Isotope shift measurements in the 660 spectral lines of Er I covering the 340–605 nm wavelength region with a Fourier Transform Spectrometer

The high-resolution infrared spectrum of BrCl has been observed with a Fourier transform spectrometer. About 850 spectral lines for the Δν = 1 sequences of the four isotopic species, 79Br35Cl, 81Br35Cl, 79Br37Cl, and 81Br37Cl have been measured between 417 and 461 cm−1. They have been fitted with a standard deviation of 0.000 146 cm−1 to a Dunham potential function using eight coefficients that included two Watson-type Δ correction terms. Dunham Yij coefficients have been derived for each of the four isotopic species. The equilibrium internuclear distance re of BrCl is 2.136 053 28 (67) Å.

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The Herschel SPIRE Fourier Transform Spectrometer Spectral Feature Finder – III. Line identification and off-axis spectra

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1613 ◽

2020 ◽

Vol 496 (4) ◽

pp. 4906-4922 ◽

Cited By ~ 4

Author(s):

Chris S Benson ◽

N Hładczuk ◽

L D Spencer ◽

A Robb ◽

J Scott ◽

...

Keyword(s):

Fourier Transform ◽

Signal To Noise Ratio ◽

European Space Agency ◽

Spectral Feature ◽

Spectral Lines ◽

Spectral Features ◽

Fourier Transform Spectrometer ◽

Line Identification ◽

Space Agency ◽

Feature Fitting

ABSTRACT The European Space Agency Herschel Spectral and Photometric Imaging Receiver (SPIRE) Fourier Transform Spectrometer (FTS) Spectral Feature Finder (FF) project is an automated spectral feature fitting routine developed within the SPIRE instrument team to extract all prominent spectral features from all publicly available SPIRE FTS observations. We present the extension of the FF to include the off-axis detectors of the FTS in sparsely sampled single-pointing observations, the results of which have been ingested into the catalogue. We also present the results from an automated routine for identifications of the atomic/molecular transitions that correspond to the spectral features extracted by the FF. We use a template of 307 atomic fine structure and molecular lines that are commonly found in SPIRE FTS spectra for the cross-match. The routine makes use of information provided by the line identification to search for low signal-to-noise ratio features that have been excluded or missed by the iterative FF. In total, the atomic/molecular transitions of 178 942 lines are identified (corresponding to 83 per cent of the entire FF catalogue), and an additional 33 840 spectral lines associated with missing features from SPIRE FTS observations are added to the FF catalogue.

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Climate Absolute Radiance and Refractivity Observatory (CLARREO)

ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences ◽

10.5194/isprsarchives-xl-7-w3-213-2015 ◽

2015 ◽

Vol XL-7/W3 ◽

pp. 213-217 ◽

Cited By ~ 3

Author(s):

J. Leckey

Keyword(s):

Climate Change ◽

Fourier Transform ◽

Phase Change ◽

Radio Occultation ◽

Wavelength Region ◽

Sufficient Accuracy ◽

Fourier Transform Spectrometer ◽

Climate Variables ◽

The Status ◽

Order Of Magnitude

The Climate Absolute Radiance and Refractivity Observatory (CLARREO) is a mission, led and developed by NASA, that will measure a variety of climate variables with an unprecedented accuracy to quantify and attribute climate change. CLARREO consists of three separate instruments: an infrared (IR) spectrometer, a reflected solar (RS) spectrometer, and a radio occultation (RO) instrument. The mission will contain orbiting radiometers with sufficient accuracy, including on orbit verification, to calibrate other space-based instrumentation, increasing their respective accuracy by as much as an order of magnitude. The IR spectrometer is a Fourier Transform spectrometer (FTS) working in the 5 to 50 μm wavelength region with a goal of 0.1 K (<i>k</i> = 3) accuracy. The FTS will achieve this accuracy using phase change cells to verify thermistor accuracy and heated halos to verify blackbody emissivity, both on orbit. The RS spectrometer will measure the reflectance of the atmosphere in the 0.32 to 2.3 μm wavelength region with an accuracy of 0.3% (<i>k</i> = 2). The status of the instrumentation packages and potential mission options will be presented.

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The Berkeley Program on Molecules of Astrophysical Interest

International Astronomical Union Colloquium ◽

10.1017/s0252921100021485 ◽

1994 ◽

Vol 146 ◽

pp. 397-411

Author(s):

Sumner P. Davis

Keyword(s):

Fourier Transform ◽

Spectral Lines ◽

Carbon Clusters ◽

Molecular Spectra ◽

Fourier Transform Spectrometer ◽

Excitation Energies ◽

Astrophysical Interest ◽

Computer Codes ◽

The Fourier Transform ◽

Systematic Program

A systematic program of laboratory analyses of selected molecular spectra of astrophysical interest started in 1958 and continues to the present time. The program includes production of spectral atlases, tabulations of spectral lines, analyses, calculations of excitation energies and molecular parameters, measurements of radiative lifetimes, and determinations of transition strengths. Work has been completed or is in progress on the spectra of ArH+, C2, carbon clusters, CN, CS, CaCl, CaH, CaS, FeD, FeH, HgH, HgD, InI, LaO, LaS, OD, OH, SH, Si2, SiC2, TiCl, TiO, TiO+, VO, YS, ZrCl, ZrO, and ZrS. The basic needs for astronomically useful data have not changed, but laboratory and analysis methods have become more sophisticated in order to cope with ever greater demands for consistency, accuracy, and breadth of information. The Fourier transform spectrometer and computer codes for analyses have enhanced our ability to satisfy some of these demands.

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