Infrared molecular and atomic lines in planets, stars, and dust clouds can only be resolved using the highest available spectral resolution. The Fourier transform spectrometer is presently the only type of spectrometer capable of resolving powers near 105 which can operate at arbitrary wavelengths in the infrared. However, because noise in a spectrum increases with resolution, working at high resolution requires maximum sensitivity. In the thermal infrared, radiation from the sky and warm optics is the dominant source of noise in a spectrum. In order to achieve 105 resolving power on even the brightest sources in the mid-infrared, special techniques must be used to minimize background radiation.
{"title":"High Resolution FTS in Astronomy at 7 to 15 Microns","authors":"D. Jennings","doi":"10.1364/hrfts.1989.wa3","DOIUrl":"https://doi.org/10.1364/hrfts.1989.wa3","url":null,"abstract":"Infrared molecular and atomic lines in planets, stars, and dust clouds can only be resolved using the highest available spectral resolution. The Fourier transform spectrometer is presently the only type of spectrometer capable of resolving powers near 105 which can operate at arbitrary wavelengths in the infrared. However, because noise in a spectrum increases with resolution, working at high resolution requires maximum sensitivity. In the thermal infrared, radiation from the sky and warm optics is the dominant source of noise in a spectrum. In order to achieve 105 resolving power on even the brightest sources in the mid-infrared, special techniques must be used to minimize background radiation.","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":"125438470","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}
In this paper we present the characteristics of the MIPAS instrument, its measurement objectives and several unique features related to high resolution emission measurements.
在本文中，我们介绍了MIPAS仪器的特点，它的测量目标和几个独特的特点有关的高分辨率发射测量。
{"title":"Characteristics of a High Resolution Fourier Transform Spectrometer to Measure Atmospheric Gas Species in Emission from Space: the MIPAS Mission","authors":"D. Lamarre, J. Giroux, H. Buijs","doi":"10.1364/hrfts.1992.fd4","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fd4","url":null,"abstract":"In this paper we present the characteristics of the MIPAS instrument, its measurement objectives and several unique features related to high resolution emission measurements.","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":"129626361","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}
Determination of the cosmic abundance of the light elements Li, Be and B is critical for the understanding of how these elements have been formed in the Universe. The Standard Model for the Big Bang nucleosynthesis, which assumes a uniform density, and its complementary model, the Non-uniform Density Model (see e.g. Kajino and Boyd, 1990), differ considerably in their predictions of Be- and B-production . However, recent determinations of the abundance of Be (Gilmore et al. 1991) and B (Duncan et al. 1992) in metal-poor stars are orders of magnitude larger than those predicted from any Big Bang nucleosynthesis model. The isotopes 9Be, 10B and 11B are therefore thought to have been produced by cosmic spallation, primarily when high-energy protons and α-particles collide with CNO nuclei in the interstellar medium.
{"title":"Isotope Shift in B I at 2090 Å as a Probe of Cosmic Nucleosynthesis","authors":"S. Johansson, U. Litzén, Jörg Kasten, M. Kock","doi":"10.1364/hrfts.1992.thd4","DOIUrl":"https://doi.org/10.1364/hrfts.1992.thd4","url":null,"abstract":"Determination of the cosmic abundance of the light elements Li, Be and B is critical for the understanding of how these elements have been formed in the Universe. The Standard Model for the Big Bang nucleosynthesis, which assumes a uniform density, and its complementary model, the Non-uniform Density Model (see e.g. Kajino and Boyd, 1990), differ considerably in their predictions of Be- and B-production . However, recent determinations of the abundance of Be (Gilmore et al. 1991) and B (Duncan et al. 1992) in metal-poor stars are orders of magnitude larger than those predicted from any Big Bang nucleosynthesis model. The isotopes 9Be, 10B and 11B are therefore thought to have been produced by cosmic spallation, primarily when high-energy protons and α-particles collide with CNO nuclei in the interstellar medium.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"19 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":"116540891","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}
A high-resolution interferometer and high-temperature absorption cell have been used in a continuing measurement program of rotation-vibration spectra of the isotopes of carbon dioxide in different spectral regions. This paper covers results for the isotopes 13C16O2 and 16O13C18O with band centers in the spectral region 600 to 800 cm-1. Only a few experimental details will be given here; additional details may be found in the literature.1 The experimental components include an infrared source, a radiation chopper, a high-temperature single-pass gas-sample absorption cell, a Michelson interferometer with "cat’s eye" mirrors employing a step-and-integrate mirror motion, and two liquid-helium-cooled detectors. A carbon dioxide gas sample was contained in the 1.75 meter single-pass stainless-steel sample cell. The central one meter section of the cell was maintained at a temperature of 800K, with temperature gradients in the end segments of the cell, ending with the cell windows at room temperature. For this study a stepping mirror displacement of 75 cm was used, giving a resolution (FWHM) of 0.006 cm-1 with triangular apodization.
