These are : a ) a high extinction-corrected luminosity > 3x10 ^ 40 Ergs s ^-1 of the hydrogen beta emission line; ( see Hydrogen spectral series ) b ) a high equivalent width greater than 5 nm; c ) a strong [ OIII ] wavelength at the 436.3 nm emission line allowing accurate abundance determination; d ) a compact structure on SDSS images; and e ) an absence of obvious active galactic nuclei spectroscopic features.
12.
The Lyman-alpha line is most simply described by the { " n ", " m " } = { 1, 2 . . . } solutions to the empirical Rydberg formula for hydrogen's Lyman spectral series . ( The Lyman-alpha frequency is produced by multiplying the Rydberg frequency for the atomic mass of hydrogen, " R M " ( see Rydberg constant ), by a factor of ( ) 2 " ( ) 2 = . ) Empirically, the Rydberg equation is in turn modeled by the semi-classical Bohr model of the atom.
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