Abstract

A review is given of the factors contributing to the noise and to the limitations in resolving power. Their mutual dependance is expressed in simple formulas.

The factors contributing to the limitations in resolving power at infinitely narrow slits are discussed in detail. Their sum is approximated by a Gauss curve of width s₀. The finite slit width s_g adds to s₀ giving an effective slit width s_eff, where s_eff²=s₀²+s_g². Expressions are given for the energy from the glower traversing the spectroscope and for the noise generated in the detector amplifier system. From these the signal-to-noise ratio and the relative random errors in D due to noise are expressed in terms of s_g, transmittancy of sample, filter time constant, and a few functions characteristic of the spectroscope. Optimal scanning conditions are discussed on this basis. It is shown that s_g in most cases ought to have a magnitude between s₀/2 and s₀.

© 1953 Optical Society of America

Noise Filter Effects in Recording Spectroscopes

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