Fourier Transform Spectroscopy is now widely used in many routine measurement applications. In principle, very high resolution can be achieved in FT Spectroscopy rivaling the resolution of infrared laser spectroscopy. In practice however, as resolution is increased, a number of operating parameters must be controlled with rapidly increasing care. Refinements of instrumentation over the last few years based on a fuller understanding of these parameters has led not only to excellent realizations of resolution but also to greater precision in observed line shapes, line intensities and frequency calibration. In FT Spectroscopy, higher resolution is achieved by recording the interferogram over increasingly greater mirror displacement or optical path difference. While the optical path difference is increased, it is necessary to maintain a high level of consistency of interferometer alignment, path difference measurement and path difference consistency for all optical rays going through the interferometer.
{"title":"Recent Advances in High Resolution Fourier Transform Spectroscopy","authors":"H. Buijs","doi":"10.1364/hrfts.1989.tub2","DOIUrl":"https://doi.org/10.1364/hrfts.1989.tub2","url":null,"abstract":"Fourier Transform Spectroscopy is now widely used in many routine measurement applications. In principle, very high resolution can be achieved in FT Spectroscopy rivaling the resolution of infrared laser spectroscopy. In practice however, as resolution is increased, a number of operating parameters must be controlled with rapidly increasing care. Refinements of instrumentation over the last few years based on a fuller understanding of these parameters has led not only to excellent realizations of resolution but also to greater precision in observed line shapes, line intensities and frequency calibration. In FT Spectroscopy, higher resolution is achieved by recording the interferogram over increasingly greater mirror displacement or optical path difference. While the optical path difference is increased, it is necessary to maintain a high level of consistency of interferometer alignment, path difference measurement and path difference consistency for all optical rays going through the interferometer.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"51 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121447091","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
R. Engleman, C. Brazier, C. Frum, A. Lee, N. Oliphant, P. Bernath, J. Brault
A number of high resolution spectra of different CN violet sources have been obtained with the Kitt Peak Fourier transform spectrometer. These sources fall into four classes.
用基特峰傅立叶变换光谱仪获得了不同CN紫外光源的高分辨光谱。这些来源可分为四类。
{"title":"High Resolution Spectroscopy of the CN Violet System","authors":"R. Engleman, C. Brazier, C. Frum, A. Lee, N. Oliphant, P. Bernath, J. Brault","doi":"10.1364/hrfts.1989.wb5","DOIUrl":"https://doi.org/10.1364/hrfts.1989.wb5","url":null,"abstract":"A number of high resolution spectra of different CN violet sources have been obtained with the Kitt Peak Fourier transform spectrometer. These sources fall into four classes.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"462 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116185731","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This paper gives some of the interesting results from three projects that involve Fourier Transform Spectroscopy (FTS) measurements, studies of molecules involved in atmospheric chemistry, high temperature studies, and the compilation of data for wavenumber calibration of infrared instrumentation. Earlier work on these projects was conducted with a tunable diode laser, now many of the measurements are made with a FTS spectrometer. The FTS instrument is not as sensitive as the diode laser spectrometer, nor does it give as high resolution, but it has the advantage of conveniently and quickly giving broad band spectra with thousands of absorption lines.
{"title":"Fourier Transform Infrared Spectroscopy at the NIST: High Temperature Molecules and Atmospheric Molecules","authors":"A. Maki","doi":"10.1364/hrfts.1989.wb3","DOIUrl":"https://doi.org/10.1364/hrfts.1989.wb3","url":null,"abstract":"This paper gives some of the interesting results from three projects that involve Fourier Transform Spectroscopy (FTS) measurements, studies of molecules involved in atmospheric chemistry, high temperature studies, and the compilation of data for wavenumber calibration of infrared instrumentation. Earlier work on these projects was conducted with a tunable diode laser, now many of the measurements are made with a FTS spectrometer. The FTS instrument is not as sensitive as the diode laser spectrometer, nor does it give as high resolution, but it has the advantage of conveniently and quickly giving broad band spectra with thousands of absorption lines.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116373334","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Raman spectra of molecules in the gasphase yield information about the energy of the rotational and the rotational-vibrational states. This information may more easily be obtained from absorption spectroscopy in the microwave and infrared region, but the less restricted selection rules governing the Raman transitions yield information not measureable in absorption.
