fiber The array 7 collects the spectral energy of different wavelengths into different optical fibers and transmits it to the light intensity adjuster 8, and changes the size of the light aperture of the relay mirror through the electric diaphragm 81 to realize the adjustment of the light intensity (see Figure 3). After adjustment The light is converged into the outgoing optical fiber array 9 through the relay lens 82, and then transmitted to the integrating sphere 10 through the outgoing optical fiber array 9. The diffuse reflection on the inner wall of the integrating sphere 10 makes the light waves of various wavelengths remix and output from the integrating sphere. . The manual iris 11 is used to change the size of the effective area of the outgoing light source, the light intensity regulator controller 12 is used to control the effective aperture of the electric iris 81, thereby adjusting the spectral energy of the corresponding wavelength, and the spectral radiance meter 13 is used to monitor the spectral radiance value and spectral distribution curve output by the integrating sphere 10 , and the xenon lamp light source controller 14 is used to control the xenon lamp light source 1 . The present invention utilizes the above-mentioned system to simulate uniform surface light sources with different weight spectral distributions.

The spectrum emitted by the xenon lamp is adjusted by the above-mentioned system, and after being emitted from the outlet of the integrating sphere to illuminate the star point plate, it enters the star simulator through the reflection of the plane mirror, and finally forms a parallel beam exiting from the outlet of the star simulator. The solid angle of the light beam emitted by the light source is much larger than the solid angle corresponding to the F# of the collimator, so most of the light energy emitted by the light source cannot simulate the light energy emitted by the infinite star point, and the diffuse reflection through the inner wall of the system becomes Harmful stray light in the star simulator system, and the existing star simulators only set some devices to block the stray light inside the system, which cannot effectively prevent the stray light from exiting the system exit. In order to fundamentally solve the influence of stray light on the system magnitude simulation accuracy, this paper proposes a new optical system structure of the star simulator, adding a secondary image plane to the optical path of the traditional collimator, and using an extinction body to divide the secondary image plane The optical path between the image plane and the primary image plane forms an airtight seal. A stray light stop and light extinction mask are installed on the secondary phase surface to absorb and block stray light. The effective simulated light beam passes through the stray light stop and light extinction smoothly. The hood forms a parallel light beam and exits from the exit port of the star simulator. The present invention just utilizes above-mentioned system to realize the function of eliminating stray light of analog systems such as faint light stars.

The specific principles are as follows:

① The realization principle of tunable spectral weight

The spectral energy radiated by the xenon light source 1 is converged by the parabolic condenser lens 2 onto the slit diaphragm 3, the light-passing area of the slit diaphragm 3 is 1mm×4mm, and the slit diaphragm 3 is located at the object focal point of the collimating lens 4 at the same time. On the plane, the effective clear aperture of the collimating lens 4 is Φ50 mm, and the focal length is 150 mm. The flat blazed grating 5 is installed at about 400 mm behind the collimating lens 4. The size of the light spot is Φ60mm, the facet of the blazed grating 5 is rectangular, and the effective area is 64mm×64mm. Therefore, all light energy is effectively reflected and diffracted. In the direction where the diffracted light exits, a distance of 500mm from the blazed grating is installed. A converging lens 6 with a focal length of 300 mm and an aperture of 100 mm can be calculated according to the characteristic size of the blazed grating, the blaze angle, and the focal length of the converging lens 6. The light waves of 350 nm to 1000 nm are arranged on the focal plane of the converging lens with a total width of about 63 mm and a length of About 8mm. The incident end of the incident fiber array 7 is installed on the focal plane of the converging lens 6, like this, the monochromatic light beams converged on the focal plane of the converging lens 6 will be respectively integrated into different optical fibers, and the incident fiber array 7 comprises 168 optical fibers in total , arranged in 4 rows according to a regular hexagon (see Figure 2), 42 in each row, the outer diameter of a single fiber is Φ1.5mm, and the core diameter is Φ1.2mm. Therefore, the overlapping width of the fiber cores of the upper and lower rows of fiber optic arrays is 0.45mm, which can avoid a large loss of spectral energy at the fiber cladding layer and cause the final spectrum to be discontinuous. Since a total of 84 optical fibers are used to collect spectral energy in the spectral range from 350nm to 1000nm, the average spectral resolution of the spectral simulator can reach 7.8nm. The monochromatic spectrum is respectively input into the light intensity adjuster 8 through the incident optical fiber array 7. The light intensity adjuster 8 includes 168 small units in total, and each small unit controls the output power of light energy of an optical fiber respectively. The incident end of the strong adjuster 8 is incident, and the size of the effective light aperture of the relay lens 82 is changed through the electric variable diaphragm 81 to achieve the purpose of adjusting the spectral output power. After the relay lens 82 converges, the effective spectrum is integrated and emitted In the optical fiber, 168 outgoing optical fibers form the outgoing optical fiber array 9 to transmit the adjusted spectrum in the integrating sphere 10. The inner wall of the integrating sphere 10 is uniformly coated with high diffuse reflection, and the spectra output by the 168 optical fibers are remixed to form A uniform spectrum emerges from the mouth of the integrating sphere. The spectral radiance meter 11 can monitor the spectral energy distribution curve inside the integrating sphere and the spectral radiance value emitted from the integrating sphere in real time, and the manual iris 10 is used to change the size of the uniform surface light source.

