CN220871902U - Double-channel seamless spectrometer - Google Patents

Abstract

The utility model discloses a double-channel seamless spectrometer which comprises an incident diaphragm, a collimation unit, a dispersion unit, a first optical filter, an imaging unit, a first detector, a second optical filter, a spectrum unit and a second detector. Compared with the seamless spectrum equipment with the prism placed on the object side, the seamless spectrometer is in butt joint with the focal plane of the front-end telescope, is not limited by the manufacturing size of the prism, can be combined with optical telescopes with different calibers, and can observe darker targets; the object prism seamless spectrum device can only carry out spectrum observation, and the double-channel seamless spectrometer can simultaneously carry out imaging and spectrum observation; the imaging image and the spectrum image establish a data mapping relation, so that the scientific application can be enhanced. Compared with a seamless spectrometer with a grating placed at the image side, the imaging and spectrum image can be independently used or combined; the light energy utilization rate is higher, and the problem that light energy loss is generated by multiple diffraction orders is avoided; can reduce the problem of overlapping and polluting adjacent celestial body spectrums.

Description

Double-channel seamless spectrometer

Technical Field

The utility model belongs to the field of spectrometers, and particularly relates to a seamless spectrometer with double channels.

Background

Imaging observations and spectroscopic observations are two means of observation commonly used in astronomy.

Imaging observation refers to directly acquiring image information of a celestial body, and generally uses a telescope or a detector to observe the celestial body. Through imaging observation, information such as brightness, running track, surface activity and the like of the celestial body can be obtained, and the method is very important for researching the problems such as formation and evolution of the celestial body. For example, imaging observation of sun surface magnetic field activity, material projection and the like, research of formation and evolution of stars, and prediction of the influence of sun activity on the earth.

The spectrum observation is to measure and analyze the spectrum of the celestial radiation by using a spectrometer. In celestial physics, we study the physical properties of chemical composition, temperature, density, velocity, etc. by measuring the spectrum of celestial bodies. Unlike imaging observations, spectroscopic observations can provide more detailed physical information, for example, by measuring the red shift of the star system, the rate of expansion of the universe can be determined, and thus the problem of universe can be studied. In addition, the spectral observation can be used for detecting the information of the motion state, the rotation speed, the magnetic field and the like of the celestial body. For example, by measuring the spectrum of the sidereal, we can determine the information of its surface temperature, chemical composition, rotation speed and movement speed.

It should be noted that imaging observations and spectroscopic observations are not isolated observations and they can be combined with one another to provide more information. For example, when observing the star system, we can obtain the information of the shape, the size and the like of the star system through imaging observation, and can obtain the information of the composition, the speed field and the like of the star in the star system through spectrum observation, so that the evolution process of the star system can be better understood.

About 4000 hundred million stars exist in the Galois system, and astronomical observation is not purely directed to star observation in the Galois system (remote stars can be regarded as a point source celestial body), but also extended celestial bodies such as a star cloud, a star group, a star system and the like (the extended celestial bodies have a certain scale in the field of view space direction). If the extended celestial body is still observed as a point source celestial body, only the extended celestial body can be researched as a whole. With the intensive research, we want to know the internal properties of the star, we need to obtain the spectral information λ of the different positions (X, Y) of the extended celestial body. The spectral information at these different positions constitutes a three-dimensional data structure, two-dimensional (X, Y) spatial information and one-dimensional spectral information. The spectrum image acquisition generally uses a two-dimensional area array detector, and three-dimensional spectrum information is required to be represented by a two-dimensional image.

The imaging observation method comprises a polychromatic imaging method and a Fabry-Perot scanning imaging method, wherein the polychromatic imaging method can be used for changing narrow-band optical filters with different wave bands, taking a picture every time the optical filters are changed, and combining the pictures with different wave bands can be used for forming three-dimensional spectrum data. The Fabry-Perot scanning imaging method utilizes two parallel flat plates to carry out multi-beam interference, light is folded back between the flat plates to improve the fineness of wave bands, and the scanning mode is to switch different wave bands by changing the space between F-P interference cavities. Their common disadvantages are large workload, low time resolution, limited observation wavelength, discontinuous spectrum.

