High resolution laboratory measurements of line positions, strengths, and pressure broadening parameters of atmospheric trace molecules are important for the analysis of atmospheric measurements. Two of the several key molecules involved in this scenario are N2O and H2O. This text describes the laboratory measurements, analysis and results of an extensive study on N2O and H2O infrared spectra. The spectra were obtained with a Fourier-transform spectrometer located in the McMath solar telescope facility at the Kitt Peak National Observatory. The spectral resolution was 0.005 cm-1 for the region below 2200 cm-1 and from 2200 to 8000 cm-1, the resolution was 0.01 cm-1.
{"title":"Laboratory Spectroscopy of H2O and N2O","authors":"R. Toth","doi":"10.1364/hrfts.1992.tha2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.tha2","url":null,"abstract":"High resolution laboratory measurements of line positions, strengths, and pressure broadening parameters of atmospheric trace molecules are important for the analysis of atmospheric measurements. Two of the several key molecules involved in this scenario are N2O and H2O. This text describes the laboratory measurements, analysis and results of an extensive study on N2O and H2O infrared spectra. The spectra were obtained with a Fourier-transform spectrometer located in the McMath solar telescope facility at the Kitt Peak National Observatory. The spectral resolution was 0.005 cm-1 for the region below 2200 cm-1 and from 2200 to 8000 cm-1, the resolution was 0.01 cm-1.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"69 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":"133747874","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}
Current techniques for processing high resolution Fourier transform spectra revolve around interactive graphical display of the spectrum on a computer. The DECOMP spectrum decomposition program is designed explicitly for the reduction of Fourier transform spectra and focuses on reducing a spectrum into a list of line parameters. Basic methods of spectrum manipulation will be demonstrated and a IBM PC - compatible computer will be available for hands-on demonstrations of the process of spectrum analysis. Figures 1 and 2 illustrate the process of background subtraction: in Figure 1 a low resolution spectrum is generated by binning the high resolution spectrum and beneath the spectrum is a background correction function generated by creating a low resolution "minima" spectrum and smoothing the spectrum. The results of the background correction are given in Figure 2. Figure 3 illustrates a common problem in Fourier transform spectroscopy: the finite length of the interferogram introduces "ringing" into the spectrum. Using a filtered fitting routine in DECOMP the ringing can be effectively removed yielding a spectrum illustrated in Figure 4, in which several new spectral features that had been hidden beneath the ringing. An example of the atlas plots that can be generated using DECOMP is given in Figure 5.
{"title":"DECOMP: A Fourier Transfom Spectra Decomposition Program","authors":"Janes W. Brault, M. Abrams","doi":"10.1364/hrfts.1989.pdp2","DOIUrl":"https://doi.org/10.1364/hrfts.1989.pdp2","url":null,"abstract":"Current techniques for processing high resolution Fourier transform spectra revolve around interactive graphical display of the spectrum on a computer. The DECOMP spectrum decomposition program is designed explicitly for the reduction of Fourier transform spectra and focuses on reducing a spectrum into a list of line parameters. Basic methods of spectrum manipulation will be demonstrated and a IBM PC - compatible computer will be available for hands-on demonstrations of the process of spectrum analysis. Figures 1 and 2 illustrate the process of background subtraction: in Figure 1 a low resolution spectrum is generated by binning the high resolution spectrum and beneath the spectrum is a background correction function generated by creating a low resolution \"minima\" spectrum and smoothing the spectrum. The results of the background correction are given in Figure 2. Figure 3 illustrates a common problem in Fourier transform spectroscopy: the finite length of the interferogram introduces \"ringing\" into the spectrum. Using a filtered fitting routine in DECOMP the ringing can be effectively removed yielding a spectrum illustrated in Figure 4, in which several new spectral features that had been hidden beneath the ringing. An example of the atlas plots that can be generated using DECOMP is given in Figure 5.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"126 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":"124451124","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 spectra of unstable species are now being currently recorded with high information Fourier transform interferometers. However to benefit on radical spectra, from the usual well-known advantages of the technique several specific difficulties must be overcome.
{"title":"New Methods in Selective Fourier Transform Spectroscopy","authors":"R. Farrenq, G. Guelachvili","doi":"10.1364/hrfts.1989.ma3","DOIUrl":"https://doi.org/10.1364/hrfts.1989.ma3","url":null,"abstract":"High resolution spectra of unstable species are now being currently recorded with high information Fourier transform interferometers. However to benefit on radical spectra, from the usual well-known advantages of the technique several specific difficulties must be overcome.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"78 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":"114307003","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}
A. Goldman, F. Murcray, R. Blatherwick, F. Murcray, J. Kosters, F. Bonomo, S. David, D. Murcray, C. Rinsland
High resolution (0.002-0.003 cm-1) Michelson type interferometer systems have been used at the University of Denver since 1987 to obtain infrared solar absorption spectra of the stratosphere during several balloon flights (~37 km), as well as ground-based solar spectra and laboratory spectra of molecules of stratospheric and tropospheric interest. The stratospheric spectra cover the 700-2200 cm-1 region and show many new spectral features of important atmospheric gases such as O3 (including 18O and 17O isotopic species), NO2, HNO3, O2, N2, COF2, ClONO2, SF6 and others. The new spectral features are enhanced by the high resolution and long path spectra obtained during sunrise and sunset. Also, new features appear as the concentrations of some trace gases increases in the atmosphere.