②Principle of stray light elimination function

After the light emitted by the integrating sphere light source illuminates the star point plate with the 2π(Sr) solid angle, the light energy radiated by the star point covers the space of 2π(Sr) solid angle, and the light energy in this 2π(Sr) solid angle space is According to the cosine radiator distribution, the total luminous flux is πLS. Generally, F#=10 of the star simulator system corresponds to the aperture angle of the optical system U=2.86°, the solid angle surrounded by the star point light source at the focus point of the exit pupil of the star simulator system is 0.031(Sr), and the included luminous flux is 0.031LS, and the total luminous flux radiated by the star point is πLS, it can be calculated that less than 1% of the light energy radiated from the star point is really useful light energy, while the remaining 99% of the energy is irradiated to the simulator The inner wall of the system forms stray light. Since there are many reasons for the formation of stray light (diffuse reflection of the inner wall of the system, scattering, scattering of optical glass, aperture diffraction, etc.), the distribution of stray light cannot be accurately tracked and calculated. The traditional star simulator only installs light shields around the optical glass of the system and dyes the inner wall of the system black, but this cannot effectively eliminate the stray light of the system. The star simulator designed and developed in this design adds a two-image plane in the optical path, and wraps the light path between the secondary image plane and the primary image plane into a closed space with a light-shielding body, and installs a medium-sized pass-through on the secondary image plane. In this way, 1% of the effective light beams will converge on the secondary image surface into a light spot with the same size as the light hole, and then exit to the next mirror smoothly, while the remaining 99% will form a light spot Astigmatism light will be absorbed by the inner wall after multiple reflections in this closed space.

The invention uses dispersion optical devices to arrange the polychromatic light separately according to the wavelength and integrate them into the optical fiber array, and transmit the spectra of different wavelengths to the light intensity adjuster through the optical fiber array, and the light intensity adjuster is adjusted according to the required spectral energy weight The amount of light passing through each wavelength, and finally the adjusted spectrum is output to the integrating sphere through the exit fiber for mixing, and then the required spectral distribution energy is uniformly output from the integrating sphere; the secondary image plane is set on the optical system, and the shading body is used to The secondary image surface and the primary image surface form a closed space, and a moderately sized light hole (stray light stop) is set on the secondary image surface, so that 1% of the effective light beam will be on the secondary image surface The upper surface converges into a light spot with the same size as the light hole, which smoothly exits to the next reflector, while the remaining 99% of the light that forms stray light will be absorbed by the inner wall after multiple reflections in this closed space. A weak light star simulation system with tunable spectral weight of the present invention solves the problem that traditional star simulators cannot simulate weak star point targets with high precision due to too much stray light; Blank for distributed light sources.

The faint light star simulation system with adjustable spectral weight of the present invention has a high ability to eliminate stray light and the function of adjustable spectral line weight, and can realize the spectral information and weak light of target stars that cannot be simulated by existing star simulators. The brightness information of the target; at the same time, the present invention can also be used for testing other optical performance indicators of the camera (focal length, field of view, MTF, visual discrimination rate, center of mass of the circle of confusion, etc.).

Claims (10)

