CN220871902U - A dual-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

A dual-channel seamless spectrometer

Technical Field

The utility model belongs to the field of spectrometers, and in particular relates to a seamless spectrometer with dual channels.

Background technique

Imaging observation and spectral observation are two commonly used observation methods in astronomy.

Imaging observation refers to directly obtaining image information of celestial bodies, generally using telescopes or detectors to observe celestial bodies. Through imaging observation, we can obtain information such as the brightness, trajectory, and surface activity of celestial bodies, which is very important for studying the formation and evolution of celestial bodies. For example, imaging observations of magnetic field activity and material ejection on the surface of the sun can be used to study the formation and evolution of stars and predict the impact of solar activity on the earth.

Spectroscopic observation uses a spectrometer to measure and analyze the spectrum of celestial radiation. In astrophysics, we measure the spectrum of celestial bodies to study their chemical composition, temperature, density, speed and other physical properties. Unlike imaging observations, spectral observations can provide more detailed physical information. For example, by measuring the redshift of galaxies, the expansion rate of the universe can be determined, thereby studying cosmological issues. In addition, spectral observations can also be used to detect the motion state, rotation speed, magnetic field and other information of celestial bodies. For example, by measuring the spectrum of a star, we can determine its surface temperature, chemical composition, rotation speed and movement speed.

It should be noted that imaging observation and spectral observation are not isolated observation methods. They can be combined with each other to provide more abundant information. For example, when observing galaxies, we can obtain information such as the galaxy's shape and size through imaging observation, and obtain information such as the composition and velocity field of stars in the galaxy through spectral observation, so as to better understand the evolution of galaxies.

There are about 400 billion stars in the Milky Way. Astronomical observations are not just for stars in the Milky Way (distant stars can be regarded as point source objects), but also for extended objects such as nebulae, star clusters, and galaxies (extended objects have a certain scale in the spatial direction of the field of view). If we still observe extended objects as point source objects, we can only study the extended objects as a whole. As the research deepens, in order to understand the properties inside the galaxy, we need to obtain the spectral information λ at different positions (X, Y) of the extended objects. The spectral information at these different positions constitutes a three-dimensional data structure, two-dimensional (X, Y) spatial information and one-dimensional spectral information. Spectral image acquisition generally uses a two-dimensional array detector, and a two-dimensional image must be used to represent the three-dimensional spectral information.

Imaging observation methods include multicolor imaging and Fabry-Perot scanning imaging. The multicolor imaging method replaces narrowband filters of different bands, takes a picture each time the filter is replaced, and combines the pictures of different bands to form three-dimensional spectral data. The Fabry-Perot scanning imaging method uses two parallel plates to perform multi-beam interference, and the light is reflected between the plates to improve the fineness of the band. The scanning method switches different bands by changing the distance between the F-P interference cavities. Their common disadvantages are large workload, low time resolution, limited observation wavelength, and non-continuous spectrum.

Common three-dimensional spectral observation methods include long-slit scanning spectroscopy, seamless spectroscopy, Fourier transform spectroscopy, and integral field spectroscopy. Long-slit scanning spectroscopy can only be achieved by relying on a long-slit spectrometer to move the slit multiple times to expose different places in the same galaxy, which is very time-inefficient. Fourier transform spectroscopy is to obtain a two-dimensional interference image by translating the scanning mirror, and use Fourier transform to analyze the spectral information of different spatial positions. Long exposure is required to ensure the contrast of the fringes. The scanning method has high requirements on the accuracy and stability of the spectrometer, which reduces the time resolution. Integral field spectroscopy cuts and expands the celestial image, arranging the image in a row along the length of the slit. Through a single exposure, the three-dimensional data cube (x, y; λ) of the two-dimensional observation target can be collected simultaneously.