{"title":"Recent Results from High Resolution Infrared Atmospheric and Laboratory Fourier Transform Spectra","authors":"A. Goldman, F. Murcray, R. Blatherwick, F. Murcray, J. Kosters, F. Bonomo, S. David, D. Murcray, C. Rinsland","doi":"10.1364/hrfts.1992.fd5","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fd5","url":null,"abstract":"High resolution (0.002-0.003 cm-1) Michelson type interferometer systems have been used at the University of Denver since 1987 to obtain infrared solar absorption spectra of the stratosphere during several balloon flights (~37 km), as well as ground-based solar spectra and laboratory spectra of molecules of stratospheric and tropospheric interest. The stratospheric spectra cover the 700-2200 cm-1 region and show many new spectral features of important atmospheric gases such as O3 (including 18O and 17O isotopic species), NO2, HNO3, O2, N2, COF2, ClONO2, SF6 and others. The new spectral features are enhanced by the high resolution and long path spectra obtained during sunrise and sunset. Also, new features appear as the concentrations of some trace gases increases in the atmosphere.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"22 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":"114310966","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 Air Force Geophysics Laboratory (AFGL) high resolution Michelson interferometer has been used to make measurement of the spectrum of CO2 in the 15 µm region. The infrared spectrum of a linear molecule like CO2 is composed of vibrational bands made up of many nearly equally spaced rotation lines. At high temperatures there is a great deal of overlapping of these bands. This overlapping causes the line density in the experimental spectrum to be very high. Since the band systems are spread over hundreds of wavenumbers, a Michelson interferometer with its capability of high resolution over wide spectral ranges is well suited to high temperature measurements.
{"title":"Hot Bands of Carbon Dioxide in the 15 Micron Region","authors":"M. Esplin, M. Hoke","doi":"10.1364/hrfts.1989.mb5","DOIUrl":"https://doi.org/10.1364/hrfts.1989.mb5","url":null,"abstract":"The Air Force Geophysics Laboratory (AFGL) high resolution Michelson interferometer has been used to make measurement of the spectrum of CO2 in the 15 µm region. The infrared spectrum of a linear molecule like CO2 is composed of vibrational bands made up of many nearly equally spaced rotation lines. At high temperatures there is a great deal of overlapping of these bands. This overlapping causes the line density in the experimental spectrum to be very high. Since the band systems are spread over hundreds of wavenumbers, a Michelson interferometer with its capability of high resolution over wide spectral ranges is well suited to high temperature measurements.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"892 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":"116383262","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 work was undertaken to obtain a reasonably complete list of the Ar lines that appear in hollow-cathode (HC) spectra. The older Ar linelists do not have the precision one wants in analyzing FTS spectra, and the available interferometric values - notably the beautiful Fabry-Perot measurements of Norlen1 - include only a selection of identified lines of wavelength <9800 Å.
{"title":"Making Use of the Argon Lines in Hollow-Cathode Spectra","authors":"W. Whaling, J. Brault","doi":"10.1364/hrfts.1992.thb1","DOIUrl":"https://doi.org/10.1364/hrfts.1992.thb1","url":null,"abstract":"This work was undertaken to obtain a reasonably complete list of the Ar lines that appear in hollow-cathode (HC) spectra. The older Ar linelists do not have the precision one wants in analyzing FTS spectra, and the available interferometric values - notably the beautiful Fabry-Perot measurements of Norlen1 - include only a selection of identified lines of wavelength <9800 Å.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"274 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":"121913459","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}
Our studies at Lawrence Livermore National Laboratory (LLNL) of lanthanide and actinide spectra with the Kitt Peak National Solar Observatory (KPNO) 1 m Fourier transform spectrometer (FTS) have included both intensity for branching ratio (BR) determination (transition probability) and frequency observations using hollow cathodes (HC) and/or electrodeless discharge lamps (EDLs) as sources. The elements we have observed, the purpose of the study and the sources used are given in Table 1.