{"title":"High Resolution Fourier Transform Raman Spectroscopy of Gases","authors":"J. Bendtsen","doi":"10.1364/hrfts.1989.tua1","DOIUrl":"https://doi.org/10.1364/hrfts.1989.tua1","url":null,"abstract":"Raman spectra of molecules in the gasphase yield information about the energy of the rotational and the rotational-vibrational states. This information may more easily be obtained from absorption spectroscopy in the microwave and infrared region, but the less restricted selection rules governing the Raman transitions yield information not measureable in absorption.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"66 3 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131660788","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The accuracy of the wavenumber measurements is often not as good as the level of their precision. To get better absolute line positions and to have this new advantage widely spread among all FT users, the need of a grid of consistent and accurate wavenumber standards is necessary. We review the present situation.
{"title":"Wavenumber Standards","authors":"Q. Kou, G. Guelachvili","doi":"10.1364/hrfts.1992.thc2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.thc2","url":null,"abstract":"The accuracy of the wavenumber measurements is often not as good as the level of their precision. To get better absolute line positions and to have this new advantage widely spread among all FT users, the need of a grid of consistent and accurate wavenumber standards is necessary. We review the present situation.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"52 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133701075","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The gas phase spectrum of the methyl nitrene radical was first observed by Carrick and Engleking1and subsequently the first rotationally resolved spectrum was obtained by Carrick et al.2The use of the Kitt Peak Fourier transform spectrometer, to detect the emission from a corona excited supersonic expansion of methyl azaide in helium, yielded a rotationally resolved spectrum limited by Doppler broadening of 0.02 cm-1. The transition, assigned as A ˜ 3 E- X ˜ 3 A 2 analagous to the A3∏ −X3∑−band of NH, was still extremely complicated however. Due to the case (a) - case (b) nature of the transition 27 branches are allowed for each subband. Giving a total of 81 branches for the 0-1, 1-0 and 1-2 subbands, the only ones likely to be populated at 15 K the observed rotational temperature. Hence the observed transition is a many line spectrum with few branches discernable.
甲基硝基自由基的气相光谱首先由Carrick和engleking1观察到，随后由Carrick等人获得了第一个旋转分辨光谱2。使用基特峰傅立叶变换光谱仪，检测由日冕激发的azaide甲基在氦中的超音速膨胀产生的发射，得到了一个旋转分辨光谱，其多普勒增宽限制为0.02 cm-1。然而，与nh3∏−X3∑−带类似的A ~ 3e - X ~ 3a2的过渡仍然非常复杂。由于情况(a) -情况(b)的性质，每个子带允许有27个分支。0- 1,1 -0和1-2子带共有81个分支，唯一可能在观测到的旋转温度15 K时填充的分支。因此，观测到的跃迁是一个多谱线光谱，只有很少的分支可识别。
{"title":"Fourier Transform Observation of Jet Cooled Emission from the CH3N and CCN radicals","authors":"C. Brazier, P. Carrick, N. Oliphant, P. Bernath","doi":"10.1364/hrfts.1989.wa5","DOIUrl":"https://doi.org/10.1364/hrfts.1989.wa5","url":null,"abstract":"The gas phase spectrum of the methyl nitrene radical was first observed by Carrick and Engleking1and subsequently the first rotationally resolved spectrum was obtained by Carrick et al.2The use of the Kitt Peak Fourier transform spectrometer, to detect the emission from a corona excited supersonic expansion of methyl azaide in helium, yielded a rotationally resolved spectrum limited by Doppler broadening of 0.02 cm-1. The transition, assigned as \u0000 \u0000 \u0000 \u0000 \u0000 \u0000 A\u0000 ˜\u0000 \u0000 \u0000 3\u0000 \u0000 \u0000 \u0000 \u0000 E-\u0000 \u0000 X\u0000 ˜\u0000 \u0000 \u0000 \u0000 3\u0000 \u0000 \u0000 A\u0000 2\u0000 \u0000 \u0000 \u0000 analagous to the A3∏ −X3∑−band of NH, was still extremely complicated however. Due to the case (a) - case (b) nature of the transition 27 branches are allowed for each subband. Giving a total of 81 branches for the 0-1, 1-0 and 1-2 subbands, the only ones likely to be populated at 15 K the observed rotational temperature. Hence the observed transition is a many line spectrum with few branches discernable.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"49 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132490922","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
I. Nolt, J. Park, M. Vanek, D. Jennings, F. Mencaraglia, B. Carli, M. Poggesi, E. Rossi, M. Carlotti, J. Radostitz
High resolution measurements of the far infrared emission spectrum of the stratosphere were first obtained in 1978 following the Italian development of a balloon-borne Fourier transform spectrometer which used new HeNe laser technology to achieve an FTI mirror stroke of 75 cm. In four flights between 1978 and 1983, this instrument provided the highest resolution measurements for validating spectral database models of the far infrared atmospheric emission1, and for retrieving a number of important stratospheric trace species2. In 1988, an International Cooperative Program was instituted by NASA and the Italian Space Agency for the purpose of upgrading the performance of this instrument for use in the Correlative Measurement Program of the Upper Atmosphere Research Satellite.
