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  1. Hyde and Forsythe: J. Frank. Inst, 183, pp. 353–354; 1917. E. F. Kingsbury: J. Frank. Inst., 183, pp. 781–782; 1917.
  2. Meeting of American Physical Society, Washington, April, 1921; Phy. Rev. (2) 18, p. 147; Aug., 1921.
  3. J. Op. Soc. Am., 5, pp. 178–183; March, 1921. Cf. also Phy. Rev. (2), 10, pp. 208–212; 1917, particularly the closing paragraph.
  4. Coblentz, B. S. Sci. Pap. No. 248; p. 470; 1916. Forsythe, J. Op. Soc. Am., 4, p. 332; 1920.
  5. In previous papers (J. Op. Soc. Am., 5, pp. 178–183; March 1921 and B. S. Sci. Pap. No. 417, Vol. 17, pp. 231–265; 1921), the color temperature 2830°K was inferred from these same data. This value was merely a rough approximation as inferred from plotting the data on a small scale and is not accurate enough for the present purpose. The revised value given in the present paper results from a more careful examination of the data, and a more precise and reliable method of reducing it.
  6. Compare also:—Jour. Op. Soc. Am., 4, pp. 389–401; 1920. B. S. Sci. Pap. No. 417, Vol. 17, p. 234; 1921.
  7. J. Op. Soc. Am., 4, pp. 389–401; 1920. B. S. Sci. Pap. 417, Vol. 17, pp. 234–235; 1921.
  8. It is to be observed that while the visibility of energy enters into the formulas used, it does not enter in such a way as to affect the temperature found so long as the same values of visibility known to be approximately correct, are used in determining all values of λc considered and the spectral distribution approximates Planck’s formula. The values of visibility actually used throughout the present paper are shown by the solid curve in Fig. 8, J. Op. Soc. Am., 4, p. 471.
  9. Letter, W. E. Forsythe, Nela Lab., to I. G. Priest, Aug. 11, 1921.
  10. J. Op. Soc. Am. 4, pp. 485–486.
  11. Ann. der Phy. (4) 39, pp. 545–568; 1912.
  12. J. Op. Soc. Am., 5, pp. 178–183; March, 1921.
  13. The curve shown in Fig. 6, J. Op. Soc. Am., 5, p. 182, was obtained by this simple process of inspection.
  14. Cf. "Experimental Method" above.
  15. By the same method as described above for deriving the color temperature of the standard lamp No. 1717 from the radiometric data.
  16. Coblentz's determinations of Lamp 1717 were made in April 1917. His determinations on Lamp 1716 were made in December 1918, after readjusting his apparatus.
  17. Letter, Forsythe to Priest, July 29, 1921.
  18. These determinations were made by Ben S. Willis, Photometric Section, Bureau of Standards.
  19. Phy. Rev. (2) 18, p. 147; Aug. 1921.
  20. Worthing, Phys. Rev. (2) 10, p. 392; 1917.
  21. Cf. Forsythe, Phy. Rev. (2), 18, p. 147; 1921.
  22. Waidner and Burgess, B. S. Bulletin, 1, pp. 109–124; 1904.
  23. B. S. Bulletin, 1, p. 123.

1921

Letter, W. E. Forsythe, Nela Lab., to I. G. Priest, Aug. 11, 1921.

Cf. Forsythe, Phy. Rev. (2), 18, p. 147; 1921.

1917

Worthing, Phys. Rev. (2) 10, p. 392; 1917.

Hyde and Forsythe: J. Frank. Inst, 183, pp. 353–354; 1917. E. F. Kingsbury: J. Frank. Inst., 183, pp. 781–782; 1917.

1916

Coblentz, B. S. Sci. Pap. No. 248; p. 470; 1916. Forsythe, J. Op. Soc. Am., 4, p. 332; 1920.

1904

Waidner and Burgess, B. S. Bulletin, 1, pp. 109–124; 1904.

Bulletin, B. S.

B. S. Bulletin, 1, p. 123.

Forsythe, W. E.

Letter, W. E. Forsythe, Nela Lab., to I. G. Priest, Aug. 11, 1921.

Other

Hyde and Forsythe: J. Frank. Inst, 183, pp. 353–354; 1917. E. F. Kingsbury: J. Frank. Inst., 183, pp. 781–782; 1917.

Meeting of American Physical Society, Washington, April, 1921; Phy. Rev. (2) 18, p. 147; Aug., 1921.

J. Op. Soc. Am., 5, pp. 178–183; March, 1921. Cf. also Phy. Rev. (2), 10, pp. 208–212; 1917, particularly the closing paragraph.

Coblentz, B. S. Sci. Pap. No. 248; p. 470; 1916. Forsythe, J. Op. Soc. Am., 4, p. 332; 1920.

In previous papers (J. Op. Soc. Am., 5, pp. 178–183; March 1921 and B. S. Sci. Pap. No. 417, Vol. 17, pp. 231–265; 1921), the color temperature 2830°K was inferred from these same data. This value was merely a rough approximation as inferred from plotting the data on a small scale and is not accurate enough for the present purpose. The revised value given in the present paper results from a more careful examination of the data, and a more precise and reliable method of reducing it.

Compare also:—Jour. Op. Soc. Am., 4, pp. 389–401; 1920. B. S. Sci. Pap. No. 417, Vol. 17, p. 234; 1921.

J. Op. Soc. Am., 4, pp. 389–401; 1920. B. S. Sci. Pap. 417, Vol. 17, pp. 234–235; 1921.

It is to be observed that while the visibility of energy enters into the formulas used, it does not enter in such a way as to affect the temperature found so long as the same values of visibility known to be approximately correct, are used in determining all values of λc considered and the spectral distribution approximates Planck’s formula. The values of visibility actually used throughout the present paper are shown by the solid curve in Fig. 8, J. Op. Soc. Am., 4, p. 471.

Letter, W. E. Forsythe, Nela Lab., to I. G. Priest, Aug. 11, 1921.

J. Op. Soc. Am. 4, pp. 485–486.

Ann. der Phy. (4) 39, pp. 545–568; 1912.

J. Op. Soc. Am., 5, pp. 178–183; March, 1921.

The curve shown in Fig. 6, J. Op. Soc. Am., 5, p. 182, was obtained by this simple process of inspection.

Cf. "Experimental Method" above.

By the same method as described above for deriving the color temperature of the standard lamp No. 1717 from the radiometric data.

Coblentz's determinations of Lamp 1717 were made in April 1917. His determinations on Lamp 1716 were made in December 1918, after readjusting his apparatus.

Letter, Forsythe to Priest, July 29, 1921.

These determinations were made by Ben S. Willis, Photometric Section, Bureau of Standards.

Phy. Rev. (2) 18, p. 147; Aug. 1921.

Worthing, Phys. Rev. (2) 10, p. 392; 1917.

Cf. Forsythe, Phy. Rev. (2), 18, p. 147; 1921.

Waidner and Burgess, B. S. Bulletin, 1, pp. 109–124; 1904.

B. S. Bulletin, 1, p. 123.

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