A synchronous large-field-of-view photometry and spectrum measurement terminal system and its application

Abstract

The present application discloses a synchronous large-field-of-view photometry and spectrum measurement terminal system and its application, wherein the synchronous large-field-of-view photometry and spectrum measurement terminal system comprises: a starlight signal passes through the telescope primary mirror, with a first through hole in the middle; a secondary mirror, located in front of the starlight signal passing through the telescope primary mirror; a large-field-of-view corrector, located in the first through hole, collecting the light reflected from the secondary mirror; a plane reflector, provided with a second through hole, reflecting the light transmitted from the large-field-of-view corrector; a photometry system, located on one side of the plane reflector, receiving the light reflected from the reflector; a relay system, located behind the plane reflector, receiving the light transmitted from the reflective large-field-of-view corrector through the second through hole; a near-infrared low-dispersion spectrometer; and a high-dispersion spectrometer. One technical effect of the present application is that the same telescope can be used for simultaneous photometry and spectrum measurement, thereby improving the observation efficiency and the utilization rate of the telescope.

Description

Technical Field

[0001] The present application belongs to the technical field of optical equipment, and specifically relates to a synchronous large-field-of-view photometry and spectrum measurement terminal system and its application. Background Art

[0002] At present, the terminal equipment of optical telescopes mainly includes photometry systems and spectrometry systems. Different terminal equipment can be switched according to observation needs. At present, the method of plane reflectors is commonly used internationally, and the target source signal is reflected to different terminal equipment of the telescope by rotating (or moving) the plane mirror. The same telescope cannot take into account both photometry and spectrometry at the same time, which greatly reduces the observation efficiency and the utilization rate of the telescope. For example, for the detection of exoplanets, a high-efficiency large-field photometry survey is required to give the candidate source of the exoplanet, and then confirm it with the radial velocity method (high-dispersion spectrometer observation), and detect the planetary atmosphere (near-infrared low-dispersion spectrum); for the search of rapid target artificial satellites and space debris, the candidate source is selected by photometry. The traditional method requires switching terminals or changing telescopes, which may cause the loss of the target; the traditional spectrometry has low observation efficiency and cannot make full use of the effective field of view of the telescope. In addition, a conversion device needs to be installed on the telescope, which not only increases the load of the telescope, but also may cause instrument failure during the switching process. Especially for space telescopes, once a failure occurs, it is difficult to repair. Therefore, it is necessary to provide an improved synchronous large-field photometry and spectrometry terminal system. Summary of the invention

[0003] One purpose of the present application is to provide a new technical solution for a synchronous large-field-of-view photometry and spectral measurement terminal system.

[0004] According to one aspect of the present application, the present application provides a synchronous large-field-of-view photometry and spectrum measurement terminal system, comprising:

[0005] The starlight signal passes through the telescope primary mirror, the front end of which is the light-incoming end and has a first through hole in the middle;

[0006] The secondary mirror has a diameter smaller than that of the primary mirror of the telescope through which the starlight signal passes, is located before the light-incoming end of the primary mirror of the telescope, and reflects the light reflected from the light-incoming end to the first through hole;

[0007] A large field correction lens, located in the first through hole, collects light reflected from the secondary mirror and is configured to correct the aberration of the field of view;

[0008] A plane reflector, provided with a second through hole, located on a side of the large field of view corrector mirror away from the secondary mirror, and reflecting light transmitted from the large field of view corrector mirror;

[0009] A photometric system, located on one side of the plane reflector, receiving the light reflected by the reflector;

[0010] A relay system, located behind the plane reflector, receives the light transmitted by the reflective large field of view corrector through the second through hole;

[0011] a near-infrared low-dispersion spectrometer configured to receive near-infrared light transmitted by the relay system;

[0012] The high-dispersion spectrometer is configured to receive the visible light transmitted by the relay system.

[0013] Optionally, the starlight signal is coaxially arranged through the telescope primary mirror, secondary mirror and the large field of view correction mirror.

[0014] Optionally, the second through hole is coaxially arranged with the large field of view corrector.

[0015] Optionally, the second through hole is configured to transmit the optical signal of a star in the field of view transmitted by the large field of view corrector to the relay system.

[0016] Optionally, the second through hole is located at a focal plane position of light transmitted by the large field of view corrector.

[0017] Optionally, a diameter of the secondary mirror is larger than a diameter of the first through hole.

[0018] Optionally, the photometry system is a multi-channel photometry system.

[0019] According to another aspect of the present application, the present application also provides an application of the above-mentioned synchronous large-field-of-view photometry and spectrometry terminal system in exoplanet detection or searching for artificial satellites and near-Earth space debris.