Different from the above-mentioned three-dimensional spectral observation of a single extended celestial body, seamless spectral observation can simultaneously observe celestial bodies in a certain sky area, obtain their positions and low-resolution spectral information, and is an important means of sky survey observation. There are various ways to implement seamless spectrometers. A dispersion prism can be placed on the object side of the telescope system, or a grating or dispersion prism can be placed on the image side of the telescope system. At present, seamless spectrometers are mainly provided with dispersion function by blazed gratings. No slits are set, and the zero-order image and low-resolution spectrum of each celestial body in the two-dimensional field of view are directly obtained. ±1-level, ±2-level and other spectra are arranged on both sides of the zero-order image according to the principle of diffraction dispersion. Among them, the zero-order image is used to provide information such as spatial position and calibration reference. Since there is no slit, the spectral resolution depends on the grating dispersion ability and the atmospheric seeing. Even if a filter is added to the spectrometer to control the spectral wavelength range, it is still impossible to avoid the overlapping and contamination of multiple order spectra (±1-level, ±2-level, etc.) of adjacent celestial bodies in the dispersion direction, which reduces the scientific utility. On the other hand, when the blazed grating is used as the main dispersion element, dispersion is produced by relying on the diffraction of light. The light energy is mainly concentrated on the blazed order. Other order spectra will also obtain different proportions of light energy, resulting in light energy loss and overlapping and contamination with other spectra.

Utility Model Content

In view of the above problems existing in the prior art, the utility model provides a dual-channel seamless spectrometer.

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

A dual-channel seamless spectrometer comprises an incident aperture, a collimation unit, a dispersion unit, a first filter, an imaging unit, a first detector, a second filter, a spectrum unit and a second detector. The first detector is arranged on the focal plane of the imaging unit, and the second detector is arranged on the focal plane of the spectrum unit. The dispersion unit is composed of at least one triangular prism. When there are multiple triangular prisms, the multiple triangular prisms are arranged in sequence according to an angle θ, and a spectroscopic film is coated on the first optical surface of the first triangular prism for light splitting. The remaining triangular prisms are used for dispersion. A light beam passes through the incident aperture and the collimation unit and is divided into two beams in the dispersion unit. One beam passes through the first filter, the imaging unit and the first detector to enter the imaging channel, and the other beam passes through the second filter, the spectrum unit and the second detector to enter the spectrum channel.

Furthermore, a reference plate is provided at the entrance aperture, and a reference light source is provided in front of the entrance aperture.

Furthermore, the reference light source is a high monochromaticity light source or a wavelength calibration light source or a celestial beam with a known characteristic spectrum.

Furthermore, the light beam passes through the beam splitter 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 spectral channel.

Furthermore, the beam splitter film is a neutral density beam splitter film, a polarization beam splitter film, or a dichroic beam splitter film.

Furthermore, the optical filter 1 and the optical filter 2 are a single optical filter assembly or a filter wheel composed of multiple optical filters.

Furthermore, the reference plate is made by arranging a two-dimensional array of transmission pinholes on an opaque substrate, and the pinhole diameter is 10 microns to 200 microns.

Furthermore, the incident aperture is an object plane or an image plane, and is in an object-image conjugate relationship with the first detector and the second detector.

Furthermore, the second optical surface of the first triangular prism, and the first optical surfaces and second optical surfaces of the remaining triangular prisms are all coated with anti-reflection films.

Furthermore, the filter 1 is arranged between the dispersion unit and the imaging unit, or is arranged inside the imaging unit, or is arranged between the imaging unit and the detector 1; the filter 2 is arranged between the dispersion unit and the spectral unit, or is arranged inside the spectral unit, or is arranged between the spectral unit and the detector 2.

Compared with the prior art, the beneficial effects of the utility model are:

Compared with seamless spectrum equipment with prisms placed on the object side, the technical advantages are:

(1) The seamless spectrometer of the utility model is connected to the focal plane of the front telescope and is not limited by the manufacturing size of the prism. It can be combined with optical telescopes of different calibers to observe darker targets.