Common three-dimensional spectroscopic methods are long-slit scanning spectroscopy, seamless spectroscopy, fourier transform spectroscopy, and integral field-of-view spectroscopy. Long slit scanning spectrum can only be realized by moving a slit to expose different places of the same star system for multiple times by relying on a long slit spectrometer, and the time efficiency is low. The Fourier transform spectroscopy is to translate a scanning mirror to obtain a two-dimensional interference image, and analyze spectral information of different spatial positions by utilizing Fourier transform. The contrast of the stripes is ensured by long-time exposure, the scanning mode has high requirements on the precision and stability of the spectrometer, and the time resolution is reduced. The integral view field spectroscopy cuts and expands the celestial body image, the images are arranged in a row along the length direction of the slit, and the simultaneous acquisition of the three-dimensional data cube (x, y; lambda) of the two-dimensional observation target can be realized through one exposure.

Different from the three-dimensional spectrum observation aiming at a single extended celestial body, the seamless spectrum observation can be used for simultaneously observing celestial bodies in a certain space area, and the acquisition of the position and low-resolution spectrum information of the celestial bodies is an important means for the observation in the sky. The seamless spectrometer has various realization methods, and can be used for placing a dispersion prism at the object side of a telescopic system and placing a grating or a dispersion prism at the image side of the telescopic system. Currently, a seamless spectrometer mainly provides a dispersion function by a blazed grating, and a zero-order image and a low-resolution spectrum of each celestial body in a two-dimensional view field are directly obtained without a slit. The spectrums of +/-1 st and +/-2 nd are divided into two sides of the zero-order image according to the principle of diffraction dispersion. Wherein the zero-order image is used to provide information such as spatial position, calibration reference, etc. The spectral resolution depends on the grating dispersive power and the atmospheric apparent power due to the absence of slits. Even if a light filter is added in the spectrometer to control the spectrum wavelength range, the overlapping pollution of a plurality of secondary spectrums (+ -1 level, +/-2 level, etc.) of adjacent celestial bodies in the dispersion direction can not be avoided, and the scientific utility is reduced. On the other hand, the blazed grating is used as a main dispersion element, dispersion is generated by means of light diffraction, light energy is mainly concentrated on blazed orders, other orders of spectrums can obtain light energy with different proportions, light energy loss is caused, and the light energy is overlapped with other spectrums to pollute the light.

Disclosure of utility model

Aiming at the problems existing in the prior art, the utility model provides a double-channel seamless spectrometer.

In order to achieve the above purpose, the present utility model provides the following technical solutions:

The utility model provides a binary channels seamless spectrum appearance, includes incident diaphragm, collimation unit, dispersion unit, light filter first, imaging unit, detector first, light filter second, spectrum unit, detector second, detector first sets up on imaging unit's focal plane, detector second sets up on spectrum unit's focal plane, dispersion unit comprises 1 at least triangular prism, and when the triangular prism had the polylith, polylith triangular prism was placed according to contained angle theta in proper order, and plated the beam splitting membrane on first optical surface of first triangular prism for the beam splitting, other triangular prism is used for the dispersion, and the light beam is through incident diaphragm and collimation unit the dispersion unit divide into two bundles, and one of them is restrainted through light filter first, imaging unit, detector first, and another one is restrainted through light filter second, spectrum unit, detector second, entering spectrum passageway.

Furthermore, a reference plate is arranged at the incidence diaphragm, and a reference light source is arranged in front of the incidence diaphragm.

Further, the reference light source is a highly monochromatic light source or a wavelength-scaled light source or a celestial light beam of known characteristic spectrum.

Further, the light beam passes through the light splitting film on the first optical surface of the first triangular prism, the reflected light beam enters the imaging channel, and the transmitted light beam enters the spectrum channel.

Further, the light splitting film is a neutral density light splitting film or a polarization light splitting film or a dichromatic light splitting film.

Further, the first filter and the second filter are single filter components or filter wheels consisting of a plurality of filters.

Further, the reference plate is made by arranging a two-dimensional array of transmissive pinholes on an opaque substrate, the pinholes having a diameter of 10 microns to 200 microns.

