Abstract

The construction and performance of a rapid scan spectrophotometer is described. The system uses a 1024–channel signal averager to accumulate many rapid spectral scans so as to average out slow changes in sky transparency. Wavelength programming is provided so that multicolor narrow-band photometry is possible in the signal averaging mode. Observations were made using a variety of scan speeds and sky conditions to evaluate the gains in accuracy compared to conventional slow scans. With sufficiently high scan speeds, it is possible to work on partly cloudy nights with only a factor of 2 loss in accuracy.

© 1971 Optical Society of America

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References

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  1. A. D. Code, W. C. Liller, Astronomical Techniques (Univ. of Chicago Press, Chicago, 1960), pp. 281–300.
  2. C. R. Lynds, R. I. Aikens, Publ. Astron. Soc. Pacific 77, 347 (1965).
    [CrossRef]
  3. W. C. Livingston, Appl. Opt. 7, 425 (1968).
    [CrossRef] [PubMed]
  4. D. E. Osterbrock, Astronom. J. 72, 1152 (1967).
    [CrossRef]
  5. J. D. R. Bahng, Bull. American Astronom. Soc. 2, 292 (1970).
  6. D. J. Schroeder, Appl. Opt. 5, 545 (1966).
    [CrossRef] [PubMed]
  7. M. A. Seeds, Ph.D. thesis, Indiana Univ., Bloomington (1970).
  8. A. H. Mikesell, Publ. U.S. Naval Observatory 17, Series 2, Part 4 (1955).

1970 (1)

J. D. R. Bahng, Bull. American Astronom. Soc. 2, 292 (1970).

1968 (1)

1967 (1)

D. E. Osterbrock, Astronom. J. 72, 1152 (1967).
[CrossRef]

1966 (1)

1965 (1)

C. R. Lynds, R. I. Aikens, Publ. Astron. Soc. Pacific 77, 347 (1965).
[CrossRef]

1955 (1)

A. H. Mikesell, Publ. U.S. Naval Observatory 17, Series 2, Part 4 (1955).

Aikens, R. I.

C. R. Lynds, R. I. Aikens, Publ. Astron. Soc. Pacific 77, 347 (1965).
[CrossRef]

Bahng, J. D. R.

J. D. R. Bahng, Bull. American Astronom. Soc. 2, 292 (1970).

Code, A. D.

A. D. Code, W. C. Liller, Astronomical Techniques (Univ. of Chicago Press, Chicago, 1960), pp. 281–300.

Liller, W. C.

A. D. Code, W. C. Liller, Astronomical Techniques (Univ. of Chicago Press, Chicago, 1960), pp. 281–300.

Livingston, W. C.

Lynds, C. R.

C. R. Lynds, R. I. Aikens, Publ. Astron. Soc. Pacific 77, 347 (1965).
[CrossRef]

Mikesell, A. H.

A. H. Mikesell, Publ. U.S. Naval Observatory 17, Series 2, Part 4 (1955).

Osterbrock, D. E.

D. E. Osterbrock, Astronom. J. 72, 1152 (1967).
[CrossRef]

Schroeder, D. J.

Seeds, M. A.

M. A. Seeds, Ph.D. thesis, Indiana Univ., Bloomington (1970).

Appl. Opt. (2)

Astronom. J. (1)

D. E. Osterbrock, Astronom. J. 72, 1152 (1967).
[CrossRef]

Bull. American Astronom. Soc. (1)

J. D. R. Bahng, Bull. American Astronom. Soc. 2, 292 (1970).

Publ. Astron. Soc. Pacific (1)

C. R. Lynds, R. I. Aikens, Publ. Astron. Soc. Pacific 77, 347 (1965).
[CrossRef]

Publ. U.S. Naval Observatory (1)

A. H. Mikesell, Publ. U.S. Naval Observatory 17, Series 2, Part 4 (1955).

Other (2)

A. D. Code, W. C. Liller, Astronomical Techniques (Univ. of Chicago Press, Chicago, 1960), pp. 281–300.

M. A. Seeds, Ph.D. thesis, Indiana Univ., Bloomington (1970).

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Figures (3)

Fig. 1
Fig. 1

Block diagram of the optical arrangement, the data collection electronics, and the scan control circuits for the signal averaging spectrometer.

Fig. 2
Fig. 2

Three typical stellar scans showing the effects of scan speed and quality of night on the accuracy. Each displayed scan represents the same amount of observing time.

Fig. 3
Fig. 3

The accuracy of an averaged scan plotted against the number of sweeps accumulated during a 10 min interval. The upper curve is data from hazy and partly cloudy nights while data in the lower curve were taken on photometric nights.

Equations (1)

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σ ¯ = - 2.5 log 10 [ 1 - pairs x F - x R x F + x R 2 N ] ,

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