PO - Prospects in interstellar medium

Details PO - Prospects in interstellar medium PO - Prospects in interstellar medium

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.133..267a&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 133, no. 2, 1987, p. 267-273. Research supported by the Fundacao de Amparo

Astronomy and Astrophysics

Astrophysics

1

Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Oxygen, Phosphorus, Vapor Phases, Astronomical Spectroscopy, Charge Transfer, Dissociation, Franck-Condon Principle, Molecular Spectra, Recombination Reactions

Scientific paper

Relevant terrestrial PO lines in the ultraviolet, infrared and microwave regions are listed in order to aid the detection of PO in interstellar clouds. Within the framework of Klein-Dunham potential, spontaneous emission rates and oscillator strengths of strong (Δυ = 0 sequence) beta bands of the PO molecule are estimated. For Sgr B2 source, under optically thin case, each of the two strongest 2π1/2, J = 2.5-1.5 rotational transitions (108.998 GHz and 109.206 GHz) of PO would have antenna temperature less than 125 mk for beam efficiency ≡0.6 and μ = 0.7D (electric dipole moment of PO in the υarcsec = 0 level of the X2π state). For Orion molecular cloud, PO (4, 4.5, 5-3, 3.5, 4)(e, f) lines are excitable at 196.305 and 196.500 GHz and each line would have antenna temperature less than 110 mK.

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