{"title":"High Resolution Spectra of Stratospheric Emission in the Spectral Range of 35 to 130 cm-1","authors":"I. Nolt, J. Park, M. Vanek, D. Jennings, F. Mencaraglia, B. Carli, M. Poggesi, E. Rossi, M. Carlotti, J. Radostitz","doi":"10.1364/hrfts.1992.fd2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fd2","url":null,"abstract":"High resolution measurements of the far infrared emission spectrum of the stratosphere were first obtained in 1978 following the Italian development of a balloon-borne Fourier transform spectrometer which used new HeNe laser technology to achieve an FTI mirror stroke of 75 cm. In four flights between 1978 and 1983, this instrument provided the highest resolution measurements for validating spectral database models of the far infrared atmospheric emission1, and for retrieving a number of important stratospheric trace species2. In 1988, an International Cooperative Program was instituted by NASA and the Italian Space Agency for the purpose of upgrading the performance of this instrument for use in the Correlative Measurement Program of the Upper Atmosphere Research Satellite.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"314 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132682933","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
High resolution Fourier transform spectra of suitable sources, such as hollow cathodes and electrodeless discharge lamps, can yield much accurate data on energy levels, isotope shifts, hyperfine splittings. and other parameters for atoms throughout the periodic table. The great dynamic range and linearity of FT spectra (and the availability of fast computers) allows the use of data reduction techniques generally unusable with more conventional photographic grating spectra. The details of producing atomic Fourier transform spectra can be found in the literature.
{"title":"Energy levels, isotope shifts, and hyperfine splittings from Fourier transform atomic spectra.","authors":"R. Engleman","doi":"10.1364/hrfts.1992.fa1","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fa1","url":null,"abstract":"High resolution Fourier transform spectra of suitable sources, such as hollow cathodes and electrodeless discharge lamps, can yield much accurate data on energy levels, isotope shifts, hyperfine splittings. and other parameters for atoms throughout the periodic table. The great dynamic range and linearity of FT spectra (and the availability of fast computers) allows the use of data reduction techniques generally unusable with more conventional photographic grating spectra. The details of producing atomic Fourier transform spectra can be found in the literature.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"129888404","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The emission spectra of Dy, Er, and Gd are reported for the infra-red region 1.1 to 5.4 microns, 8940 to 1835 cm-1. Two sources, a water cooled hollow cathode and an electrodeless discharge lamp, were employed. The spectra were recorded using the National Solar Observatory McMath lm Fourier transform spectrometer (FTS) at Kitt Peak, AZ over the spectral region of 40 000 to 1817 cm-1. Improved frequencies are possible by calibration using argon lines and the frequencies of argon reported by Norlen1. The energy levels published2 in NSRDS-NBS 60 were used to calculate all possible transition energies. These energy values were then matched with the observed frequencies. The neutral (I) and singly ionized atom (II) frequencies were calculated and matched.