{"title":"Transition probabilities using branching ratios determined with the Kitt Peak FTS lifetimes obtained by laser and other techniques - lanthanides and U II.*","authors":"E. Worden, J. Conway","doi":"10.1364/hrfts.1992.fa2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fa2","url":null,"abstract":"Our studies at Lawrence Livermore National Laboratory (LLNL) of lanthanide and actinide spectra with the Kitt Peak National Solar Observatory (KPNO) 1 m Fourier transform spectrometer (FTS) have included both intensity for branching ratio (BR) determination (transition probability) and frequency observations using hollow cathodes (HC) and/or electrodeless discharge lamps (EDLs) as sources. The elements we have observed, the purpose of the study and the sources used are given in Table 1.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"63 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":"129245151","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 concepts of VUV FTS and imaging FTS have become somewhat linked by studies of the feasibility of a satellite-borne imaging FTS combining spectral and spatial resolution, primarily for solar physics. In the recent ESA study (SIMURIS) the main target of such an instrument is the chromospheric emission spectrum from the end of the continuum, about 180 nm, to Lyman alpha at 121 nm. Instrumentally, however, the two concepts are almost independent. I shall treat them as such in this paper, but I will conclude it with a brief discussion of the merits of an imaging FTS relative to those of a grating spectrometer equipped with a similar array detector.
{"title":"VUV Fourier transform spectroscopy (with imaging)","authors":"A. Thorne","doi":"10.1364/hrfts.1992.sab2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.sab2","url":null,"abstract":"The concepts of VUV FTS and imaging FTS have become somewhat linked by studies of the feasibility of a satellite-borne imaging FTS combining spectral and spatial resolution, primarily for solar physics. In the recent ESA study (SIMURIS) the main target of such an instrument is the chromospheric emission spectrum from the end of the continuum, about 180 nm, to Lyman alpha at 121 nm. Instrumentally, however, the two concepts are almost independent. I shall treat them as such in this paper, but I will conclude it with a brief discussion of the merits of an imaging FTS relative to those of a grating spectrometer equipped with a similar array detector.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"16 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":"126751719","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}
A new, compact Fourier Transform Michelson UV-visible interferometer (FTUV) with an apodized resolving power greater than 300,000 at 300nm, high throughput, and wide spectral coverage has been developed. This instrument features a flex pivot swing carriage mechanism driven by a voice coil actuator to achieve essentially frictionless motion with high mirror velocity stability. Small residual alignment errors are corrected dynamically to 0.1μrad using a servo-controlled piezo-electric driven mirror tilt mechanism. The instrument is designed for high resolution laboratory and atmospheric detection and spectroscopy of reactive radicals and molecules.
{"title":"A Compact, High Resolution Fourier Transform Interferometer for Atmospheric Spectroscopy in the Near Ultraviolet","authors":"R. Cageao, S. Sander, R. Friedl","doi":"10.1364/hrfts.1992.fd8","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fd8","url":null,"abstract":"A new, compact Fourier Transform Michelson UV-visible interferometer (FTUV) with an apodized resolving power greater than 300,000 at 300nm, high throughput, and wide spectral coverage has been developed. This instrument features a flex pivot swing carriage mechanism driven by a voice coil actuator to achieve essentially frictionless motion with high mirror velocity stability. Small residual alignment errors are corrected dynamically to 0.1μrad using a servo-controlled piezo-electric driven mirror tilt mechanism. The instrument is designed for high resolution laboratory and atmospheric detection and spectroscopy of reactive radicals and molecules.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"152 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":"133123563","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}
Modern telescopes make it possible to obtain spectra in high resolution (Δ/Δλ ≈ 100000) and high signal-to-noise ratio from 120 nm to 5 μm for hundreds of thousands of stars in our own Galaxy. The high accuracy obtainable in these observations puts very strong qualitative and quantitative requirements on the atomic and molecular data to be used in the analysis. Different types of atomic data are needed, and in this paper we will focus on wavelengths, line identifications and oscillator strengths. We will demonstrate the need for FTS accuracy in wavelengths for direct application to stellar spectra as concerns calibration and line identification. The FTS accuracy is also needed in the analysis of a complex and line-rich spectrum in order to establish the term system, which subsequently also leads to line identifications. We will also discuss the use of FTS-intensities for obtaining experimental branching ratios to compare with observed line absorption in stellar spectra.
{"title":"The Need for FTS Accuracy in the Analysis of Complex Laboratory and Stellar Spectra","authors":"S. Johansson, U. Litzén, D. Leckrone, G. Wahlgren","doi":"10.1364/hrfts.1992.fa3","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fa3","url":null,"abstract":"Modern telescopes make it possible to obtain spectra in high resolution (Δ/Δλ ≈ 100000) and high signal-to-noise ratio from 120 nm to 5 μm for hundreds of thousands of stars in our own Galaxy. The high accuracy obtainable in these observations puts very strong qualitative and quantitative requirements on the atomic and molecular data to be used in the analysis. Different types of atomic data are needed, and in this paper we will focus on wavelengths, line identifications and oscillator strengths. We will demonstrate the need for FTS accuracy in wavelengths for direct application to stellar spectra as concerns calibration and line identification. The FTS accuracy is also needed in the analysis of a complex and line-rich spectrum in order to establish the term system, which subsequently also leads to line identifications. We will also discuss the use of FTS-intensities for obtaining experimental branching ratios to compare with observed line absorption in stellar spectra.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"35 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":"131877048","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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