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  1. D. Desmarais and E. H. Pinnington, J. Opt. Soc. Am. 57, 1245 (1967).
    [Crossref]
  2. A. S. King, Astrophys. J. 72, 221 (1930).
    [Crossref]
  3. A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
    [Crossref]
  4. J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).
    [Crossref]
  5. W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U. S.) Monograph 32—Part I (U. S. Govt. Printing Office, Washington, D. C., 1961).
  6. A. Gatterer and J. Junkes, Spektren der Seltenen Erden (Specola Vaticana, Vatican, 1945).
  7. J. Sugar, J. Opt. Soc. Am. 58, 1519 (1968).
    [Crossref]
  8. J. H. McElaney, J. Opt. Soc. Am. 57, 870 (1967).
    [Crossref]
  9. Comparisons with other rare-earth spectra indicate that the 6s2 shell has little effect upon the 4ƒn configuration, and thus the ground multiplets for the first and third spectra are nearly identically spaced. Therefore, the ground-state 4I levels in Ho i should lie very close to the corresponding levels at 0, 5438, 8644, and 10770 cm−1 in Ho iii. For Ho ii, we obtain energies of 5750±50 and 6000±50 cm−1 for the second pair of levels, (13/2,1/2)7 and (13/2, 1/2)6, by interpolation between known levels in neighboring elements. This method forecasts the ground-state interval of 637.8 cm−1, to within ±20 cm−1.

1968 (1)

1967 (2)

1963 (1)

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).
[Crossref]

1961 (1)

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
[Crossref]

1930 (1)

A. S. King, Astrophys. J. 72, 221 (1930).
[Crossref]

Cabezas, A. Y.

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
[Crossref]

Conway, J. G.

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).
[Crossref]

Corliss, C. H.

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U. S.) Monograph 32—Part I (U. S. Govt. Printing Office, Washington, D. C., 1961).

Desmarais, D.

Gatterer, A.

A. Gatterer and J. Junkes, Spektren der Seltenen Erden (Specola Vaticana, Vatican, 1945).

Junkes, J.

A. Gatterer and J. Junkes, Spektren der Seltenen Erden (Specola Vaticana, Vatican, 1945).

King, A. S.

A. S. King, Astrophys. J. 72, 221 (1930).
[Crossref]

Lindgren, I.

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
[Crossref]

Marrus, R.

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
[Crossref]

McElaney, J. H.

Meggers, W. F.

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U. S.) Monograph 32—Part I (U. S. Govt. Printing Office, Washington, D. C., 1961).

Pinnington, E. H.

Scribner, B. F.

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U. S.) Monograph 32—Part I (U. S. Govt. Printing Office, Washington, D. C., 1961).

Sugar, J.

Wybourne, B. G.

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).
[Crossref]

Astrophys. J. (1)

A. S. King, Astrophys. J. 72, 221 (1930).
[Crossref]

J. Opt. Soc. Am. (3)

Phys. Rev. (2)

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
[Crossref]

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).
[Crossref]

Other (3)

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U. S.) Monograph 32—Part I (U. S. Govt. Printing Office, Washington, D. C., 1961).

A. Gatterer and J. Junkes, Spektren der Seltenen Erden (Specola Vaticana, Vatican, 1945).

Comparisons with other rare-earth spectra indicate that the 6s2 shell has little effect upon the 4ƒn configuration, and thus the ground multiplets for the first and third spectra are nearly identically spaced. Therefore, the ground-state 4I levels in Ho i should lie very close to the corresponding levels at 0, 5438, 8644, and 10770 cm−1 in Ho iii. For Ho ii, we obtain energies of 5750±50 and 6000±50 cm−1 for the second pair of levels, (13/2,1/2)7 and (13/2, 1/2)6, by interpolation between known levels in neighboring elements. This method forecasts the ground-state interval of 637.8 cm−1, to within ±20 cm−1.

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Tables (3)

Tables Icon

Table I Zeeman-effect data for neutral holmium.

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Table II Transitions giving the 637.4-cm−1 interval and the 3.1-cm−1 hfs difference in Ho ii.

Tables Icon

Table III Total hfs widths for 10 proposed excited-state levels in Ho ii.