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HIGH VIBRATIONAL LEVELS OF $O_{2}(b^{1}\Sigma^{+}_{g})$ AND $O_{2}(a^{1}\Delta_{g})$

Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/20077

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Title: HIGH VIBRATIONAL LEVELS OF $O_{2}(b^{1}\Sigma^{+}_{g})$ AND $O_{2}(a^{1}\Delta_{g})$
Creators: Kalogerakis, K. S.; Huestis, D. L.; Cosby, P. C.; Slanger, T. G.; Copeland, Richard A.; Totth, A.
Issue Date: 2001
Abstract: Relaxation of laser-excited $O_{2}(A^{3}\Sigma^{+}_{u}$, $v = 6-10)$ in collisions with $O_{2}$ populates high vibrational levels of $O_{2}(b^{1}\Sigma^{+}_{g})$ and $O_{2}(a^{1}\Delta_{g})$. Previous work on the spectroscopy of $O_{2}$ emissions from the Earth's night atmosphere has enabled us to assign the Q-branches of thirteen $(v^{\prime},v^{\prime\prime})$ bands in the $(2+1)$ REMPI spectra of $O_{2}(b^{1}\Sigma^{+}_{g}$, $v^{\prime\prime}= 10 - 15)$ and $O_{2}(a^{1}\Delta_{g}$, $v^{\prime\prime}= 16 - 19)$, through the intermediate Rydberg levels $3d\pi {^{1}\Sigma^{+}_{g}}(v^{\prime} = 2 - 5)$ and $^{1}\Delta = 4, 5)$, repectively. The derived spectroscopic constants for $O_{2}(b^{1}\Sigma^{+}_{g}, v^{\prime\prime} = 10 - 13)$ agree with our previous work. Improved values are obtained for $v^{\prime\prime} = 14, 15$. Our constants for $3d\pi {^{1}\Sigma^{+}_{g}}(v^{\prime\prime}= 5)$ are the first available. Our spectra are better calibrated and our constants for the $v^{\prime} = 2 - 4$ levels significantly more precise than the 1988-1992 work in the groups of Chupka and Houston. The energies of $O_{2}(a^{1}\Delta_{g}, v^{\prime\prime} = 16 - 19)$ were known previously only to within about $80 cm^{-1}$ from the 1995 electron scattering work of Allan. The highest level known accurately from nightglow spectra is $v^{\prime\prime} = 11$. Our spectral analysis gives precise rotational constants and $\Delta G$ values for these vibrational levels and for $3d\pi {^{1}\Delta_{g}} (v^{\prime}= 4, 5)$. The absolute term energies are uncertain by about $5 cm^{-1}$ based on earlier work in the groups of Chupka and Houston. Supported by the NASA Geospace Sciences and Planetary Atmospheres programs and by the NSF Aeronomy and Physics/REU programs.
URI: http://hdl.handle.net/1811/20077
Other Identifiers: 2001-MH-10
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