{"title":"Band Centers and Line Positions of Hot Bands of 13C16O2 and 16O13C18O in the 15 Micron Region","authors":"M. Esplin, M. Hoke","doi":"10.1364/hrfts.1992.fd6","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fd6","url":null,"abstract":"A high-resolution interferometer and high-temperature absorption cell have been used in a continuing measurement program of rotation-vibration spectra of the isotopes of carbon dioxide in different spectral regions. This paper covers results for the isotopes 13C16O2 and 16O13C18O with band centers in the spectral region 600 to 800 cm-1.\u0000 Only a few experimental details will be given here; additional details may be found in the literature.1 The experimental components include an infrared source, a radiation chopper, a high-temperature single-pass gas-sample absorption cell, a Michelson interferometer with \"cat’s eye\" mirrors employing a step-and-integrate mirror motion, and two liquid-helium-cooled detectors. A carbon dioxide gas sample was contained in the 1.75 meter single-pass stainless-steel sample cell. The central one meter section of the cell was maintained at a temperature of 800K, with temperature gradients in the end segments of the cell, ending with the cell windows at room temperature. For this study a stepping mirror displacement of 75 cm was used, giving a resolution (FWHM) of 0.006 cm-1 with triangular apodization.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"33 6","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132365268","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}
Calcium hydride is an important astrophysical molecule which has been detected in the Sun [1,2] and other stars [3]. It is also believed that this free radical is an important constituent of the interstellar medium [4]. However, a search for the CaH in interstellar medium is hindered by the unavailability of accurate frequencies for the low-N rotational transitions.
{"title":"High Resolution Infrared Fourier Transform Emission Spectroscopy and Rotational Spectroscopy of Metal Hydrides: 2Σ+ State of CaH","authors":"C. Frum, J. Oh, E. Cohen, H. Pickett","doi":"10.1364/hrfts.1992.thd6","DOIUrl":"https://doi.org/10.1364/hrfts.1992.thd6","url":null,"abstract":"Calcium hydride is an important astrophysical molecule which has been detected in the Sun [1,2] and other stars [3]. It is also believed that this free radical is an important constituent of the interstellar medium [4]. However, a search for the CaH in interstellar medium is hindered by the unavailability of accurate frequencies for the low-N rotational transitions.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"10 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":"116480928","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 hydroxyl radical plays an important role in a variety of atmospheric, astrophysical, and chemical processes. Both absorption in, and fluorescence from, the strong (0-0) band of the A2Σ+ - X2∏ system are widely used in concentration measurements of OH (e.g., Stimpfle et al. 1990; Desgroux and Cottereau 1991).
羟基自由基在各种大气、天体物理和化学过程中起着重要作用。A2Σ+ - X2∏系统强(0-0)波段的吸收和荧光均广泛用于OH浓度测量(例如，stimple等人，1990;Desgroux and Cottereau 1991)。
{"title":"Fourier Transform Spectra of the A2Σ+ (v=0) -X2∏ (v=o) Band of OH","authors":"G. Stark, J. Brault, M. Abrams","doi":"10.1364/hrfts.1992.thd2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.thd2","url":null,"abstract":"The hydroxyl radical plays an important role in a variety of atmospheric, astrophysical, and chemical processes. Both absorption in, and fluorescence from, the strong (0-0) band of the A2Σ+ - X2∏ system are widely used in concentration measurements of OH (e.g., Stimpfle et al. 1990; Desgroux and Cottereau 1991).","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"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":"122325807","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}
Until recently, very few measurements of broadening of O3 absorption lines have been made (see Table IV of Ref. 1), covering only about 230 different vibration-rotation lines. However, investigators desiring to accurately model infrared radiative transfer in the terrestrial atmosphere require spectroscopic parameters (including air-broadened halfwidths) for thousands of vibration-rotation lines (2). Self-broadened halfwidths are needed for accurate quantitative analysis of laboratory spectra of gas mixtures containing high concentrations of ozone. In the studies reported here, the broad spectral coverage possible with Fourier transform spectroscopy has enabled us to measure air- and nitrogen-broadened halfwidths and shifts for about 70 ozone lines in the 9 μm region, and self-broadened halfwidths for over 160 ozone lines in the 4-14 μm region. The results are compared with previous measurements and calculations.