(2) The objective prism seamless spectrometer can only perform spectral observation, while the dual-channel seamless spectrometer can perform imaging and spectral observation at the same time.

(3) Establishing a data mapping relationship between imaging images and spectral images can enhance scientific use.

Compared with seamless spectrometers with gratings placed on the image side, the technical advantages are:

(1) Imaging and spectral imaging can be used independently or in combination;

(2) It has a higher light energy utilization rate and does not cause the problem of light energy loss caused by multiple diffraction orders;

(3) Each celestial body produces only one spectrum, which reduces the problem of overlapping and contamination between the spectra of adjacent celestial bodies.

BRIEF DESCRIPTION OF THE DRAWINGS

Fig. 1 is a working principle diagram of a dual-channel seamless spectrometer;

FIG2 is a schematic diagram of the working structure of the dispersion unit prism;

FIG3 is a top view of a dispersion unit triangular prism 1;

FIG4 is a top view of a dispersion unit composed of n dispersion prisms;

FIG5 is a schematic diagram of the relationship between imaging and spectral data mapping;

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

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

Detailed ways

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

As an important dispersion element, the prism can meet the requirements of low-resolution dispersion and has the technical advantages of no mutual contamination of sub-spectra and loss of diffraction light energy. This embodiment provides a new seamless spectrometer based on the dispersion prism, which can obtain the position and spectrum information of celestial bodies within a certain field of view with a single exposure, and solves the problems of mutual contamination of celestial spectra and loss of light energy caused by multi-order diffraction in grating-type seamless spectrometers. The imaging and spectral images are both independent of each other and can be mapped to each other, thereby enhancing the scientific role of seamless spectral survey observations.

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

The dual-channel seamless spectrometer includes an incident aperture 1, a collimation unit 2, a dispersion unit 3, a filter 1 4, an imaging unit 5, a detector 1 6, a filter 2 7, a spectral unit 8, a detector 2 9, a reference plate 10 and a reference light source 11, see Figure 1.

The dual-channel seamless spectrometer has two channels, imaging and spectrum, which are shot simultaneously to obtain imaging and spectrum images respectively. The imaging image is used to obtain the spatial and brightness information of different celestial bodies in the observation field, and the spectrum image is used to obtain the spectrum information of different celestial bodies in a certain band in the observation field. The spectral resolution is less than or equal to 1000.

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

The observation mode can take imaging images and spectral images of different celestial bodies in the observation field, from which the space, brightness and spectral information of different celestial bodies can be measured, as shown in Figure 1. The convergent light beam in the observation field is incident, imaged on the incident aperture 1, collimated by the collimation unit 2, and the parallel light beam is incident on the dispersion unit 3, and the light is split by the splitting surface of the triangular prism 1 3-1 in the dispersion unit 3. The reflected light beam enters the imaging channel, and the transmitted light beam is refracted and dispersed into the spectral channel. In the imaging channel, the reflected light beam passes through the filter 1 4, and only the light beam of the required wavelength band is observed to pass through, and enters the imaging unit 5 for convergence imaging, and finally the imaging image 12 is collected by the detector 1 6. The transmitted light beam enters the spectral channel through the refraction and dispersion of the triangular prism 1 3-1 and the triangular prism 2 3-2 of the dispersion unit 3, and the dispersed light beam passes through the filter 2 7, and only the light beam of the required wavelength band is observed to pass through, and enters the spectral unit 8 for convergence imaging, and finally the spectral image 13 is collected by the detector 2 9.

