CN1635346A - Space modulation type interference spectrum imager on-satellite calibration method - Google Patents
Space modulation type interference spectrum imager on-satellite calibration method Download PDFInfo
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- 238000010521 absorption reaction Methods 0.000 claims abstract description 16
- 230000003287 optical effect Effects 0.000 claims description 20
- 230000004044 response Effects 0.000 claims description 12
- 238000003384 imaging method Methods 0.000 claims description 10
- 230000005855 radiation Effects 0.000 claims description 10
- 238000009826 distribution Methods 0.000 claims description 6
- 238000005316 response function Methods 0.000 claims description 6
- 230000010354 integration Effects 0.000 claims description 5
- 230000008569 process Effects 0.000 claims description 4
- 229910000722 Didymium Inorganic materials 0.000 claims description 3
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- 239000013307 optical fiber Substances 0.000 description 2
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- 229910052736 halogen Inorganic materials 0.000 description 1
- 150000002367 halogens Chemical class 0.000 description 1
- WFKWXMTUELFFGS-UHFFFAOYSA-N tungsten Chemical compound [W] WFKWXMTUELFFGS-UHFFFAOYSA-N 0.000 description 1
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Abstract
A space modulation type interference spectrum imager on-satellite calibration method. The method comprises the following steps: a uniform surface light source with a flat spectral curve enters an integrating sphere to obtain a surface light source with higher surface uniformity; generating an absorption peak on the spectral curve of the light source; the parallel light with a certain field angle is generated by the collimating lens system to become a wide-spectrum calibration light source with characteristic spectral lines, and the spectral curve of the calibration light source is measured by an instrument. The calibration light source is imaged on a primary image surface slit through a front lens of a hyper-spectrum imager, then an interference image is generated on a detector array through an interferometer, a Fourier lens and a cylindrical mirror, and the spectrum curve of the calibration light source is obtained through computer restoration; and comparing the spectral curve with a spectral curve obtained in advance to obtain the required calibration parameters. And correcting the data obtained by the instrument by using the calibration parameters to finish calibration.
Description
Technical field
The present invention relates to calibrating method on a kind of spatial modulation type interference spectrum imager star.
Background technology
The interference type spectral imaging technique also claims interference imaging spectral technology, developed the nineties in last century, employing be the remote sensing observations means, on the star calibration be one of its core key technology, also be in conceptual phase at present in the world.
In engineering practice, owing to the character of material, the reasons of debuging such as precision, there is certain gap in the target information federation that instrument obtains with realistic objective, needs to obtain by calibration the parameter of correction, the result that instrument the is obtained realistic target conditions of trying one's best is so need calibrate.
The calibration of interference type super spectrum imager is different with common CCD remote sensing camera.What the common CCD remote sensing camera obtained is the several picture of target, and only need carry out the radiancy calibration can meet the demands; And interference type super spectrum imager also will obtain the spectral information of target except the several picture that obtains target, so it should carry out the radiancy calibration, also will carry out spectral calibration.
Because the principle of work of interference type super spectrum imager is different with the principle of color dispersion-type imaging spectrometer, what color dispersion-type imaging spectrometer detector received is the direct sunshine spectrum information of target, is the Fourier transform information of target optical spectrum and interference type imaging spectrometer detector receives.It is identical that both calibrate purpose, but method divergence is bigger.
The U.S. in the powerful moonlet of in July, 2000 emission be in the world first drop into practical interference type super spectrum imager, originally powerful moonlet is want with an optical fiber sunshine to be introduced into the light source of instrument as calibration, uncommon nationality compares the data of instrument acquisition and known solar spectrum, and the parameter that obtains revising.But this imagination does not finally try out, but compares correction with the calibration of terrestrial radiation field.Since to the shortcoming that the solar spectrum characteristic is understood, the present domestic optical fiber that is suitable for AEROSPACE APPLICATION of also can not produce.
Summary of the invention
The invention solves background technology and can't realize spaceborne interference type super spectrum imager calibration, promptly can not carry out the technical matters of radiancy calibration and spectral calibration simultaneously.
Technical solution of the present invention is:
Calibrating method on a kind of spatial modulation type interference spectrum imager star, its special character is: this method comprises:
1). by
Cola illuminator or integration sphere light source systemLight source sends the smooth uniform area light source of the curve of spectrum, enters integrating sphere 4 by inlet 3, obtains the higher area source of surface uniformity.