{"title":"Fourier-Transform Spectroscopy of Ozone Broadening","authors":"M. A. Smith, C. Rinsland, V. Devi","doi":"10.1364/hrfts.1989.wa7","DOIUrl":"https://doi.org/10.1364/hrfts.1989.wa7","url":null,"abstract":"Until recently, very few measurements of broadening of O3 absorption lines have been made (see Table IV of Ref. 1), covering only about 230 different vibration-rotation lines. However, investigators desiring to accurately model infrared radiative transfer in the terrestrial atmosphere require spectroscopic parameters (including air-broadened halfwidths) for thousands of vibration-rotation lines (2). Self-broadened halfwidths are needed for accurate quantitative analysis of laboratory spectra of gas mixtures containing high concentrations of ozone. In the studies reported here, the broad spectral coverage possible with Fourier transform spectroscopy has enabled us to measure air- and nitrogen-broadened halfwidths and shifts for about 70 ozone lines in the 9 μm region, and self-broadened halfwidths for over 160 ozone lines in the 4-14 μm region. The results are compared with previous measurements and calculations.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"73 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":"127968401","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}
Fourier-transform spectroscopy of the thermal emission spectrum of the Earth’s stratosphere is a technique of growing importance in the study of ozone-layer chemistry. The far-infrared part of this thermal spectrum, here roughly 7-700 cm-1, includes detectable transitions of many species which are key indicators of the degree to which catalytic reactions of chlorine and bromine compounds are able to destroy ozone. A unique advantage of measuring thermal emission is that the instrument can examine the stratosphere at night as easily as it does the day. It is this combination of circumstances, namely the ability to measure species such as OH and HO2, and the ability to measure throughout the day-night cycle, which has made the far-infrared Fourier-transform spectrometer (FTS) a valuable asset in the study of the stratospheric ozone layer.
{"title":"Far-Infrared Fourier-Transform Spectroscopy of the Stratosphere","authors":"W. Traub","doi":"10.1364/hrfts.1992.fc2","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fc2","url":null,"abstract":"Fourier-transform spectroscopy of the thermal emission spectrum of the Earth’s stratosphere is a technique of growing importance in the study of ozone-layer chemistry. The far-infrared part of this thermal spectrum, here roughly 7-700 cm-1, includes detectable transitions of many species which are key indicators of the degree to which catalytic reactions of chlorine and bromine compounds are able to destroy ozone. A unique advantage of measuring thermal emission is that the instrument can examine the stratosphere at night as easily as it does the day. It is this combination of circumstances, namely the ability to measure species such as OH and HO2, and the ability to measure throughout the day-night cycle, which has made the far-infrared Fourier-transform spectrometer (FTS) a valuable asset in the study of the stratospheric ozone layer.","PeriodicalId":159025,"journal":{"name":"High Resolution Fourier Transform Spectroscopy","volume":"32 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":"128435175","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}
For more than 15 years our project in the Atmospheric Chemistry Division of NCAR has flown a Fourier transform spectrometer aboard aircraft to record the infrared absorption spectrum of the stratosphere. These spectra, now totaling more than 45,000, have been used to derive the concentrations of a number of stratospheric gases and to define their latitudinal, seasonal and diurnal variations.
{"title":"Stratospheric Fourier Transform Spectroscopy","authors":"M. Coffey, W. Mankin","doi":"10.1364/hrfts.1992.fd3","DOIUrl":"https://doi.org/10.1364/hrfts.1992.fd3","url":null,"abstract":"For more than 15 years our project in the Atmospheric Chemistry Division of NCAR has flown a Fourier transform spectrometer aboard aircraft to record the infrared absorption spectrum of the stratosphere. These spectra, now totaling more than 45,000, have been used to derive the concentrations of a number of stratospheric gases and to define their latitudinal, seasonal and diurnal variations.","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":"129950632","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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