CN115900690A - Evaluation method for signal-to-noise ratio of star measurement - Google Patents
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Abstract
The invention belongs to the field of astronomical navigation, and particularly relates to an evaluation method for a star measurement signal-to-noise ratio, which comprises the following steps: determining the to-be-detected spectrum sections of the to-be-detected star and the detection background, segmenting each to-be-detected spectrum section according to the signal-to-noise ratio calculation precision requirement, and calculating the signal electron number corresponding to each segmented spectrum generated by the to-be-detected star; the number N of signal electrons corresponding to each segment S Adding the signals to obtain the final signal electron number generated by the star to be detected; respectively calculating the number of signal electrons corresponding to each segmented spectrum generated by the background; the number N of signal electrons corresponding to each segment B Adding, as a final signal electron count generated by the background; and calculating the measurement signal-to-noise ratio of the to-be-measured star based on the final signal electronic number generated by the to-be-measured star and the final signal electronic number generated by the background to complete evaluation. The invention provides a sectional integration mode to calculate the signal electron number generated by the star body and the background, and can remarkably improve the analysis precision and the credibility of the star measuring capability of the star sensor.
Description
Technical Field
The invention belongs to the field of astronomical navigation, and particularly relates to an evaluation method for a star body measurement signal-to-noise ratio.
Background
The astronomical navigation can comprehensively provide core navigation information such as position, course, attitude, speed and the like, especially plays a unique important role in a complex electromagnetic environment, has the advantages of high measurement precision, no interference, no time drift, high reliability and the like, and becomes indispensable equipment in a comprehensive navigation system.
The star measurement capability is one of the core indexes of astronomical navigation equipment, but the existing star sensor has some problems in the analysis process of the star measurement capability, wherein the main problems are that parameters such as atmospheric background, transmittance and star point energy related to the star measurement capability of the existing star sensor are generally calculated by adopting a single spectrum wavelength point, and the parameters are distributed along with the wavelength, so that certain errors can be caused, and the analysis accuracy and the reliability of the star measurement capability of the star sensor are seriously influenced.
Disclosure of Invention
Aiming at the defects and improvement requirements of the prior art, the invention provides an evaluation method of a star body measurement signal-to-noise ratio, and aims to improve the evaluation precision of the star body measurement signal-to-noise ratio so as to improve the analysis precision and the reliability of the star measuring capability of a star sensor.
To achieve the above object, according to an aspect of the present invention, there is provided a method for evaluating a signal-to-noise ratio of a star measurement, comprising:
determining a first to-be-detected spectrum section of the to-be-detected star, segmenting the first to-be-detected spectrum section according to the signal-to-noise ratio calculation precision requirement, and respectively calculating the number of signal electrons corresponding to each segmented spectrum generated by the to-be-detected star; the number N of signal electrons corresponding to each segment S Adding the signals to obtain the final signal electron number generated by the star body to be detected;
determining a second spectrum section to be detected of the detection background, segmenting the second spectrum section to be detected according to the signal-to-noise ratio calculation precision requirement, and respectively calculating the signal electron number corresponding to each segmented spectrum generated by the background; the number N of signal electrons corresponding to each segment B Adding, as a final signal electron count generated by the background;
and calculating the measurement signal-to-noise ratio of the to-be-measured star body based on the final signal electronic number generated by the to-be-measured star body and the final signal electronic number generated by the background to finish evaluation.
Further, the length of the segments ranges from 1 to 50 nanometers.
Further, the star body to be detected is a fixed star.
Further, for countingCalculating N S The atmospheric transmittance of (a) is calculated in the following manner:
adopting improved Modtran/CART graphical interface software and combining configuration files of the Modtran/CART graphical interface software to automatically generate the atmospheric transmittance tau a (λ) a distribution curve with the wavelength of the first to-be-measured spectral band, wherein the improved Modtran/CART graphical interface software is configured with a configuration file generated by Matlab, and the configuration file is used for automatically inputting the value of a parameter for calculation of the atmospheric transmittance at each wavelength.
Further, for calculating N B The transmission background intensity of the atmospheric irradiation is calculated and obtained by the following method:
adopting improved Modtran/CART graphical interface software and combining configuration files of the Modtran/CART graphical interface software to automatically generate the background intensity I of atmospheric irradiation transmission B (lambda) a distribution curve along with the wavelength of the second spectral band to be measured, wherein the improved Modtran/CART graphical interface software is configured with a configuration file generated by Matlab, and the configuration file is used for automatically inputting the value of a parameter for calculation of the atmospheric irradiation transmission background intensity under each wavelength.
