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NIST Atomic Spectra Database Lines Data

H I: 13 Lines of Data Found
Z = 1, H isoelectronic sequence 
Example of how to reference these results:
Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2023). NIST Atomic Spectra Database (ver. 5.11), [Online]. Available: https://physics.nist.gov/asd [2024, April 16]. National Institute of Standards and Technology, Gaithersburg, MD. DOI: https://doi.org/10.18434/T4W30F
BibTex Citation (new window)
 
Wavelength range: 380 - 700 nm
λ in: vacuum
Highest relative intensity: 500000

Primary data sources
Query NIST Bibliographic Databases for
H I (new window)
Energy Levels:  Kramida 2010     Most of the given level values are essentially experimental ones. More accurate theoretical data on fine-structure energy levels and transitions between them can be obtained in the NIST Database of Energy Levels of Hydrogen and Deuterium. The levels designated only by a principal quantum number n in the configuration column represent centers of groups of all fine-structure levels having the given n. Their values were derived from line series observed in emission from solar corona and are relevant only for this type of observations. Uncertainties of the level values vary between 3 and 23 in the units of the last given decimal place. The level values in square brackets were obtained by interpolation or extrapolation of experimental fine-structure intervals or by fitting the Ritz-type formulas along series of levels. The level values in parentheses were derived from the theoretical values in the NIST Database of Energy Levels of Hydrogen and Deuterium by adding to them calculated off-diagonal magnetic-dipole hyperfine shifts. H I Energy Levels
Lines:  Kramida 2010     The lines corresponding to transitions associated with the levels designated only by the principal quantum numbers (e.g., 2-3 or 1s-2) correspond to observations in which the fine structure of transitions is completely unresolved. Their observed and calculated (Ritz) wavelengths, given here, are pertinent to observations of the solar corona. The observed intensity values of these lines, given in arbitrary units, are pertinent to the same type of observations. Intensity values given in parentheses are extrapolated values. Relative intensities of lines in laboratory light sources differ from those in the solar corona by several orders of magnitude and strongly depend on experimental conditions. Wavelengths of centers of gravity and various blended groups of fine-structure components of the Balmer series lines, derived assuming Boltzmann populations in an optically thin medium, are given without level classifications. Their identities and uncertainties are explained in the "Line Ref." column. H I Line Wavelengths and Classification
Transition Probabilities:  Wiese & Fuhr 2009, Jitrik & Bunge 2004     The data of Jitrik & Bunge 2004 have been scaled to the CODATA-2018 values of the fundamental constants by A. Kramida for the release of ASD v. 5.10 in October 2022. H I Transition Probabilities

 Observed 
 Wavelength 
 Vac (nm) 		  Unc. 
 (nm) 		  Rel. 
 Int. 
(?) 		 Aki
 (s−1) 		  fik   Acc.   Ei 
 (cm−1) 		    Ek 
 (cm−1) 		  Lower Level 
 Conf., Term, J 		  Upper Level 
 Conf., Term, J 		  gi   -   gk   Type   TP
Ref.		  Line
Ref.
                                         
383.6485       0.0006        30000  1.2156e+05   5.4317e-03    AAA 82 259.158         -  108 324.7253      2         9         8 - 162  T8637 L7436c29
389.0166       0.0006        70000  2.2148e+05   8.0397e-03    AAA 82 259.158         -  107 965.0568      2         8         8 - 128  T8637 L7436c29
397.1198       0.0006        30000  4.3889e+05   1.2711e-02    AAA 82 259.158         -  107 440.4508      2         7         8 - 98  T8637 L7436c29
410.2892       0.0006        70000  9.7320e+05   2.2105e-02    AAA 82 259.158         -  106 632.1681      2         6         8 - 72  T8637 L7436c29
434.1692       0.0006        90000  2.5304e+06   4.4694e-02    AAA 82 259.158         -  105 291.657       2         5         8 - 50  T8637 L7436c29
                                         
486.264488953  0.000000008     9.6680e+06   6.8544e-02    AAA 82 258.9543992821  -  102 823.8943175   2s   2S   1/2   4p   2P°   3/2   2 - 4  T7771 L9477
486.265570377  0.000000012     9.6682e+06   3.4273e-02    AAA 82 258.9543992821  -  102 823.8485825   2s   2S   1/2   4p   2P°   1/2   2 - 2  T7771 L9477
486.271        0.005         180000  8.4193e+06   1.1938e-01    AAA 82 259.158         -  102 823.904       2         4         8 - 32  T8637 L7439c30
656.4522552    0.0000024       5.3877e+07   6.9614e-01    AAA 82 258.9191133     -  97 492.319433    2p   2P°   1/2   3d   2D   3/2   2 - 4  T7771 L2752
656.4537684    0.0000004       2.2448e+07   2.9005e-01    AAA 82 258.9543992821  -  97 492.319611    2s   2S   1/2   3p   2P°   3/2   2 - 4  T7771 L6891c38
                                         
656.4584404    0.0000004       2.2449e+07   1.4503e-01    AAA 82 258.9543992821  -  97 492.211200    2s   2S   1/2   3p   2P°   1/2   2 - 2  T7771 L6891c38
656.460        0.003         500000  4.4101e+07   6.4108e-01    AAA 82 259.158         -  97 492.304       2         3         8 - 18  T8637 L7400c29
656.466464     0.000006        6.4651e+07   6.2654e-01    AAA 82 259.2850014     -  97 492.355566    2p   2P°   3/2   3d   2D   5/2   4 - 6  T7771 L2752

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