[0020] One technical effect of the present application is that light and spectrum can be measured simultaneously using the same telescope, thereby improving observation efficiency and telescope utilization. BRIEF DESCRIPTION OF THE DRAWINGS

[0021] The drawings described herein are used to provide a further understanding of the present application and constitute a part of the present application. The illustrative embodiments of the present application and their descriptions are used to explain the present application and do not constitute an improper limitation on the present application. In the drawings:

[0022] Figure 1 It is a schematic diagram of the structures of some embodiments of the present application.

[0023] In the figure: 1. Secondary mirror, 2. Starlight signal passing through the telescope primary mirror, 3. Large field of view correction mirror, 4. Photometry system, 5. Plane reflector, 6. Relay system, 7. Near-infrared low-dispersion spectrometer, 8. High-dispersion spectrometer. DETAILED DESCRIPTION

[0024] The following will describe the implementation methods of the present application in detail with the help of accompanying drawings and examples, so that the implementation process of how the present application uses technical means to solve technical problems and achieve technical effects can be fully understood and implemented accordingly.

[0025] According to one aspect of the present application, the present application provides a synchronous large-field-of-view photometry and spectrum measurement terminal system. In some embodiments, reference Figure 1 , including: starlight signals are transmitted through the telescope primary mirror 2, secondary mirror 1, large field of view corrector 3, plane reflector 5, photometry system 4, relay system 6, near-infrared low-dispersion spectrometer 7 and high-dispersion spectrometer 8.

[0026] The front end of the starlight signal passing through the telescope main mirror 2 is the light input end. The starlight signal passes through the telescope main mirror 2 with a first through hole in the middle. The diameter of the secondary mirror 1 is larger than the diameter of the first through hole. The diameter of the secondary mirror 1 is smaller than the diameter of the starlight signal passing through the telescope main mirror 2. The secondary mirror 1 is located before the light input end of the starlight signal passing through the telescope main mirror 2, and reflects the light reflected from the light input end to the first through hole. After the design of the distance between the main and secondary mirrors is completed, the secondary mirror has a fine-tuning mechanism that can make small adjustments according to the different pointing heights. The fine-tuning mechanism is a conventional setting in this field and will not be described here.

[0027] The large field of view corrector 3 is located at the first through hole. The light reflected by the secondary mirror 1 is collected to the large field of view corrector 3. The large field of view corrector 3 is used to correct the aberration of the field of view. Usually, the starlight signal is coaxially arranged through the telescope primary mirror 2, the secondary mirror 1 and the large field of view corrector 3.

[0028] The plane reflector 5 is provided with a second through hole. The plane reflector 5 is located on the side of the large field of view corrector 3 away from the secondary mirror 1. Most of the light transmitted from the large field of view corrector 3 is reflected by the plane reflector 5 to the photometric system 4. Part of the light transmitted from the large field of view corrector 3 is transmitted to the relay system 6 through the second through hole. The second through hole is a small hole, and the diameter thereof can be designed by those skilled in the art according to the needs.

[0029] In some embodiments, during observation, the second through hole can transmit the light signal of a star in the field of view transmitted by the large field of view corrector 3 to the relay system 6. In some embodiments, the second through hole is coaxially arranged with the large field of view corrector 3. In some embodiments, the second through hole is located at the focal plane position of the light transmitted by the large field of view corrector 3, that is, the second through hole is located at the focal plane position of the front light collecting system.

[0030] The photometric system 4 is usually a multi-channel photometric system for large field of view observation. The photometric system 4 is located on one side of the plane reflector 5 and receives the light reflected by the reflector 5 .

[0031] The relay system 6 is located behind the plane reflector 5, and receives the light transmitted through the second through hole by the reflective large field of view corrector 3. Through the sub-band beam splitter of the relay system 6, the visible light part reaches the high dispersion spectrometer 8, and the near infrared part reaches the near infrared low dispersion spectrometer 7. The relay system 6 generally adopts the conventional configuration in this field, which will not be described in detail here.

[0032] The basic process of the optical path is that the starlight signal passes through the telescope primary mirror 2, secondary mirror 1, and large field of view corrector 3, and then the field of view is separated by the plane reflector 5. After part of the light signal (small field of view) enters the relay system 6, it reaches the high dispersion spectrometer 8 and the near-infrared low dispersion spectrometer 7 for spectral analysis, and part of the light signal is reflected to the photometry system for large field of view observation.