2). make the curve of spectrum of this light source produce absorption peak.Place didymium glass or other has the absorption peak transparent material and makes its curve of spectrum produce two, three or more absorption peak at outlet 5 places.
3). produce directional light through calibration lens system, promptly with certain visual angleBecome the wide range scaling light source that has characteristic spectral line, record the curve of spectrum of this scaling light source with reference instrument.
4). scaling light source is imaged on image planes slit through the preset lens of hyperspectral imager, and then lists the generation interference image through interferometer, fourier transform lens, cylindrical mirror at detector array.This image after computing machine recovery software rejuvenation, obtains the curve of spectrum of the scaling light source of hyperspectral imager acquisition,
5). with this curve of spectrum and the comparison of the curve of spectrum that we obtain in advance, just can obtain the calibration parameter of our needs.Smooth wide range can be used for the radiancy calibration, and the absorption peak of light source can be used for determining the spectral resolution of instrument, and the position of spectral line and relative amplitude.
6). with above-mentioned calibration parameter the data that instrument obtains are revised, finished calibration.
Above-mentioned collimating mirror focal length is identical with the imaging spectrometer preset lens with relative aperture; Collimating mirror 6 with the preset lens of hyperspectral imager with the optical convergence of integrating sphere 4 outgoing on the slit of hyperspectral imager optical system, then by interferometer, Fourier lens, cylindrical mirror imaging on detector; Collimating mirror 6---light source is become directional light; Thus, the scaling light source of whole scaling system generation just becomes the wide spectrum light source that has characteristic spectral line.Wide spectrum light source can be as the radiancy calibration, and the characteristic spectral line of light source carries out the spectral characteristic analysis by spectrum recovering, can determine the situation of change of spectrum line position, reaches the purpose of relative calibration on the star; Again through calibration lens system 6, last light is through catoptron 7 light path of turning back, and the optical system that is introduced into instrument is calibrated.
Above-mentioned calibration is meant determines that remote sensor exports the process of accurate numerical value, and main means are to measure the response of remote sensor to a known radiation characteristic target.Concerning interference type super spectrum imager, the calibration content comprises that mainly spectral calibration and radiancy calibrate two aspects, wherein the radiancy calibration comprises that again relative radiancy is calibrated and the absolute radiation degree is calibrated two kinds, the radiancy calibration is used for determining the relative radiometric response of each spectral coverage of instrument and the relative radiometric response of detector different units relatively, absolute radiometric calibration is used for determining the instrument output signal, enables to react the absolute radiation intensity of input signal.
Described spectral calibration: be exactly position, frequency and the maximum optical path difference of determining the interferogram zero optical path difference, thereby determine the centre wavelength and the half band-width of each spectral coverage.It is very important to the spectral resolution that guarantees instrument, and whether the duty to interferometer normally is topmost criterion simultaneously.
Described radiancy calibration: mainly carry out relative radiancy calibration usually on the star.
The scaling light source of known spectra intensity distributions B (σ) enters hyperspectral imager, and the interference strength that obtains pixel is distributed as:
I(x)＝∫K(σ)B(σ)cos(2πxσ)dσ+IN
IN is the zero input response of pixel, and x is an optical path difference, and σ is a wave number.K (σ) is the spectral response functions of system.
Above-mentioned interference figure carries out inversefouriertransform after filtering, phase place correction, obtain recovered light spectral intensity distribution B ' (σ), then has
B’(σ)＝K(i，j)×B(σ)
K (i, j) in, i and j be representation space direction pixel number and spectral coverage number respectively.(i j) is exactly the spectrum modified value of i row detector unit, (j=1,2 to K ... N, N are the spectral coverage number), i.e. spectral response functions.
Use the same method, can be listed as (i=2 each ... M) modified value is obtained in the unit, and (i j), provides spectral radiant emittance correction data, finishes the calibration of spectral radiant emittance to obtain a complete two-dimentional correction factor matrix K at last.
The present invention has the following advantages:
1. realized the calibration of spaceborne interference type super spectrum imager;
2. can finish radiancy calibration and spectral calibration simultaneously;
3. calibration precision can reach: relative accuracy is 5%, and absolute precision is 10%;
4. material, instrument do not need special;
5. adopt existing material, instrument can realize calibrating purpose.