{"title":"The infra-red spectra of dysprosium, erbium and gadolinium in the 1.1 to 5.4 micron region*","authors":"J. Conway, E. Worden","doi":"10.1364/hrfts.1992.thd7","DOIUrl":"https://doi.org/10.1364/hrfts.1992.thd7","url":null,"abstract":"The emission spectra of Dy, Er, and Gd are reported for the infra-red region 1.1 to 5.4 microns, 8940 to 1835 cm-1. Two sources, a water cooled hollow cathode and an electrodeless discharge lamp, were employed. The spectra were recorded using the National Solar Observatory McMath lm Fourier transform spectrometer (FTS) at Kitt Peak, AZ over the spectral region of 40 000 to 1817 cm-1. Improved frequencies are possible by calibration using argon lines and the frequencies of argon reported by Norlen1. The energy levels published2 in NSRDS-NBS 60 were used to calculate all possible transition energies. These energy values were then matched with the observed frequencies. The neutral (I) and singly ionized atom (II) frequencies were calculated and matched.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"4 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114648855","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The infrared ro-vibration spectrum of carbon monoxide provides a powerful observational diagnostic for the investigation of late-type stellar atmospheres. At temperatures of several thousands of degrees, CO vibrational states up to v=7 and rotational states up to j≈100 are populated. The corresponding lines are formed over, and therefore probe, a large range in altitude. The strongest fundamental lines (Δv=1) originate in the upper photosphere and in the chromosphere, regions which are only inadequately described by present stellar atmosphere theories. Numerical simulations have shown that CO affects the stellar atmospheric structure through cooling in optically thin lines (e.g. Johnson, 1973). CO observations are important, because the model predictions can be tested reliably only from observations of species that are intimately involved. This is particularly true in view of the dilemma posed by the contradicting results of 'conventional' chromospheric diagnostics and first CO Δv=1 observations on the Sun (Ayres and Testerman, 1981) and Arcturus (Heasley et al., 1978). The present study has been conducted to establish CO fundamental bands as an observational diagnostic for the higher layers of cool stellar atmospheres.
一氧化碳的红外无振动谱为研究晚期恒星大气提供了有力的观测诊断。在几千度的温度下，CO的振动态高达v=7，旋转态高达j≈100。相应的线是在一个很大的高度范围内形成的，因此可以探测到。最强的基本线(Δv=1)起源于上层光球层和色球层，这是目前恒星大气理论所不能充分描述的区域。数值模拟表明，CO通过光学细线的冷却作用影响恒星大气结构(例如Johnson, 1973)。CO观测很重要，因为只有通过对密切相关的物种的观测才能可靠地检验模式预测。考虑到“传统”色球诊断和对太阳(Ayres and Testerman, 1981)和大角星(Heasley et al.， 1978) CO Δv=1观测的矛盾结果所造成的困境，这一点尤其正确。本研究的目的是建立CO基本波段，作为低温恒星大气高层的观测诊断。
{"title":"FTS Observation of CO Fundamental Bands in Cool Stellar Atmospheres","authors":"G. Wiedemann, T. Ayres, D. Jennings","doi":"10.1364/hrfts.1989.mb4","DOIUrl":"https://doi.org/10.1364/hrfts.1989.mb4","url":null,"abstract":"The infrared ro-vibration spectrum of carbon monoxide provides a powerful observational diagnostic for the investigation of late-type stellar atmospheres. At temperatures of several thousands of degrees, CO vibrational states up to v=7 and rotational states up to j≈100 are populated. The corresponding lines are formed over, and therefore probe, a large range in altitude. The strongest fundamental lines (Δv=1) originate in the upper photosphere and in the chromosphere, regions which are only inadequately described by present stellar atmosphere theories. Numerical simulations have shown that CO affects the stellar atmospheric structure through cooling in optically thin lines (e.g. Johnson, 1973). CO observations are important, because the model predictions can be tested reliably only from observations of species that are intimately involved. This is particularly true in view of the dilemma posed by the contradicting results of 'conventional' chromospheric diagnostics and first CO Δv=1 observations on the Sun (Ayres and Testerman, 1981) and Arcturus (Heasley et al., 1978). The present study has been conducted to establish CO fundamental bands as an observational diagnostic for the higher layers of cool stellar atmospheres.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"64 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114767329","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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