Abstract

A tungsten ribbon filament lamp fitted with a sapphire window and operated at a temperature of 2800 K is shown to be a stable reproducible calibration source over the wavelength range 1500–2700 Å. Spectra of the lamp obtained using a 50-cm Ebert spectrometer and an extreme-solar-blind photomultiplier with pulse-counting electronics are reproducible to better than ±10% over this spectral range. Careful calibration of the spectrometer and photomultiplier has allowed a direct measurement of the absolute spectral radiance of the lamp, hence the apparent emissivity of the hot tungsten filament, from 1500 Å to 2700 Å.

© 1971 Optical Society of America

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References

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  1. M. W. P. Cann, Appl. Opt. 8, 1645 (1969).
    [CrossRef] [PubMed]
  2. T. D. Parkinson, Ph.D. Thesis, Univ. of Pittsburgh, Pittsburgh, Pa. (1969).
  3. W. G. Fastie, “Absolute Radiometry in Space Astronomy,” in Optical Telescope Technology, NASA SP-233 (U.S. GPO, Washington, D.C., 1970).
  4. L. G. Leighton, Illum. Eng. 57, 121 (1962).
  5. J. A. R. Samson, Techniques of Vacuum Ultraviolet Spectroscopy (Wiley, New York, 1967).
  6. D. F. Heath, P. A. Sacher, Appl. Opt. 5, 937 (1966).
    [CrossRef] [PubMed]
  7. W. E. Forsythe, E. Q. Adams, J. Opt. Soc. Amer. 35, 108 (1945).
    [CrossRef]
  8. J. C. DeVos, Physica 20, 690 (1954).
    [CrossRef]
  9. H. C. Hamaker (communicated by L. S. Ornstein), Physica3, 561 (1936).
    [CrossRef]
  10. C. B. Opal, Ph.D. Thesis, The Johns Hopkins Univ., Baltimore, Md. (1969).
  11. J. C. Fleming, Appl. Opt. 5, 195 (1966).
    [CrossRef]

1969 (1)

1966 (2)

1962 (1)

L. G. Leighton, Illum. Eng. 57, 121 (1962).

1954 (1)

J. C. DeVos, Physica 20, 690 (1954).
[CrossRef]

1945 (1)

W. E. Forsythe, E. Q. Adams, J. Opt. Soc. Amer. 35, 108 (1945).
[CrossRef]

Adams, E. Q.

W. E. Forsythe, E. Q. Adams, J. Opt. Soc. Amer. 35, 108 (1945).
[CrossRef]

Cann, M. W. P.

DeVos, J. C.

J. C. DeVos, Physica 20, 690 (1954).
[CrossRef]

Fastie, W. G.

W. G. Fastie, “Absolute Radiometry in Space Astronomy,” in Optical Telescope Technology, NASA SP-233 (U.S. GPO, Washington, D.C., 1970).

Fleming, J. C.

Forsythe, W. E.

W. E. Forsythe, E. Q. Adams, J. Opt. Soc. Amer. 35, 108 (1945).
[CrossRef]

Hamaker, H. C.

H. C. Hamaker (communicated by L. S. Ornstein), Physica3, 561 (1936).
[CrossRef]

Heath, D. F.

Leighton, L. G.

L. G. Leighton, Illum. Eng. 57, 121 (1962).

Opal, C. B.

C. B. Opal, Ph.D. Thesis, The Johns Hopkins Univ., Baltimore, Md. (1969).

Ornstein, L. S.

H. C. Hamaker (communicated by L. S. Ornstein), Physica3, 561 (1936).
[CrossRef]

Parkinson, T. D.

T. D. Parkinson, Ph.D. Thesis, Univ. of Pittsburgh, Pittsburgh, Pa. (1969).

Sacher, P. A.

Samson, J. A. R.

J. A. R. Samson, Techniques of Vacuum Ultraviolet Spectroscopy (Wiley, New York, 1967).

Appl. Opt. (3)

Illum. Eng. (1)

L. G. Leighton, Illum. Eng. 57, 121 (1962).

J. Opt. Soc. Amer. (1)

W. E. Forsythe, E. Q. Adams, J. Opt. Soc. Amer. 35, 108 (1945).
[CrossRef]

Physica (1)

J. C. DeVos, Physica 20, 690 (1954).
[CrossRef]

Other (5)

H. C. Hamaker (communicated by L. S. Ornstein), Physica3, 561 (1936).
[CrossRef]

C. B. Opal, Ph.D. Thesis, The Johns Hopkins Univ., Baltimore, Md. (1969).

J. A. R. Samson, Techniques of Vacuum Ultraviolet Spectroscopy (Wiley, New York, 1967).

T. D. Parkinson, Ph.D. Thesis, Univ. of Pittsburgh, Pittsburgh, Pa. (1969).

W. G. Fastie, “Absolute Radiometry in Space Astronomy,” in Optical Telescope Technology, NASA SP-233 (U.S. GPO, Washington, D.C., 1970).

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Figures (3)

Fig. 1
Fig. 1

Optical instrumentation for standard lamp measurements.

Fig. 2
Fig. 2

Measured emissivity of tungsten at 2800 K. —, present; — - —, Ref. 7; ……, Ref. 8; - - - - - -, Ref. 9. Note that data have not been normalized. Inner bars represent uncertainties exclusive of photomultiplier calibration; outer bars include photomultiplier.

Fig. 3
Fig. 3

Observed (A12O3, 2798 K) and predicted (MgF2, 3000 K) standard lamp spectra.

Tables (2)

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Table I Observed Tungsten Lamp Spectra

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Table II Spectral Radiance of Tungsten Filament Lamp and 2798 K Blackbody

Equations (1)

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S = [ 1 / ( R ¯ - R s ) ] [ 1 / ( 3 - 1 ) ] [ 1 = i 3 ( R i - R ¯ ) 2 ] 1 2 ,

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