The calibration mode refers to the wavelength calibration of the spectrum using the spectral channel independently, and the imaging channel may not be involved, as shown in Figure 6. The reference plate 10 is placed at the incident aperture 1, and the reference light source 11 emits a convergent beam to illuminate the reference plate 10. The reference beam passes through the pinhole array on the reference plate 10, is collimated by the collimation unit 2, and the parallel beam enters the dispersion unit 3. The beam is split by the splitting surface of the triangular prism 1 3-1 in the dispersion unit 3, and the reflected beam enters the imaging channel. The transmitted beam is refracted and dispersed into the spectral channel. The transmitted beam enters the spectral channel through the refraction and dispersion of the triangular prism 1 3-1 and the triangular prism 2 3-2 of the dispersion unit 3. The dispersed beam passes through the filter 2 7, and only the beam of the required wavelength band is observed to pass through, and enters the spectral unit 8 for convergence imaging. Finally, the detector 2 9 collects the spectral image 13. The one-dimensional spectral data is obtained by using the spectrum extraction method, and the wavelength and pixel correspondence of the one-dimensional spectral data are solved by comparing with the known wavelength data of the reference light source 11.

The mapping mode is shown in FIG5. The reference plate 10 is placed at the incident aperture 1. The reference light source 11 emits a convergent beam to illuminate the reference plate 10. The reference beam passes through the pinhole array on the reference plate 10 and is collimated by the collimation unit 2. The parallel beam enters the dispersion unit 3 and is split by the dichroic surface of the triangular prism 3-1 in the dispersion unit 3. The reflected beam enters the imaging channel, and the transmitted beam is refracted and dispersed to enter the spectral channel. In the imaging channel, the reflected beam passes through the filter 4, and only the beam of the required wavelength band is observed to pass through. It enters the imaging unit 5 for convergent imaging, and finally the imaging image 12 is collected by the detector 6. The transmitted beam enters the spectral channel through the refraction and dispersion of the triangular prism 3-1 and the corner prism 3-2 of the dispersion unit 3. The dispersed beam passes through the filter 7, and only the beam of the required wavelength band is observed to pass through. It enters the spectral unit 8 for convergent imaging, and finally the spectral image 13 is collected by the detector 9. Taking the known relative position (δX ₀ , δY ₀ ) of the pinhole on the reference plate 10 as a reference, a data mapping relationship is established using the relative position (δX ₁ , δY ₁ ) of the pinhole image on the imaging image 12 and the relative position (δX ₂ , δY ₂ ) of the characteristic spectral line on the spectral image 13 to solve the spatial, brightness and spectral information of any position (X, Y) in the observation field of view.

The imaging and spectral channels are exposed simultaneously, and the celestial image spots in the imaging image and the celestial spectrum in the spectral image have a one-to-one mapping relationship. The working principle of the dual-channel seamless spectrometer includes a corresponding dual-channel data mapping method. A reference plate with a two-dimensional pinhole array is placed at the entrance aperture, that is, the relative position relationship of each pinhole in the reference plate has been calibrated (δX ₀ , δY ₀ ), and the pinholes on the reference plate form a conjugate relationship with the focal plane of the dual channel. The reference plate is illuminated with a reference light source, and the reference light passes through the pinholes distributed in the two-dimensional array and enters the spectrometer. The imaging and spectral channels are exposed simultaneously to obtain the imaging image and spectral image of the two-dimensional pinhole array. With the calibrated relative position of the pinholes on the reference plate (δX ₀ , δY ₀ ) as a reference, the relative position of the pinhole image spots on the imaging image (δX ₁ , δY ₁ ) and the relative position of the characteristic spectral lines on the spectral image (δX ₂ , δY ₂ ) are used to establish a data mapping relationship, as shown in Figure 5. For different observations, this mapping relationship is used to extract the imaging and spectral data of each celestial body from the observation data for scientific research.

The incident aperture: The aperture shape is generally square, but can also be circular or other polygonal. The light beam passing through the aperture is the effective light beam, and the light beam absorbed or emitted by the structure outside the aperture is the invalid light beam. The incident aperture 1 is the object plane or image plane, and is in an object-image conjugate relationship with the detector 1 6 and the detector 2 9.

The collimation unit can be composed of a transmissive, reflective or folding optical system to provide a light beam collimation function. The incident light beam passing through the incident aperture 1 becomes a parallel light beam after passing through the collimation unit 2.

