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Interstellar H3O(+) and its relation to the O2 and H2O abundances
Phillips, T. G.; van Dishoeck, Ewine F.; Keene, Jocelyn
AA(California Inst. of Technology, Pasadena), AB(Leiden Observatory, Netherlands), AC(California Inst. of Technology, Pasadena)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 2, p. 533-550. (ApJ Homepage)
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NASA/STI Keywords:
Hydronium Ions, Interstellar Chemistry, Molecular Interactions, Molecular Spectra, Oxygen, Abundance, Interstellar Extinction, Radio Spectra
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An interstellar medium study of the three reasonably accessible low-lying submillimeter lines of the H3O(+) molecular ion at 396, 364, and 307 GHz is presented. An analysis of the H3O(+) line ratios shows that under high density (about 10 exp 6 - 10 exp 7/cu cm) and high-temperature (greater than about 50 K), the 396 GHz line is about a factor of two stronger than the 364 GHz line, with the 307 GHz line much weaker. For lower densities, the excitation of the 364 GHz line can be very sensitive to dust radiation pumping, and it is shown that this is the case in Sgr B2, resulting in the 364 GHz line being a factor of 2-3 stronger than the 396 GHz line. Under almost all conditions, the 307 GHz line is weak, the exception being for densities greater than about 10 exp 7/cu cm.

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