Description of drawings
Accompanying drawing is the structural representation of calibration optical system on the star of the present invention.
Drawing reference numeral explanation: 1-light source, 2-condenser, 3-inlet, 4-integrating sphere, 5-outlet, 6-collimation
MirrorSystem, the 7-catoptron.
Embodiment
The curve of spectrum of scaling system light source of the present invention can record in advance.The spectrum of halogen tungsten lamp is more smooth, through integration sphere light source system, can produce some sharp-pointed absorption peaks on the spectral line, and the number of absorption peak, position are relevant with the material of integrating sphere mouth.Utilize the flat of spectrum to do the radiancy calibration, do spectral calibration with the position and the halfwidth of absorption peak.
Referring to accompanying drawing, the present invention by
The cola illuminator,
Integration sphere light source systemWith
Calibration lens systemForm.
By
Cola illuminator or integration sphere light source systemLight source sends the smooth uniform area light source of the curve of spectrum, enters integrating sphere 4 by inlet 3, obtains the higher area source of surface uniformity.
2. make the curve of spectrum of this light source produce absorption peak.Place didymium glass or other has the absorption peak transparent material and makes its curve of spectrum produce two, three or more absorption peak at outlet 5 places.
3. produce directional light through calibration lens system, promptly with certain visual angleBecome the wide range scaling light source that has characteristic spectral line, record the curve of spectrum of this scaling light source with reference instrument.
4. scaling light source is imaged on image planes slit through the preset lens of hyperspectral imager, and then lists the generation interference image through interferometer, fourier transform lens, cylindrical mirror at detector array.This image after computing machine recovery software rejuvenation, obtains the curve of spectrum of the scaling light source of hyperspectral imager acquisition,
5. with this curve of spectrum and the comparison of the curve of spectrum that we obtain in advance, just can obtain the calibration parameter of our needs.Smooth wide range can be used for the radiancy calibration, and the absorption peak of light source can be used for determining the spectral resolution of instrument, and the position of spectral line and relative amplitude.
6. with above-mentioned calibration parameter the data that instrument obtains are revised, finished calibration.
The collimating mirror focal length is identical with the imaging spectrometer preset lens with relative aperture.
Collimating mirror 6 with the preset lens of hyperspectral imager with the optical convergence of integrating sphere 4 outgoing on the slit of hyperspectral imager optical system, then by interferometer, Fourier lens, cylindrical mirror imaging on detector.Collimating mirror 6---light source is become directional light.
Like this, the scaling light source that produces of whole scaling system just becomes the wide spectrum light source that has characteristic spectral line.Wide spectrum light source can be as the radiancy calibration, and the characteristic spectral line of light source carries out the spectral characteristic analysis by spectrum recovering, can determine the situation of change of spectrum line position, reaches the purpose of relative calibration on the star.Again through calibration lens system 6, last light is through catoptron 7 light path of turning back, and the optical system that is introduced into instrument is calibrated.Lambert's plate 8,
In engineering practice, because material character, process, debug reasons such as precision, and space environment and ground environment is different, can cause the variation of the signal that instrument collects, therefore, need to obtain the parameter of correction by calibration.
Supplementary notes:
Calibration is meant determines that remote sensor exports the process of accurate numerical value, and main means are to measure the response of remote sensor to a known radiation characteristic target.Concerning interference type super spectrum imager, the calibration content comprises that mainly spectral calibration and radiancy calibrate two aspects, wherein the radiancy calibration comprises that again relative radiancy is calibrated and the absolute radiation degree is calibrated two kinds, the radiancy calibration is used for determining the relative radiometric response of each spectral coverage of instrument and the relative radiometric response of detector different units relatively, absolute radiometric calibration is used for determining the instrument output signal, enables to react the absolute radiation intensity of input signal.
Spectral calibration: be exactly position, frequency and the maximum optical path difference of determining the interferogram zero optical path difference, thereby determine the centre wavelength and the half band-width of each spectral coverage.It is very important to the spectral resolution that guarantees instrument, and whether the duty to interferometer normally is topmost criterion simultaneously.
Radiancy calibration: mainly carry out relative radiancy calibration usually on the star.