Furthermore, the incident diaphragm is an object plane or an image plane, and is in conjugate relation with the first detector and the second detector.

Further, the second optical surface of the first triangular prism, the first optical surfaces and the second optical surfaces of the other triangular prisms are all plated with an antireflection film.

Further, the first optical filter is arranged between the dispersion unit and the imaging unit, or inside the imaging unit, or between the imaging unit and the first detector; the second optical filter is arranged between the dispersion unit and the spectrum unit, or inside the spectrum unit, or between the spectrum unit and the second detector.

Compared with the prior art, the utility model has the beneficial effects that:

Compared with a seamless spectrum device with a prism placed on the object side, the technical advantages are that:

(1) The seamless spectrometer is in butt joint with the focal plane of the front-end telescope, is not limited by the manufacturing size of the prism, and can be combined with optical telescopes with different calibers to observe darker targets.

(2) The object prism seamless spectrum device can only conduct spectrum observation, and the double-channel seamless spectrometer can conduct imaging and spectrum observation at the same time.

(3) The imaging image and the spectrum image establish a data mapping relation, so that the scientific application can be enhanced.

Compared with a seamless spectrometer with a grating placed in an image space, the method has the technical advantages that:

(1) The imaging and the spectrum image can be used independently or in combination;

(2) The light energy utilization rate is higher, and the problem that light energy loss is generated by multiple diffraction orders is avoided;

(3) Each celestial body only generates one spectrum, so that the problem of mutual overlapping pollution of adjacent celestial body spectrums is reduced.

Drawings

FIG. 1 is a schematic diagram of the operation of a two-channel seamless spectrometer;

FIG. 2 is a schematic diagram of the operation structure of a dispersion unit prism;

FIG. 3 is a top view of a first triangular prism of a dispersive unit;

FIG. 4 is a top view of a dispersion unit consisting of n dispersion prisms;

FIG. 5 is a schematic diagram of imaging and spectral data mapping;

FIG. 6 is a schematic diagram of one-dimensional spectral data obtained using a spectral extraction method.

The marks in the figure: 1-incident diaphragm, 2-collimation unit, 3-dispersion unit, 3-1-triangular prism one, 3-1-1-triangular prism one first optical surface, 3-1-2-triangular prism one second optical surface, 3-2-triangular prism two, 3-2-1-triangular prism two first optical surface, 3-2-2-triangular prism two second optical surface, 3-n-triangular prism n, 4-optical filter one, 5-imaging unit, 6-detector one, 7-optical filter two, 8-spectrum unit, 9-detector two, 10-reference plate, 11-reference light source, 12-imaging image, 13-spectral image.

Detailed Description

The utility model is described in further detail below with reference to the accompanying drawings.

The prism can meet the requirement of low-resolution dispersion as an important dispersion element, and has the technical advantages of no secondary spectrum mutual pollution and diffraction light energy loss. The embodiment provides a novel seamless spectrometer by means of the dispersion prism, the celestial body position and spectrum information in a certain view field can be obtained through single exposure, the problems of mutual pollution, light energy loss and the like of celestial body spectrums caused by multi-level diffraction existing in the grating type seamless spectrometer are solved, imaging and spectrum images can be mutually independent and can be mapped, and therefore the scientific effect of observation of seamless spectrums on patrol days is improved.

Definition of the direction: the direction of the optical axis of the incident light beam is Z; the space direction is X, and is perpendicular to the optical axis direction Z, and the X-Z plane is a sagittal plane of light beam propagation; the dispersion direction is Y, which is perpendicular to the space direction X and the optical axis direction Z, and the Y-Z plane is the meridian plane of light beam propagation.

The dual-channel seamless spectrometer comprises an incident diaphragm 1, a collimation unit 2, a dispersion unit 3, a first optical filter 4, an imaging unit 5, a first detector 6, a second optical filter 7, a spectrum unit 8, a second detector 9, a reference plate 10 and a reference light source 11, and is shown in the attached figure 1.

