Signal-to-Noise Ratio Characteristics of an Inductively Coupled Plasma/Fourier Transform Spectrometer

1986 ◽  
Vol 40 (6) ◽  
pp. 804-813 ◽  
Author(s):  
S. Marra ◽  
G. Horlick
Keyword(s):  
Fourier Transform ◽  
Inductively Coupled Plasma ◽  
Signal To Noise Ratio ◽  
Emission Spectra ◽  
Atomic Emission ◽  
Emission Spectrometry ◽  
Fourier Transform Spectrometer ◽  
Signal To Noise ◽  
Inductively Coupled ◽  
Noise Ratio

Inductively coupled plasma/Fourier transform spectroscopy (ICP-FTS) has the potential to become an excellent combined technique for analytical atomic emission spectrometry. However, the noise performance and behavior of a Fourier transform spectrometer for the measurement of atomic emission spectra in the ultraviolet spectral region is not well understood or characterized. In this study the noise behavior of ICP-FTS is empirically evaluated. The key empirical measurement carried out is the evaluation of complete standard deviation and signal-to-noise ratio spectra (i.e., those parameters measured as a function of wavenumber). A study of these spectra, along with the corresponding emission spectra as a function of concentration and matrix, allows an assessment of noise distribution, multiplex advantage/disadvantage, the nature of the limiting noise, detection limits, and precision.

Fourier Deconvolution of Overlapping Line Pairs in Inductively Coupled Plasma-Atomic Emission Spectrometry

1989 ◽  
Vol 43 (1) ◽  
pp. 96-103 ◽  
Author(s):  
Eric H. Van Veen ◽  
M. Pieter Goudzwaard ◽  
Margaretha T. C. De Loos-Vollebregt ◽  
Leo De Galan
Keyword(s):  
Inductively Coupled Plasma ◽  
Gaussian Approximation ◽  
Signal To Noise Ratio ◽  
Detection Limits ◽  
Atomic Emission ◽  
Emission Lines ◽  
Emission Spectrometry ◽  
Plasma Atomic Emission Spectrometry ◽  
Spectral Window ◽  
Inductively Coupled

A deconvolution procedure utilizing Fourier transformation has been developed to reduce line overlap in ICP-AES. Line broadening is caused by physical processes and by instrumental broadening. Convenient deconvolution, however, turns out to be restricted to broadening common to the emission lines in the spectral window, i.e., to instrumental broadening. Deconvolution for the “true” instrumental broadening function and for a Gaussian approximation to this function yields similar results, but the former allows for fast automated data processing with regard to any spectral region and sample composition. A straightforward procedure is reported for the determination of this function independent of wavelength. At the present noise level, a twofold reduction in linewidth can be achieved for emission lines having a small physical width in comparison to the instrumental width. With data acquired from both a high- and a medium-resolution monochromator, results from overlapping line pairs show linear analytical curves and improved detection limits. Due to the decrease in signal-to-noise ratio on deconvolution, the detection limits measured for isolated lines cannot be attained.

scholarly journals A New Multichannel Fourier Transform Spectrometer

1999 ◽  
Vol 170 ◽  
pp. 36-40
Author(s):  
Tyler E. Nordgren ◽  
Arsen R. Hajian
Keyword(s):  
Fourier Transform ◽  
Extrasolar Planets ◽  
Signal To Noise Ratio ◽  
Fourier Transform Spectrometer ◽  
Test Bed ◽  
Signal To Noise ◽  
Stellar Spectra ◽  
Band Emission ◽  
Noise Ratio ◽  
Ratio Scales

AbstractStellar spectra have been obtained using a multichannel Fourier Transform Spectrometer (FTS) which incorporates components of the Navy Prototype Optical Interferometer. It is well known that a FTS can provide superior wavelength stability as compared to traditional spectrometers. Unfortunately the FTS traditionally suffers from exceptionally poor sensitivity, which until now has limited its uses to sources with high fluxes and/or those with narrow band emission (e.g. the Sun, nebulae, and laboratory samples). We present stellar observations using a new FTS design which overcomes this sensitivity limitation by using a conventional multichannel spectrometer in conjunction with the FTS system. The signal-to-noise ratio of spectra from our test-bed observations are consistent with the theoretical prediction and show that for N channels the sensitivity scales like N, while the signal-to-noise ratio scales like . With this type of an instrument on a 3-m telescope and 9 000 channels we expect to be able to detect and measure such exciting astrophysical phenomenon as gravitational redshifts from single, main sequence stars and extrasolar planets of terrestrial mass.

The Effect of Integration Time and Interval on Precision with Three Pneumatic Nebulizers Used for Inductively Coupled Plasma Atomic Emission Spectrometry

1985 ◽  
Vol 39 (6) ◽  
pp. 989-993 ◽  
Author(s):  
S. W. McGeorge ◽  
E. D. Salin
Keyword(s):  
Inductively Coupled Plasma ◽  
Signal To Noise Ratio ◽  
Atomic Emission ◽  
Emission Spectrometry ◽  
Integration Time ◽  
Plasma Atomic Emission Spectrometry ◽  
Inductively Coupled ◽  
Relative Standard ◽  
Clearing Time ◽  
Long Term Behavior

The long-term behavior of three popular pneumatic nebulizers was observed and compared, with particular attention given to signal-to-noise ratio. Results indicate that sample changeover time and, consequently, spray-chamber clearing time, should be as short as possible. Precision varied widely for each nebulizer depending on the interval between data values. Integration times as short as 0.1 s can yield relative standard deviations of about 1%. Each of the nebulizers was capable of delivering better than 1% RSD, and two provided RSDs less than 0.4% under certain conditions. The implications of these measurements on instrument and experiment design are discussed.

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