The scaling light source of known spectra intensity distributions B (σ) enters hyperspectral imager, and the interference strength that obtains pixel is distributed as:
I(x)＝∫K(σ)B(σ)cos(2πxσ)dσ+IN
IN is the zero input response of pixel, and x is an optical path difference, and σ is a wave number.K (σ) is the spectral response functions of system.
Above-mentioned interference figure carries out inversefouriertransform after filtering, phase place correction, obtain recovered light spectral intensity distribution B ' (σ), then has
B’(σ)＝K(i，j)×B(σ)
K (i, j) in, i and j be representation space direction pixel number and spectral coverage number respectively.(i j) is exactly the spectrum modified value of i row detector unit, (j=1,2 to K ... N, N are the spectral coverage number), i.e. spectral response functions.
Use the same method, can be listed as (i=2 each ... M) modified value is obtained in the unit, and (i j), provides spectral radiant emittance correction data, finishes the calibration of spectral radiant emittance to obtain a complete two-dimentional correction factor matrix K at last.
Claims (3)
- Calibrating method on 1 one kinds of spatial modulation type interference spectrum imager stars, it is characterized in that: this method comprises:1). by Cola illuminator or integration sphere light source systemLight source sends the smooth uniform area light source of the curve of spectrum, enters integrating sphere 4 by inlet 3, obtains the higher area source of surface uniformity.2). make the curve of spectrum of this light source produce absorption peak.Place didymium glass or other has the absorption peak transparent material and makes its curve of spectrum produce two, three or more absorption peak at outlet 5 places.3). produce directional light through calibration lens system, promptly with certain visual angleBecome the wide range scaling light source that has characteristic spectral line, record the curve of spectrum of this scaling light source with reference instrument.4). scaling light source is imaged on image planes slit through the preset lens of hyperspectral imager, and then lists the generation interference image through interferometer, fourier transform lens, cylindrical mirror at detector array.This image after computing machine recovery software rejuvenation, obtains the curve of spectrum of the scaling light source of hyperspectral imager acquisition,5). with this curve of spectrum and the comparison of the curve of spectrum that we obtain in advance, just can obtain the calibration parameter of our needs.Smooth wide range can be used for the radiancy calibration, and the absorption peak of light source can be used for determining the spectral resolution of instrument, and the position of spectral line and relative amplitude.6). with above-mentioned calibration parameter the data that instrument obtains are revised, finished calibration.
- Calibrating method on the 2 spatial modulation type interference spectrum imager stars according to claim 1, it is characterized in that: described collimating mirror focal length is identical with the imaging spectrometer preset lens with relative aperture; Collimating mirror 6 with the preset lens of hyperspectral imager with the optical convergence of integrating sphere 4 outgoing on the slit of hyperspectral imager optical system, then by interferometer, Fourier lens, cylindrical mirror imaging on detector; Collimating mirror 6---light source is become directional light; Thus, the scaling light source of whole scaling system generation just becomes the wide spectrum light source that has characteristic spectral line.Wide spectrum light source can be as the radiancy calibration, and the characteristic spectral line of light source carries out the spectral characteristic analysis by spectrum recovering, can determine the situation of change of spectrum line position, reaches the purpose of relative calibration on the star; Again through calibration lens system 6, last light is through catoptron 7 light path of turning back, and the optical system that is introduced into instrument is calibrated.
- Calibrating method on the 3 spatial modulation type interference spectrum imager stars according to claim 1 and 2, it is characterized in that: described calibration is meant determines that remote sensor exports the process of accurate numerical value, and main means are to measure the response of remote sensor to a known radiation characteristic target.Concerning interference type super spectrum imager, the calibration content comprises that mainly spectral calibration and radiancy calibrate two aspects, wherein the radiancy calibration comprises that again relative radiancy is calibrated and the absolute radiation degree is calibrated two kinds, the radiancy calibration is used for determining the relative radiometric response of each spectral coverage of instrument and the relative radiometric response of detector different units relatively, absolute radiometric calibration is used for determining the instrument output signal, enables to react the absolute radiation intensity of input signal.Described spectral calibration: be exactly position, frequency and the maximum optical path difference of determining the interferogram zero optical path difference, thereby determine the centre wavelength and the half band-width of each spectral coverage.It is very important to the spectral resolution that guarantees instrument, and whether the duty to interferometer normally is topmost criterion simultaneously.Described radiancy calibration: mainly carry out relative radiancy calibration usually on the star.The scaling light source of known spectra intensity distributions B (σ) enters hyperspectral imager, and the interference strength that obtains pixel is distributed as:I(x)＝∫K(σ)B(σ)cos(2π×σ)dσ+ININ is the zero input response of pixel, and x is an optical path difference, and σ is a wave number.K (σ) is the spectral response functions of system.Above-mentioned interference figure carries out inversefouriertransform after filtering, phase place correction, obtain recovered light spectral intensity distribution B ' (σ), then hasB’(σ)＝K(i，j)×B(σ)K (i, j) in, i and j be representation space direction pixel number and spectral coverage number respectively.(i j) is exactly the spectrum modified value of i row detector unit, (j=1,2 to K ... N, N are the spectral coverage number), i.e. spectral response functions.Use the same method, can be listed as (i=2 each ... M) modified value is obtained in the unit, and (i j), provides spectral radiant emittance correction data, finishes the calibration of spectral radiant emittance to obtain a complete two-dimentional correction factor matrix K at last.