The dual-channel seamless spectrometer is provided with two channels of imaging and spectrum, and simultaneously shooting is carried out to respectively obtain imaging and spectrum images. And obtaining space and brightness information of different celestial bodies in the observation field by using the imaging image, and obtaining spectrum information of different celestial bodies in a certain wave band by using the spectrum image, wherein the spectrum resolution is less than or equal to 1000.

The dual-channel seamless spectrometer has three working modes: observation mode, scaling mode, and mapping mode.

The observation mode can be used for shooting imaging images and spectrum images of different celestial bodies in an observation field, and space, brightness and spectrum information of the different celestial bodies can be measured from the imaging images and the spectrum images, and the space, the brightness and the spectrum information of the different celestial bodies are shown in the figure 1. Converging light beams in an observation view field are incident and imaged on an incident diaphragm 1, collimated by a collimation unit 2, parallel light beams are incident into a dispersion unit 3, the light splitting is carried out by utilizing a light splitting surface of a triangular prism I3-1 in the dispersion unit 3, reflected light beams enter an imaging channel, and transmitted light beams are refracted and dispersed to enter a spectrum channel. In the imaging channel, the reflected light beam passes through the first optical filter 4, only the light beam with a required wave band is observed to pass through, the reflected light beam enters the imaging unit 5 to perform convergent imaging, and finally the first detector 6 acquires an imaging image 12. The transmitted light beam enters a spectrum channel through the refraction dispersion of a triangular prism I3-1 and a triangular prism II 3-2 of a dispersion unit 3, the dispersed light beam passes through a filter II 7, only the light beam with a required observation wave band passes through, enters a spectrum unit 8 for convergence imaging, and finally a spectrum image 13 is acquired by a detector II 9.

The calibration mode refers to that the spectrum channel is independently used to complete the wavelength calibration of the spectrum, and the imaging channel can not participate, as shown in fig. 6. The reference plate 10 is placed at the incidence diaphragm 1, the reference light source 11 emits convergent light beams to irradiate the reference plate 10, the reference light beams pass through a pinhole array on the reference plate 10, are collimated by the collimating unit 2, the parallel light beams are injected into the dispersing unit 3, the light splitting is carried out by utilizing the light splitting surface of the triangular prism one 3-1 in the dispersing unit 3, the reflected light beams enter the imaging channel, and the refraction and dispersion of the transmitted light beams enter the spectrum channel. The transmitted light beam enters a spectrum channel through the refraction dispersion of a triangular prism I3-1 and a triangular prism II 3-2 of a dispersion unit 3, the dispersed light beam passes through a filter II 7, only the light beam with a required observation wave band passes through, enters a spectrum unit 8 for convergence imaging, and finally a spectrum image 13 is acquired by a detector II 9. And obtaining one-dimensional spectrum data by using a spectrum extraction method, and solving the corresponding relation between the wavelength of the one-dimensional spectrum data and the pixel by comparing the known wavelength data of the reference light source 11.

The mapping mode is shown in fig. 5, the reference plate 10 is placed at the incident diaphragm 1, the reference light source 11 emits a converging light beam, the reference plate 10 is irradiated, the reference light beam passes through the pinhole array on the reference plate 10, the collimation unit 2 is used for collimation, the parallel light beam is injected into the dispersion unit 3, the light splitting is carried out by utilizing the light splitting surface of the triangular prism one 3-1 in the dispersion unit 3, the reflected light beam enters the imaging channel, and the refraction and dispersion of the transmitted light beam enter the spectrum channel. In the imaging channel, the reflected light beam passes through the first optical filter 4, only the light beam with a required wave band is observed to pass through, the reflected light beam enters the imaging unit 5 to perform convergent imaging, and finally the first detector 6 acquires an imaging image 12. The transmitted light beam enters a spectrum channel through the refraction dispersion of a triangular prism I3-1 and an angular prism II 3-2 of a dispersion unit 3, the dispersed light beam passes through a filter II 7, only the light beam with a required observation wave band passes through, enters a spectrum unit 8 for convergence imaging, and finally a spectrum image 13 is acquired by a detector II 9. The relative position of the pinhole on the reference plate 10 (δx ₀,δY₀) is used as a reference, and the relative position of the pinhole on the imaging image 12 (δx ₁,δY₁) and the relative position of the characteristic spectral line on the spectral image 13 (δx ₂,δY₂) are used to establish a data mapping relationship for resolving the spatial, brightness and spectral information of any position (X, Y) within the observation field of view.

