Abstract

A method for the compensation of a variable light source in photoelectric spectrophotometry is presented. The outputs of a scanning photo-cell and a monitoring cell are fed to two amplifiers. The outputs of these amplifiers are then fed to a self-balancing recording potentiometer. The equipment has laboratory as well as astrophysical applications. The limiting magnitude at which useful spectrophotometry with a resolution of 1A is approximately 4. Further development work is in progress.

© 1950 Optical Society of America

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References

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  1. G. Van Biesbroeck, McDonald Observatory Contribution No. 1, 103 (1936).
  2. G. Kron, Electronics 21, 103 (1948).
  3. , Vacuum Tube Amplifiers, p. 480.
  4. Dieke and Crosswhite, J. Opt. Soc. Am. 35, 480 (1945).

1948 (1)

G. Kron, Electronics 21, 103 (1948).

1945 (1)

Dieke and Crosswhite, J. Opt. Soc. Am. 35, 480 (1945).

1936 (1)

G. Van Biesbroeck, McDonald Observatory Contribution No. 1, 103 (1936).

Crosswhite,

Dieke and Crosswhite, J. Opt. Soc. Am. 35, 480 (1945).

Dieke,

Dieke and Crosswhite, J. Opt. Soc. Am. 35, 480 (1945).

Kron, G.

G. Kron, Electronics 21, 103 (1948).

Van Biesbroeck, G.

G. Van Biesbroeck, McDonald Observatory Contribution No. 1, 103 (1936).

Electronics (1)

G. Kron, Electronics 21, 103 (1948).

J. Opt. Soc. Am. (1)

Dieke and Crosswhite, J. Opt. Soc. Am. 35, 480 (1945).

McDonald Observatory Contribution No. 1 (1)

G. Van Biesbroeck, McDonald Observatory Contribution No. 1, 103 (1936).

Other (1)

, Vacuum Tube Amplifiers, p. 480.

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Figures (4)

Fig. 1
Fig. 1

Fluctuations in the transmission of a narrow slit caused by variations in the seeing disk. The tracing on the right shows the constancy of a stellar image when the entrance slit of the spectrograph is sufficiently wide to pass the entire stellar image. The tracing on the left shows the variation of the transmitted light when the slit is of such width that only 14 percent of the total light is transmitted. Cassegrain focus of 82-inch reflector of the McDonald Observatory.

Fig. 2
Fig. 2

Schematic diagram of the electrical circuit employed for the compensation of seeing.

Fig. 3
Fig. 3

Schematic diagram of the optical system employed for the photoelectric scanning of stellar spectra.

Fig. 4
Fig. 4

The tracing to the right again shows seeing fluctuations while in the center figure are the same fluctuations when compensated for by the apparatus described in the text. The figure to the left is a tracing of Hγ in αCMa. Coudé focus of 82-inch reflector of the McDonald Observatory.

Equations (4)

Equations on this page are rendered with MathJax. Learn more.

e = i r = ( b E c / R ) r .
( b E c / R ) r = a E 1 .
a E 1 / b E c = r / R .
I 1 / I c = r / R .