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Cited By (7)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN100470216C (en) * | 2007-10-30 | 2009-03-18 | 中国科学院西安光学精密机械研究所 | Comparison method of different types of spectrometers |
| CN101187705B (en) * | 2007-12-19 | 2011-05-18 | 中国科学院空间科学与应用研究中心 | Spectrum irradiance standard light source for ultraviolet optical instrument radiometric calibration |
| CN101620177B (en) * | 2008-07-03 | 2011-08-03 | 韩国轮胎株式会社 | System and method for analyzing tire uniformity |
| CN102788643A (en) * | 2012-07-13 | 2012-11-21 | 中国科学院长春光学精密机械与物理研究所 | Method for calibrating ontrack high-precision optical spectrum of space remote sensing optical spectrum instrument |
| CN103293680A (en) * | 2013-06-17 | 2013-09-11 | 山东神戎电子股份有限公司 | Inside-chamber reflecting dodging lighting device for laser lighting |
| CN104266758A (en) * | 2014-10-21 | 2015-01-07 | 中国科学院光电研究院 | Reference wave number calibration method of large-aperture space heterodyning interference spectrum imager |
| CN110399646A (en) * | 2019-07-01 | 2019-11-01 | 西安工业大学 | A kind of DFDI instrument models method for building up for being outer planet detection |
Family Cites Families (1)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| US6051835A (en) * | 1998-01-07 | 2000-04-18 | Bio-Rad Laboratories, Inc. | Spectral imaging apparatus and methodology |
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2003
- 2003-12-31 CN CNB2003101247569A patent/CN100494923C/en not_active Expired - Fee Related
Cited By (9)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN100470216C (en) * | 2007-10-30 | 2009-03-18 | 中国科学院西安光学精密机械研究所 | Comparison method of different types of spectrometers |
| CN101187705B (en) * | 2007-12-19 | 2011-05-18 | 中国科学院空间科学与应用研究中心 | Spectrum irradiance standard light source for ultraviolet optical instrument radiometric calibration |
| CN101620177B (en) * | 2008-07-03 | 2011-08-03 | 韩国轮胎株式会社 | System and method for analyzing tire uniformity |
| CN102788643A (en) * | 2012-07-13 | 2012-11-21 | 中国科学院长春光学精密机械与物理研究所 | Method for calibrating ontrack high-precision optical spectrum of space remote sensing optical spectrum instrument |
| CN102788643B (en) * | 2012-07-13 | 2014-03-12 | 中国科学院长春光学精密机械与物理研究所 | Method for calibrating ontrack high-precision optical spectrum of space remote sensing optical spectrum instrument |
| CN103293680A (en) * | 2013-06-17 | 2013-09-11 | 山东神戎电子股份有限公司 | Inside-chamber reflecting dodging lighting device for laser lighting |
| CN103293680B (en) * | 2013-06-17 | 2015-07-01 | 山东神戎电子股份有限公司 | Inside-chamber reflecting dodging lighting device for laser lighting |
| CN104266758A (en) * | 2014-10-21 | 2015-01-07 | 中国科学院光电研究院 | Reference wave number calibration method of large-aperture space heterodyning interference spectrum imager |
| CN110399646A (en) * | 2019-07-01 | 2019-11-01 | 西安工业大学 | A kind of DFDI instrument models method for building up for being outer planet detection |
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