The imaging and spectrum channels are exposed simultaneously, and celestial body image spots in the imaging image and celestial body spectrums in the spectrum image have a one-to-one mapping relation. The working principle of the dual-channel seamless spectrometer comprises a corresponding dual-channel data mapping method. At the entrance stop, a reference plate of a two-dimensional pinhole array is placed, namely: the relative positional relationship (delta X ₀,δY₀) of each pinhole in the reference plate is calibrated, and the pinholes on the reference plate form a conjugate relationship with the focal plane of the dual channels. The reference plate is illuminated with a reference light source, which passes through pinholes distributed in a two-dimensional array and enters the spectrometer. And the imaging and the spectrum channel are simultaneously exposed to obtain an imaging image and a spectrum image of the two-dimensional pinhole array. The calibrated relative position (delta X ₀,δY₀) of the pinholes on the reference plate is taken as a reference, and the relative position (delta X ₁,δY₁) of the pinholes on the imaging image and the relative position (delta X ₂,δY₂) of characteristic spectral lines on the spectral image are utilized to establish a data mapping relationship, as shown in figure 5. For different observations, imaging and spectrum data of each celestial body are extracted from the observation data by using the mapping relation and are used for scientific research.

The entrance diaphragm: the aperture is generally square in shape, or may be circular or other polygonal, and the light beam transmitted through the aperture is an effective light beam, and the light beam absorbed or emitted by a structure other than the aperture is an ineffective light beam. The incident diaphragm 1 is an object plane or an image plane, and is in conjugate relation with the first detector 6 and the second detector 9.

The collimation unit: can be composed of a transmission type, reflection type or foldback type optical system to provide the light beam collimation function. The incident light beam passing through the incident diaphragm 1 passes through the collimator unit 2 to become a parallel light beam.

The dispersion unit: the dispersion unit is a core component of the dual-channel seamless spectrometer and provides the functions of light splitting and dispersion. Light splitting function: the beam is split into two beams that enter the imaging and spectral channels, respectively. Dispersion function: within the spectral channels, the chromatic dispersion phenomenon of triangular prisms is exploited to provide the required spectral resolution. As shown in fig. 4, the three-dimensional prism comprises at least 1 triangular prism which is arranged in sequence according to an included angle theta. The first optical surface of the first triangular prism (i.e., triangular prism 3-1) provides a light splitting function, and the remaining triangular prisms provide a dispersion function. The triangular prisms (triangular prism one 3-1, triangular prism two 3-2 … triangular prism n3-n, in this embodiment, n.ltoreq.5) are made of high dispersion glass material with low abbe coefficient, and the dispersion phenomenon is generated by utilizing the law that the refractive index of the material changes with the wavelength. In this embodiment, a dispersion unit 3 composed of two triangular prisms (triangular prism one 3-1 and triangular prism two 3-2) is taken as an example for detailed description, as shown in fig. 2. The optical performance of the triangular prism is determined by three parameters of an incident angle alpha, a material refractive index n and a vertex angle A, as shown in figure 3. The lower the abbe number, the higher the dispersion intensity of the dispersion unit 3, and the higher the spectral resolution of the two-channel seamless spectrometer, using a glass material. The larger the apex angle A of the triangular prism is, the larger the dispersion strength of the dispersion unit 3 is, and the higher the spectral resolution of the dual-channel seamless spectrometer is. The more triangular prisms used, the greater the dispersion strength of the dispersive unit 3, and the higher the spectral resolution of the two-channel seamless spectrometer. The first triangular prism 3-1 and the second triangular prism 3-2 are arranged in an X-Y plane, the normal line of the first optical surface 3-1-1 of the first triangular prism and the incident optical axis form an angle alpha ₁, and the second optical surface 3-1-2 of the first triangular prism and the first optical surface 3-2-1 of the second triangular prism form an angle theta. The angle of incidence α ₁ of triangular prism one 3-1 within the operating band is determined by the minimum deflection angle β of triangular prism one 3-1, and the angle θ is defined as the sum of the angles of incidence (α ₁+α₂) of two adjacent triangular prisms.

