Chemistry and rotational excitation of O2 in interstellar clouds. II - The ^16^O^18^O isotopomer J/A+A/328/617 J/A+A/328/617 16^O 18^O isotopomer collision rate Chemistry and rotational excitation of O2 in interstellar clouds. II - The ^16^O^18^O isotopomer P Marechal Y P Viala L Pagani Astron. Astrophys. 328 617 1997 1997A&A...328..617M Atomic physics Radio lines ISM: abundances ISM: molecules molecular processes radio lines: ISM In this paper, a chemical model of interstellar clouds including ^18^O and ^13^C isotopic reactions with a non-LTE calculations of ^16^O^18^O rotational population has been used to predict the intensity of the three ^16^O^18^O lines observable from the ground, namely 234, 298 and 402GHz.
Collision rates ^16^O^18^O-He (cm^3/s) Collision rates ^16^O^18^O-He (cm^3/s) Collision rates ^16^O^18^O-He (cm^3/s) Nu N value of the upper level --- Ju J value of the upper level --- Nl N value of the lower level --- Jl J value of the lower level --- a0 Collision rate factor (k_ul_=a_0-*T^0.3^) --- table4.texLaTeX version of table4 Patricia Bauer CDS 1997Jun12Priscilla MARECHAL <priscila@mesiom.obspm.fr> J_A+A_328_617.xml