The invention also provides a star measuring capability analysis method of the star sensor, which adopts the measured signal-to-noise ratio of the star to be measured obtained by the evaluation method of the star measurement signal-to-noise ratio to analyze the star measuring capability of the star sensor.
The present invention also provides a computer-readable storage medium including a stored computer program, wherein when the computer program is executed by a processor, the storage medium controls a device on which the storage medium is located to execute the method for evaluating the signal-to-noise ratio of the star measurement as described above and/or the method for analyzing the star measuring capability of the star sensor as described above.
Generally, by the above technical solution conceived by the present invention, the following beneficial effects can be obtained:
(1) The invention provides a sectional integration mode for calculating the signal electron number generated by the star body and the background, and can remarkably improve the analysis precision and the reliability of the star measuring capability of the star sensor. According to a star measurement capability calculation formula, the number of signal electrons generated by a star body and a background is related to photon energy of a detection waveband, the energy of a photon with a single spectrum point wavelength, namely the central wavelength photon energy, which is generally adopted at present can be calculated according to a 0-star spectrum irradiation table to obtain the central wavelength photon energy of a to-be-measured waveband (generally within a range of 400-1000 nm), for example, the central wavelength of a visible light waveband is 550nm. Actually, the spectral irradiance of the star and the background is changed along with the wavelength distribution, and certain error is caused by adopting the photon energy with the central wavelength. The star target energy and the background energy are equally subdivided (for example, subdivided according to 1-50 nanometers) in a spectrum section to be measured (for example, a 400-1000 wave band), and the analysis precision and the reliability are obviously improved by the form of segmented integration.
(2) The invention also provides a method for combining Matlab to provide automatic support for calculation of atmospheric transmittance and atmospheric irradiation transmission background intensity, so that the calculation time of the parameters related to the star measurement capability is obviously reduced, and the calculation efficiency is improved.
Drawings
Fig. 1 is a flow chart of a method for evaluating a signal-to-noise ratio of a star measurement according to an embodiment of the present invention;
FIG. 2 is a schematic diagram illustrating influence factors of a photoelectric star measuring capability according to an embodiment of the present invention;
FIG. 3 is a schematic diagram of a star sensor receiving radiation from a star body according to an embodiment of the present invention;
FIG. 4 is a schematic diagram of a star sensor receiving spatial background radiation according to an embodiment of the present invention;
FIG. 5 shows the atmospheric transmittance τ provided by an embodiment of the present invention a (λ) automated computation flow chart;
fig. 6 shows transmittance τ generated by Matlab automatically generating configuration files according to an embodiment of the present invention a (λ) plot of distribution with wavelength;
FIG. 7 is a graph of a stellar spectral distribution of a G2 type 0 stellar provided by an embodiment of the present invention;
FIG. 8 is a diagram illustrating an embodiment of generating an atmospheric irradiation transmission background intensity I by automatically generating a configuration file according to Matlab B (λ) distribution curve with wavelength;
FIG. 9 is a graph of the daytime atmospheric background radiation at a height of 50km and in a wavelength range of 400-1000nm provided by an embodiment of the present invention.
Detailed Description
In order to make the objects, technical solutions and advantages of the present invention more apparent, the present invention is described in further detail below with reference to the accompanying drawings and embodiments. It should be understood that the specific embodiments described herein are merely illustrative of the invention and are not intended to limit the invention. In addition, the technical features involved in the embodiments of the present invention described below may be combined with each other as long as they do not conflict with each other.
Example one
A method for evaluating a signal-to-noise ratio of a star measurement, as shown in fig. 1, includes:
determining a first to-be-detected spectrum section of the to-be-detected star, segmenting the first to-be-detected spectrum section according to the signal-to-noise ratio calculation precision requirement, and respectively calculating the number of signal electrons corresponding to each segmented spectrum generated by the to-be-detected star; the number N of signal electrons corresponding to each segment S Adding the signals to obtain the final signal electron number generated by the star body to be detected;
determining a second spectrum section to be detected of the detection background, segmenting the second spectrum section to be detected according to the signal-to-noise ratio calculation precision requirement, and respectively calculating the signal electron number corresponding to each segmented spectrum generated by the background; the number N of signal electrons corresponding to each segment B Adding, as a final signal electron count generated by the background;
and calculating the measurement signal-to-noise ratio of the to-be-measured star based on the final signal electronic number generated by the to-be-measured star and the final signal electronic number generated by the background to complete evaluation.