The first optical surface 3-1-1 of the triangular prism I is an incident surface of the dispersion unit 3, an incident light beam enters the first optical surface 3-1-1 of the triangular prism I at an incident angle alpha ₁, the first optical surface 3-1-1 of the triangular prism I is plated with an optical light-splitting film, and the light-splitting film can reflect a part of light in proportion and transmit another part of light. The second optical surface 3-1-2 of the triangular prism I, the first optical surface 3-2-1 of the triangular prism II and the second optical surface 3-2-2 of the triangular prism II are plated with antireflection films. The light beam reflected by the first optical surface 3-1-1 of the triangular prism I enters an imaging channel, and an imaging image is acquired to obtain space position and brightness information of a celestial body in an observation field. The light beam transmitted through the first optical surface 3-1-1 of the triangular prism I is refracted through the triangular prism I3-1 and the triangular prism II 3-2, the light beam is dispersed and enters a spectrum channel, a spectrum image is acquired, and celestial body spectrum information in an observation field is obtained.

The first optical surface 3-1-1 of the triangular prism one is a light splitting film: the optical splitting film on the first optical surface 3-1-1 of the triangular prism I is generally a neutral density splitting film, and the reflected light and the transmitted light distribute light energy in proportion, so that the optical splitting film has the same polarization state and wave band range. The optical splitting film on the first optical surface 3-1-1 of the triangular prism one may be a polarizing splitting film, the polarization states of the reflected light and the transmitted light are in an orthogonal relationship, and the light energy of the reflected light and the transmitted light is determined by the polarization states of the incident light beam, so that the optical splitting film has the same band range. The optical splitting film on the first optical surface 3-1-1 of the triangular prism one may also be a dichroic splitting film, and the difference between the operating band of the reflected light and the transmitted light is determined by the dichroic splitting film.

The first filter and the second filter: the first filter 4 and the second filter 7 provide a limited range of working wave bands, intercept the light beams of non-working wave bands and avoid the problem of mutual overlapping pollution caused by redundant spectrums. The first filter 4 and the second filter 7 can be single filter components, or filter wheels consisting of a plurality of filters, and different filters can be switched according to scientific research requirements. The first filter 4 is placed between the dispersing unit 3 and the imaging unit 5, can be placed inside the imaging unit 5, and can be placed between the imaging unit 5 and the first detector 6. The second filter 7 is placed between the dispersive unit 3 and the spectroscopic unit 8, or inside the spectroscopic unit 8, or between the spectroscopic unit 8 and the second detector 9.

The imaging unit: the beam converging function may be provided by a transmissive, reflective or refractive optical system. The imaging light beams reflected by the dispersion unit 3 are focused on a focal plane through the imaging unit 5, and the image spots of all celestial bodies in the observation field are obtained.

The spectrum unit 8: the beam converging function may be provided by a transmissive, reflective or refractive optical system. The dispersive light beam transmitted by the dispersive unit 3 is focused on a focal plane through the spectrum unit 8, and a dispersive spectrum of each celestial body in the observation field is obtained.

The first detector and the second detector are as follows: are placed on the focal planes of the imaging unit 5 and the spectroscopic unit 8, respectively, for acquiring imaging and spectroscopic images. The photoelectric detector can be various linear arrays or area arrays, and is mainly a CCD or CMOS area array detector.

The reference plate: the opaque substrate is provided with a two-dimensional array of transmissive pinholes, typically selected in the range of 10 to 200 microns in diameter, through which an incident light beam may pass into the collimating unit 2.