[0033] The present application uses a plane reflector with a second through hole to achieve field of view separation. The optical signal passing through the second through hole reaches the high-dispersion spectrometer and the near-infrared low-dispersion spectrometer respectively via the relay system, and the optical signal reflected by the plane mirror reaches the photometry system. The telescope photometry and spectrum measurement are achieved simultaneously. The present application adopts the front-end sharing of the light collecting system and the back-end splitting method to carry out the optical path fusion design. The plane reflector at the focal plane position of the light collecting system completes the field of view separation, and there is almost no light signal loss. Without the need for terminal switching, the problem that the same telescope cannot perform photometry and spectrum measurement at the same time is solved, which can greatly improve the observation efficiency and the utilization rate of the telescope. It also has the ability to respond quickly to fast-moving targets in the field of view, such as artificial satellites, space debris, asteroids, etc., that is, the advantage of the shared front-end field of view.

[0034] According to another aspect of the present application, the present application also provides an application of the above-mentioned synchronous large-field-of-view photometry and spectrometry terminal system in exoplanet detection or searching for artificial satellites and near-Earth space debris.

[0035] Taking the detection of exoplanets as an example, the candidate source of exoplanets passes through the telescope's primary mirror 2, secondary mirror 1, and large-field correction mirror 3 through the starlight signal, and enters the small hole of the plane reflector 5. After passing through the sub-band beam splitter of the relay system 6, the visible light part enters the high-dispersion spectrometer 8 for line-of-sight velocity measurement to authenticate the exoplanet; the near-infrared part enters the near-infrared low-dispersion spectrometer 7 to study the atmosphere of the exoplanet. The light signal reflected by the plane reflector 5 enters the large-field multi-channel photometry system, which performs time-series multi-color photometry observations on the targets in the field of view to search for candidate sources of exoplanets, greatly improving work efficiency.

[0036] For example, certain words are used in the specification and claims to refer to specific components or methods. Those skilled in the art should understand that different regions may use different nouns to refer to the same component. This specification and claims do not use differences in names as a way to distinguish components. For example, "including" mentioned throughout the specification and claims is an open term, so it should be interpreted as "including but not limited to". "Approximately" means that within an acceptable error range, those skilled in the art can solve the technical problem within a certain error range and basically achieve the technical effect. The subsequent description of the specification is a preferred embodiment of the present application, but the description is for the purpose of illustrating the general principles of the present application, and is not used to limit the scope of the present application. The scope of protection of the present application shall be determined by the attached claims.

[0037] It should also be noted that the terms "include", "comprises" or any other variations thereof are intended to cover non-exclusive inclusion, so that a product or system including a series of elements includes not only those elements, but also other elements not explicitly listed, or also includes elements inherent to such a product or system. In the absence of more restrictions, the elements defined by the sentence "comprises a ..." do not exclude the existence of other identical elements in the product or system including the elements.

[0038] The above description shows and describes several preferred embodiments of the invention, but as mentioned above, it should be understood that the invention is not limited to the form disclosed herein, and should not be regarded as excluding other embodiments, but can be used in various other combinations, modifications and environments, and can be modified within the scope of the invention concept described herein through the above teachings or the technology or knowledge of the relevant field. Changes and modifications made by those skilled in the art should be within the scope of protection of the claims attached to the invention without departing from the spirit and scope of the invention.

Claims

1. A synchronous large-field photometry and spectrum measurement terminal system, It is characterized in that include: The starlight signal passes through the telescope primary mirror, the front end of which is the light-incoming end and has a first through hole in the middle; The secondary mirror has a diameter smaller than that of the primary mirror of the telescope through which the starlight signal passes, is located before the light-incoming end of the primary mirror of the telescope, and reflects the light reflected from the light-incoming end to the first through hole; A large field correction lens, located in the first through hole, collects light reflected from the secondary mirror and is configured to correct the aberration of the field of view; A plane reflector, provided with a second through hole, located on a side of the large field of view corrector mirror away from the secondary mirror, and reflecting light transmitted from the large field of view corrector mirror; A photometric system, located on one side of the plane reflector, receiving the light reflected by the reflector; A relay system, located behind the plane reflector, receives the light transmitted by the reflective large field of view corrector through the second through hole; a near-infrared low-dispersion spectrometer configured to receive near-infrared light transmitted by the relay system; a high-dispersion spectrometer configured to receive visible light transmitted by the relay system; The starlight signal is coaxially arranged through the telescope primary mirror, secondary mirror and the large field correction mirror; The second through hole is coaxially arranged with the large field of view corrector lens; The second through hole is configured to transmit the optical signal of a star in the field of view transmitted by the large field of view corrector to the relay system; The second through hole is located at the focal plane of the light transmitted by the large field of view corrector; The diameter of the secondary mirror is larger than the diameter of the first through hole; The photometry system is a multi-channel photometry system.

2. Application of the synchronous large-field-of-view photometry and spectrometry terminal system as claimed in claim 1 in the detection of exoplanets or the search for artificial satellites and near-Earth space debris.

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