As shown in fig. 2, which is a schematic diagram of influence factors of the photoelectric star measurement capability, the calculation of the photoelectric channel star measurement capability involves complex parameters such as star radiation, sky background, atmospheric transmittance of a detection band, transmittance of an optical system, relative aperture of the optical system, focal length of the optical system, quantum efficiency of a detector, noise, and the like. The signal-to-noise ratio of the optoelectrical stellatemic channel, which is stellatemic capability dependent, can be calculated by:
in the formula, K e An additional factor for the processing circuit, typically 0.8; n is a radical of S The number of signal electrons generated for the star; n is a radical of B The number of signal electrons generated for background; sigma T Selecting the RMS value of the dark current noise electronic number of the detector according to related parameters of a detector manual; sigma R To read the RMS value of the number of circuit noise electrons, it was chosen according to the relevant parameters of the detector manual. Therefore, the key to the calculation of the star measuring ability is the number N of signal electrons generated by the star S The number of signal electrons N generated by the calculation and background of (2) B And (4) calculating.
Number N of signal electrons for each segmented spectrum generated by the star to be measured S The star sensor receives a schematic diagram of radiation of a star body, as shown in fig. 3, the field angle of the star to the earth radiation is generally less than 0.01 ″, the star can be regarded as a point light source at infinity, and the star can be regarded as parallel light. The photoelectric effect of the star on a certain imaging pixel of the photoelectric detector produces N number of electrons per second S The method specifically comprises the following steps:
in the formula, D is the aperture of the optical system of the star sensor; λ is wavelength and range is λ 1 To lambda 2 ；E ph (λ) is the energy of a single photon at wavelength λ, E ph (λ) = hc/λ, h is planck constant 6.6 × 10 -34 J/s, c is the speed of light 3X 10 8 m/s；τ a (λ) is the atmospheric transmittance; tau is 0 (lambda) is the optical system transmittance, which is related to the optical system characteristics, varies with wavelength, and can be obtained by a calculation formula and a test method; QE (lambda) is the corresponding efficiency of the detector quantum, namely the number of electrons converted by photons of a detection waveband in a photoelectric detector, and is inquired through a typical detector quantum response efficiency curve; e m (lambda) isThe spectral irradiance of the fixed star on the detection surface of the star sensor is W.m -2 ·m -1 。
Number of signal electrons N generated with respect to background B As shown in fig. 4, the star sensor receives a schematic diagram of spatial background radiation, and the sky background is simplified into a uniform radiance target, and the spatial background radiation is processed by using an extended source target, so that the atmospheric transmittance does not need to be considered when calculating the spatial background radiation. The photoelectric effect generated by the photoelectric effect of the space background on a certain imaging pixel of the photoelectric detector is N B The calculation is as follows:
wherein λ is the wavelength and the range is λ 1 To lambda 2 (ii) a Omega is a solid angle occupied by a unit pixel, the unit is sphericity, and the relation between omega and the field angle of the star sensor is
N is the direction pixel, and omega is inversely proportional to the square of the focal length f of the optical system; i is B (lambda) is the scattered radiation intensity of the space background light before the space background light is transmitted to the star sensor optical system, and the unit is W.m -2 ·sr -1 ·m -1 (ii) a D is the aperture of the optical system; e ph (λ) is the energy of a single photon at wavelength λ, E ph (λ) = hc/λ, h is planck constant 6.6 × 10 -34 J/s, c is the speed of light 3X 10 8 m/s；τ 0 (lambda) is the optical system transmittance, which is related to the optical system characteristics, varies with wavelength, and can be obtained by a calculation formula and a test method; QE (λ) is the detector quantum efficiency, i.e. the number of electrons converted in the photodetector by photons in a detection band, which is queried by a typical detector quantum response efficiency curve.
Preferably, the length of the segments ranges from 1 to 50 nanometers.
Preferably, the atmospheric transmittance τ is shown in FIG. 5 a (lambda) automatic calculation process, in the traditional calculation process, atmosphere permeationExcess rate tau a The (lambda) is generally calculated by Modtran/CART graphical interface, but the method is complicated to operate, too slow and prone to errors. This example proposes a transmittance τ a (lambda) automatic calculation technology generates the atmospheric transmittance tau by automatically generating configuration files through Matlab a And (lambda) along with the distribution curve of the wavelength, the calculation time is greatly shortened, and the reliability of the calculation result is improved.
Specifically, a configuration file of Modtran/CART graphical interface software is automatically generated through Matlab;
generating the atmospheric transmittance tau by adopting Modtran/CART graphical interface software and combining the configuration file a (lambda) a distribution curve along with the wavelength of the first to-be-measured spectral band, wherein the configuration file is used for automatically inputting the value of a parameter for calculation for calculating the atmospheric transmittance at each wavelength.