The reference light source: the types of reference light sources required to provide the mapping pattern may be high monochromaticity light sources, wavelength scaled light sources, celestial light beams of known characteristic spectra. The high monochromaticity light source is used as a reference light source 11, a spectrum channel generates a monochromatic image of a pinhole array, each pinhole corresponds to one monochromatic image and is similar to the image pattern of an imaging channel, the relative positions of different monochromatic images are measured, and the mapping relation between imaging and spectrum images is solved. The wavelength calibration light source is taken as a reference light source 11, the spectrum channel generates a calibration spectrum image of the pinhole array, each pinhole corresponds to one calibration spectrum, the calibration spectrum has characteristic emission or absorption spectral lines, the relative positions of different pinholes corresponding to the same characteristic spectral line are measured, and the mapping relation between imaging and spectrum image is solved. The celestial body light beam with known characteristic spectrum is taken as a reference light source 11, such as sunlight, a spectrum channel generates celestial body spectrum images penetrating through a pinhole array, each pinhole corresponds to one celestial body spectrum, the celestial body spectrum has known characteristic absorption or emission spectral lines, the relative positions of different pinholes corresponding to the same characteristic spectral line are measured, and the mapping relation between imaging and spectrum images is solved.

The imaging and spectrum channels are simultaneously exposed to obtain imaging and spectrum images respectively, and the method has the advantages of high time resolution and high observation efficiency. The imaging image only comprises celestial space position and brightness information in the observation field of view, and can be independently used as imaging or photometry observation, so that the problem of spectrum pollution is avoided. In the spectrum image, each celestial body only has one spectrum covering a specified wave band, so that the problem of loss caused by that the light energy of a part occupied by the non-blazed level of the multi-level spectrum is polluted mutually is avoided.

The above description is only of the preferred embodiments of the present utility model, and is not intended to limit the present utility model. Any modification, equivalent replacement, improvement, etc. made within the spirit and principle of the present utility model should be included in the protection scope of the present utility model.

Claims (10)

1. The utility model provides a binary channels seamless spectrum appearance, its characterized in that includes incident diaphragm, collimation unit, dispersion unit, light filter one, imaging unit, detector one, light filter two, spectrum unit, detector two, detector one sets up on imaging unit's focal plane, detector two sets up on spectrum unit's focal plane, dispersion unit comprises 1 at least triangular prism, and when the triangular prism had the polylith, polylith triangular prism was placed according to contained angle theta in proper order, and plated the beam splitting membrane on the first optical surface of third triangular prism for the beam splitting, other triangular prism is used for the dispersion, and the light beam is through incident diaphragm and collimation unit the dispersion unit divide into two bundles, and one of them is through light filter one, imaging unit, detector one gets into imaging channel, another one is through light filter two, spectrum unit, detector two, entering spectrum channel.

2. The dual channel seamless spectrometer according to claim 1, wherein a reference plate is disposed at the entrance stop, and a reference light source is disposed in front of the entrance stop.

3. A dual channel seamless spectrometer according to claim 2, in which the reference light source is a highly monochromatic light source or a wavelength-scaled light source or a celestial light beam of known characteristic spectrum.

4. The dual channel seamless spectrometer according to claim 1, wherein the light beam passes through a beam splitting film on the first optical surface of the first triangular prism, reflects the light beam into the imaging channel, and transmits the light beam into the spectral channel.

5. The dual channel seamless spectrometer according to claim 1, wherein the light splitting film is a neutral density light splitting film or a polarizing light splitting film or a dichroic light splitting film.

6. The dual channel seamless spectrometer according to claim 1, wherein the first filter and the second filter are a single filter assembly or a filter wheel comprising a plurality of filters.

7. The dual channel seamless spectrometer according to claim 2, wherein the reference plate is made by arranging a two-dimensional array of transmissive pinholes on an opaque substrate, the pinholes having a diameter of 10 microns to 200 microns.

8. The dual-channel seamless spectrometer according to claim 1, wherein the incident diaphragm is an object plane or an image plane, and is in an object-image conjugate relationship with the first detector and the second detector.

9. The dual channel seamless spectrometer according to claim 1, wherein the second optical surface of the first triangular prism, the first optical surfaces of the remaining triangular prisms, and the second optical surfaces are coated with an anti-reflection film.

10. The dual-channel seamless spectrometer according to claim 1, wherein the first filter is disposed between the dispersive unit and the imaging unit, or disposed inside the imaging unit, or disposed between the imaging unit and the first detector; the second optical filter is arranged between the dispersion unit and the spectrum unit, or inside the spectrum unit, or between the spectrum unit and the second detector.