The dispersion unit: The dispersion unit is the core component of the dual-channel seamless spectrometer, providing splitting and dispersion functions. Splitting function: Split the light beam into two beams, which enter the imaging and spectral channels respectively. Dispersion function: In the spectral channel, the dispersion phenomenon of the triangular prism is used to provide the required spectral resolution. As shown in Figure 4, it is composed of at least one triangular prism, which is arranged in sequence according to the angle θ. The first optical surface of the first triangular prism (i.e., triangular prism 1 3-1) provides a splitting function, and the remaining triangular prisms provide a dispersion function. The triangular prisms (triangular prism 1 3-1, triangular prism 2 3-2...triangular prism n3-n, in this embodiment, n≤5) are made of a high-dispersion glass material with a low Abbe coefficient, and the law that the refractive index of the material changes with the wavelength produces a dispersion phenomenon. This embodiment is described in detail by taking the dispersion unit 3 composed of two triangular prisms (triangular prism 1 3-1 and triangular prism 2 3-2) as an example, as shown in Figure 2. The optical properties of the triangular prism are determined by three parameters: the incident angle α, the material refractive index n, and the vertex angle A, as shown in Figure 3. The lower the glass material with the lower Abbe coefficient, the greater the dispersion strength of the dispersion unit 3, and the higher the spectral resolution of the dual-channel seamless spectrometer. The greater the vertex angle A of the triangular prism, the greater the dispersion strength of the dispersion unit 3, and the higher the spectral resolution of the dual-channel seamless spectrometer. The more triangular prisms are used, the greater the dispersion strength of the dispersion unit 3, and the higher the spectral resolution of the dual-channel seamless spectrometer. The triangular prism 1 3-1 and the triangular prism 2 3-2 are placed in the XY plane, and the angle between the normal of the first optical surface 3-1-1 of the triangular prism 1 and the incident light axis is the incident angle α ₁ , and the angle between the second optical surface 3-1-2 of the triangular prism 1 and the first optical surface 3-2-1 of the triangular prism 2 is θ. In the working band, the incident angle α ₁ of the triangular prism 1 3-1 is determined by the minimum deflection angle β of the triangular prism 1 3-1, and the angle θ is defined as the sum of the incident angles of two adjacent triangular prisms (α ₁ +α ₂ ).

The first optical surface 3-1-1 of the triangular prism 1 is the incident surface of the dispersion unit 3. The incident light beam enters the first optical surface 3-1-1 of the triangular prism 1 at an incident angle _α1 . The first optical surface 3-1-1 of the triangular prism 1 is coated with an optical spectroscopic film, which can reflect a part of the light in proportion and transmit another part of the light. The second optical surface 3-1-2 of the triangular prism 1, the first optical surface 3-2-1 of the triangular prism 2, and the second optical surface 3-2-2 of the triangular prism 2 are coated with an anti-reflection film. The light beam reflected by the first optical surface 3-1-1 of the triangular prism 1 enters the imaging channel, and the imaging image is collected to obtain the spatial position and brightness information of the celestial body in the observation field. The light beam transmitted by the first optical surface 3-1-1 of the triangular prism 1 is refracted by the triangular prism 1 3-1 and the triangular prism 2 3-2, and the light beam is dispersed and enters the spectral channel. The spectral image is collected to obtain the spectral information of the celestial body in the observation field.

The optical spectroscopic film on the first optical surface 3-1-1 of the triangular prism 1: The optical spectroscopic film on the first optical surface 3-1-1 of the triangular prism 1 is generally a neutral density spectroscopic film, and the reflected light and the transmitted light distribute the light energy in proportion, and have the same polarization state and wavelength range. The optical spectroscopic film on the first optical surface 3-1-1 of the triangular prism 1 can also be a polarization spectroscopic film, and the polarization state of the reflected light is orthogonal to that of the transmitted light, and the light energy of the reflected light and the transmitted light is determined by the polarization state of the incident light beam itself, and has the same wavelength range. The optical spectroscopic film on the first optical surface 3-1-1 of the triangular prism 1 can also be a dichroic spectroscopic film, and the difference between the working wavelength band of the reflected light and the transmitted light is determined by the dichroic spectroscopic film.