As shown in FIG. 6, transmittance τ generated for automatic profile generation by Matlab a (lambda) along with the distribution curve of the wavelength, the calculation condition is the middle latitude summer atmosphere condition, and the 50km high atmosphere transmission window is vertically observed towards the zenith at noon in summer.
The spectral irradiance of the fixed star reaching the detection surface of the star sensor is related to the type and grade of the star and changes along with the wavelength distribution. In the design of the star sensor, parameters such as the detection capability of the star sensor are generally predicted and estimated by taking star and the like as concepts. In the analysis process of the star measuring capability of the traditional star sensor, a single spectrum wavelength point is generally adopted to calculate the spectral irradiance of a fixed star, so that a large error is caused. In the embodiment, as mentioned above, the stellar spectral irradiance is subdivided into the full-working spectral range according to 1-50 nanometers, and the distributed energy integral calculation is performed on the subdivided spectral range by combining the atmospheric transmittance, the optical system transmittance and the detector quantum response efficiency curve, so as to calculate the star measurement capability related parameter N of the star sensor S 。
The G2-type 0-class star is taken as an example to describe the star target energy calculation process proposed in the present embodiment. As shown in fig. 7, is an astroglia spectral distribution curve of a G2 type 0 isostar. The optical system design of the star sensor needs to reduce reflection and dispersion as much as possible, and the passing range of the spectrum is 400-1000 nm.
Its spectral irradiance E 0 (λ) was subdivided by 50nm into the full operating spectral range, as shown in Table 1.
TABLE 1 Spectrum irradiance distribution table of G2 type 0 star
According to the spectral irradiance distribution table in the table 1, the number N of electrons generated by the photoelectric effect per second on a pixel of a certain imaging of the photoelectric detector by the star can be calculated by substituting the formula (2) into the corresponding efficiency curve of the gas transmission rate, the optical system transmission rate and the detector quantum S 。
Preferably, the background intensity I is transmitted by atmospheric radiation during conventional calculations B The (lambda) is generally calculated by Modtran/CART graphical interface, but the method is complicated to operate, too slow and prone to errors. According to the automatic calculation technology of the atmospheric background radiation intensity, as shown in fig. 8, the atmospheric radiation transmission background intensity I is generated by automatically generating a configuration file through Matlab B And (lambda) along with the distribution curve of the wavelength, the calculation time is greatly shortened, and the reliability of the calculation result is improved. Specifically, a configuration file of Modtran/CART graphical interface software is automatically generated through Matlab; generating the background intensity I of atmospheric irradiation transmission by adopting Modtran/CART graphical interface software and combining the configuration file B (lambda) a distribution curve along with the wavelength of the second spectral band to be measured, wherein the configuration file is used for automatically inputting the value of a parameter for calculation for calculating the transmission background intensity of the atmospheric irradiation under each wavelength.
As shown in fig. 9, the curve is a 50km height 400-1000nm band daytime atmospheric background radiation curve generated by using an atmospheric background radiation intensity automatic calculation technology. The observed atmospheric mode is the average atmospheric condition in the northwest region. The observation zenith angle range is changed at intervals of 5 degrees from 45 degrees to 65 degrees, the solar zenith angle range is changed at intervals of 10 degrees from 0 degrees to 70 degrees, the observation azimuth angle is changed at intervals of 20 degrees relative to the solar azimuth angle range from 0 degrees to 180 degrees, and the iterative computation is carried out for 1000 times.
The atmospheric irradiation transmission background energy calculation method provided by the embodiment of the invention is characterized in that the radiation intensity of the sky background radiation maximum position in the whole day area pointing to the daytime is subdivided into the whole working spectral range according to 1-50 nanometers, and the star sensor star measurement capability related parameter N is calculated by combining the transmittance of an optical system and the quantum response efficiency curve of a detector and by using a method of energy integration of distribution of the subdivided spectral range B 。
The spectral radiation intensity was subdivided into the full operating spectral range at 50nm as shown in table 2.