1. A dim light magnitude simulation system with tunable spectral weight, characterized in that: the tunable spectral weight dim light magnitude simulation system includes a spectral weight adjustable spectral simulation subsystem and is set in an adjustable spectral weight The large-aperture stray-eliminated star simulator subsystem on the exit light path of the spectrum simulation subsystem. 2. The faint light star magnitude simulation system with adjustable spectral weight according to claim 1, characterized in that: the spectral simulation subsystem with adjustable spectral weight includes a light source system, a light splitting system, a light intensity adjustment system, and a spectral mixing system. and a monitoring system and a control system; the spectroscopic system, the light intensity adjustment system, and the spectrum mixing and monitoring system are sequentially arranged on the exit light path of the light source system; the control system is respectively connected with the light source system, the light intensity adjustment system, and the spectrum mixing and monitoring The system is connected. 3. The spectral weight tunable type weak light magnitude simulation system according to claim 2, characterized in that: The light source system includes a xenon light source, a parabolic condenser, a slit stop and a collimating lens; the xenon light source is arranged in a concave cavity formed by the parabolic condenser; the slit stop and the collimating lens are arranged in sequence through The outgoing light path reflected by the parabolic condenser mirror; The spectroscopic system includes a blazed grating and a converging lens; the blazed grating is set on the outgoing light path after the collimator lens; the converging lens is set on the outgoing light path of the blazed grating; the light intensity adjustment system includes an incident optical fiber array, a light Strong regulator and outgoing fiber array; the incident fiber array is arranged on the outgoing light path after the converging lens, and the incident end of the incident fiber array coincides with the focal plane of the image side of the converging lens; the light intensity adjuster is arranged on The outgoing optical path of the incident optical fiber; the outgoing optical fiber array is arranged on the outgoing optical path of the light intensity adjuster; The spectrum mixing and monitoring system includes an integrating sphere, a spectral radiance meter probe and a manual iris; the integrating sphere is arranged on the outgoing optical path of the outgoing optical fiber array; the spectral radiance meter probe is arranged on the inner wall of the integrating sphere ; The manual iris is arranged at the exit of the integrating sphere; The control system includes a xenon lamp controller, a light intensity regulator controller and a spectral radiance meter controller; the xenon lamp controller is connected to the xenon lamp light source; the light intensity regulator controller is connected to the light intensity regulator; the spectrum The radiometer controller is connected with the integrating sphere and is used for monitoring the spectral radiance value and the spectral distribution curve of the output of the integrating sphere. 4. The spectral weight tunable faint light magnitude simulation system according to claim 3, characterized in that: the light intensity regulator comprises an electric iris and a relay lens; the electric iris and The relay lens is sequentially arranged on the outgoing light path after passing through the incident optical fiber array. 5. The spectral weight tunable weak light magnitude simulation system according to claim 4, characterized in that: the relay mirror is a lens with a diameter of Φ8mm and a focal length of 5mm; the slit diaphragm is a rectangular light diaphragm, the size of the rectangular diaphragm is 1 mm × 4 mm; the collimating lens is a lens with a diameter of Φ50 mm and a focal length of 150 mm; the grating constant of the blazed grating is 3.33 × 10 ^-3 mm, and the blazed wavelength is 0.5 μm , the blaze angle is 4.3°, and the effective depiction area is 64mm×64mm; the convergent lens is a lens with a diameter of Φ100mm and a focal length of 300mm; the incident optical fiber array includes 168 optical fibers; The angular shape is arranged in 4 rows; the diameter of a single fiber of the incident fiber array is Φ1.5mm, and the core diameter of the incident fiber array is Φ1.0mm; the outgoing fiber array includes 168 optical fibers, and the outgoing fiber array The diameter of a single fiber is Φ2mm, and the core diameter of the outgoing fiber array is Φ1.5mm. 6. The spectral weight tunable weak light magnitude simulation system according to any one of claims 1-5, characterized in that: the large-aperture stray light elimination star simulator subsystem includes a collimator, and the The collimator includes a primary mirror, a first reflector, a second reflector, a third reflector and a plane reflector; the plane reflector is arranged on the outgoing optical path of the spectrum weight adjustable spectrum simulation subsystem; The second reflection mirror is arranged on the reflection light path of the plane reflection mirror and the third reflection mirror; the third reflection mirror and the first reflection mirror are arranged on the reflection light path of the second reflection mirror; The main mirror is set on the reflection optical path of the first reflector; the outgoing light of the spectral weight adjustable spectrum simulation subsystem passes through the plane reflector, the second reflector, the third reflector, and the second reflector in turn. mirror, primary mirror, and primary mirror. 7. The faint light magnitude simulation system with tunable spectral weight according to claim 6, characterized in that: the large-aperture stray light elimination star simulator subsystem also includes a stray light elimination component arranged inside the collimator . 8. The dim light magnitude simulation system with tunable spectral weight according to claim 7, characterized in that: the stray light elimination component includes a stray light elimination component arranged between the third reflection mirror and the second reflection mirror A light stop and a light extinction mask arranged on the stray light stop; the stray light stop is set on the reflected light path from the third reflector to the second reflector. 9. The faint light magnitude simulation system with tunable spectral weight according to claim 8, characterized in that: the stray light elimination component further comprises a first stray light elimination cylinder, a parallel light The shading cover outside the exit port of the light pipe, the second stray light elimination tube arranged on the outside of the main reflector, the third stray light elimination tube arranged on the outside of the first reflector, and the second reflector and the third reflector The extinction body on the optical path in the middle of the secondary reflector; the extinction body is spliced by two extinction tubes with different calibers; the stray light elimination diaphragm is a clear hole of Φ1mm. 10. The spectral weight tunable weak light magnitude simulation system according to claim 9, characterized in that: the large-aperture stray light elimination star simulator subsystem also includes a star point board, and the star point board is arranged on The primary image plane of the collimator.

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