The filter one and filter two: filter one 4 and filter two 7 provide a limited range of working bands, cut off the light beams of non-working bands, and avoid the problem of overlapping pollution caused by redundant spectra. Filter one 4 and filter two 7 can be a single filter assembly, or a filter wheel composed of multiple filters. Different filters can be switched according to the needs of scientific research. Filter one 4 is placed between the dispersion unit 3 and the imaging unit 5, or it can be placed inside the imaging unit 5, or it can be placed between the imaging unit 5 and the detector one 6. Filter two 7 is placed between the dispersion unit 3 and the spectral unit 8, or it can be placed inside the spectral unit 8, or it can be placed between the spectral unit 8 and the detector two 9.

The imaging unit can be composed of a transmission, reflection or reentry optical system to provide a beam converging function. The imaging beam reflected by the dispersion unit 3 is converged on the focal plane through the imaging unit 5 to obtain image spots of various celestial bodies in the observation field.

The spectral unit 8 can be composed of a transmissive, reflective or reentrant optical system to provide a beam converging function. The dispersed light beam transmitted by the dispersion unit 3 is converged on the focal plane through the spectral unit 8 to obtain the dispersion spectrum of each celestial body in the observation field.

The detector 1 and the detector 2 are respectively placed on the focal planes of the imaging unit 5 and the spectral unit 8 to collect imaging and spectral images. They can be various linear array or planar array photoelectric detectors, mainly CCD or CMOS planar array detectors.

The reference plate has a two-dimensional array of transmission pinholes on an opaque substrate, the diameter of the pinholes is generally selected in the range of 10 microns to 200 microns, and the incident light beam can pass through the pinholes and enter the collimation unit 2.

The reference light source: provides the reference light source required for the mapping mode, which can be a high monochromatic light source, a wavelength calibration light source, or a celestial beam with a known characteristic spectrum. With a high monochromatic light source as the reference light source 11, the spectral channel generates a monochromatic image of the pinhole array, each pinhole corresponds to a monochromatic image, which is similar to the image style of the imaging channel. The relative positions of different monochromatic images are measured to solve the mapping relationship between the imaging and the spectral image. With a wavelength calibration light source as the reference light source 11, the spectral channel generates a calibrated spectral image of the pinhole array, each pinhole corresponds to a calibration spectrum, and the calibration spectrum has a characteristic emission or absorption spectrum line. The relative positions of different pinholes corresponding to the same characteristic spectrum line are measured to solve the mapping relationship between the imaging and the spectral image. With a celestial beam with a known characteristic spectrum as the reference light source 11, such as sunlight, the spectral channel generates a celestial spectrum image through the pinhole array, each pinhole corresponds to a celestial spectrum, and the celestial spectrum has a known characteristic absorption or emission spectrum line. The relative positions of different pinholes corresponding to the same characteristic spectrum line are measured to solve the mapping relationship between the imaging and the spectral image.

The imaging and spectral channels are exposed simultaneously to obtain imaging and spectral images respectively, which has the advantages of high temporal resolution and high observation efficiency. The imaging image only contains the spatial position and brightness information of the celestial body within the observation field of view, and can be used independently for imaging or photometric observation without the problem of spectral contamination. In the spectral image, each celestial body has only one spectrum covering the specified band, avoiding the problem of multi-level spectra contaminating each other and non-shining levels occupying part of the light energy and causing loss.

The above description is only a preferred embodiment of the present invention and is not intended to limit the present invention. Any modification, equivalent replacement and improvement made within the spirit and principle of the present invention shall be included in the protection scope of the present invention.

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.