TABLE 2 background radiation intensity distribution chart
| Wavelength mum | Background radiation intensity W/cm 2 /sr/ |
| 1 | 4.17E-07 |
| 0.95 | 6.14E-07 |
| 0.9 | 8.45E-07 |
| 0.85 | 1.02E-06 |
| 0.8 | 1.31E-06 |
| 0.75 | 1.96E-06 |
| 0.7 | 2.78E-06 |
| 0.65 | 3.86E-06 |
| 0.6 | 6.44E-06 |
| 0.55 | 8.98E-06 |
| 0.5 | 1.34E-05 |
| 0.45 | 2.12E-05 |
| 0.4 | 2.55E-05 |
According to the background spectrum radiation intensity distribution table in the table 2, the number of electrons generated by photoelectric effect per second on a certain imaging pixel of the photoelectric detector by the space background can be calculated by substituting the formula (3) into the optical system transmittance and the corresponding efficiency curve of the detector quantum B 。
Finally, the number N of signal electrons generated by the star body S And the number N of signal electrons generated by the background B The signal-to-noise ratio of the photoelectric star measurement channel capable of feeding back the star measurement capability can be calculated by substituting the formula (1).
Example two
A star sensor star measurement capability analysis method adopts the measured signal-to-noise ratio of the to-be-measured star obtained by the star body measurement signal-to-noise ratio evaluation method in the embodiment to carry out star sensor star measurement capability analysis.
The related technical solution is the same as the first embodiment, and is not described herein again.
EXAMPLE III
A computer readable storage medium comprising a stored computer program, wherein when the computer program is executed by a processor, the storage medium controls a device on which the storage medium is located to perform a method for evaluating a signal-to-noise ratio of a star measurement as described above and/or a method for analyzing a star capability of a star sensor as described above.
The related technical solutions are the same as those of the first embodiment and the second embodiment, and are not described herein again.
It will be understood by those skilled in the art that the foregoing is only a preferred embodiment of the present invention, and is not intended to limit the invention, and that any modification, equivalent replacement, or improvement made within the spirit and principle of the present invention should be included in the scope of the present invention.
Claims (7)
1. A method for evaluating a signal-to-noise ratio of a star measurement is characterized by comprising the following steps:
determining a first to-be-detected spectrum section of the to-be-detected star, segmenting the first to-be-detected spectrum section according to the signal-to-noise ratio calculation precision requirement, and respectively calculating the number of signal electrons corresponding to each segmented spectrum generated by the to-be-detected star; the number N of signal electrons corresponding to each segment S Adding the signals to obtain the final signal electron number generated by the star body to be detected;
determining a second spectrum section to be detected of the detection background, segmenting the second spectrum section to be detected according to the signal-to-noise ratio calculation precision requirement, and respectively calculating the signal electron number corresponding to each segmented spectrum generated by the background; the number N of signal electrons corresponding to each segment B Adding, as a final signal electron count generated by the background;
and calculating the measurement signal-to-noise ratio of the to-be-measured star body based on the final signal electronic number generated by the to-be-measured star body and the final signal electronic number generated by the background to finish evaluation.
2. The method of claim 1, wherein the length of the segments is in the range of 1-50 nm.
3. The evaluation method according to claim 1, wherein the star to be tested is a star.
4. The evaluation method according to claim 1, for calculating N S Is calculated in the following way:
adopting improved Modtran/CART graphical interface software and combining configuration files of the Modtran/CART graphical interface software to automatically generate the atmospheric transmittance tau a (lambda) a distribution curve with the wavelength of the first to-be-measured spectral band, wherein the improved Modtran/CART graphical interface software is configured with a configuration file generated by Matlab, and the configuration file is used for automatically inputting the value of a parameter for calculation for calculating the atmospheric transmittance at each wavelength.
5. The evaluation method according to claim 1, for calculating N B The transmission background intensity of the atmospheric irradiation is calculated by the following method:
adopting improved Modtran/CART graphical interface software and combining configuration files of the Modtran/CART graphical interface software to automatically generate the background intensity I of atmospheric irradiation transmission B (lambda) a distribution curve along with the wavelength of the second spectral band to be measured, wherein the improved Modtran/CART graphical interface software is configured with a configuration file generated by Matlab, and the configuration file is used for automatically inputting the value of a parameter for calculation of the atmospheric irradiation transmission background intensity under each wavelength.
6. A star sensor star measurement capability analysis method, characterized in that the star sensor star measurement capability analysis is performed by using the measured signal-to-noise ratio of the to-be-measured star obtained by the star measurement signal-to-noise ratio evaluation method according to any one of claims 1 to 5.
7. A computer-readable storage medium, comprising a stored computer program, wherein when the computer program is executed by a processor, the computer program controls a device on which the storage medium is located to perform a method for evaluating a star body measurement signal-to-noise ratio according to any one of claims 1 to 5 and/or a method for analyzing a star measurement capability of a star sensor according to claim 6.
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| CN117473799B (en) * | 2023-12-28 | 2024-04-09 | 苏州泰瑞迅科技有限公司 | Radiation detector point source efficiency calculation method and system based on super computing platform |
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