Precise spectroscopy of astrophysically important species

Details Precise spectroscopy of astrophysically important species Precise spectroscopy of astrophysically important species

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spie.6580e...1l&link_type=abstract

15th Symposium on High-Resolution Molecular Spectroscopy. Edited by Ponomarev, Yurii N.; Mikhailenko, Semen N.; Sinitsa, Leonid

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Detailed studies of physical and chemical conditions in regions of star formation need multiline observations of different molecular species. A correct retrieval of systematic velocity fields in these objects from such measurements requires accuracy of rest frequencies of about 1 m/s. Because of a very small thermal line broadening at typical kinetic temperatures in dark clouds (Tk ~10 K) the precise knowledge of the hyperfine structure of observed transitions is extremely important for line shape analysis. Unfortunately, the available laboratory uncertainty for a large number of measured transitions is about 30 - 100 kHz. This value is comparable with molecular line widths in dark clouds and very often it is sufficient only for identification of observed species but not for detailed kinematical studies from multiline data. Taking into account our recent laboratory and radio astronomical studies, a large set of molecular spectra were measured with ~10-9 relative uncertainty, including precise estimates of hf structure. It is shown that whereas laboratory methods are sufficiently good for stable molecules, the use of radio astronomical measurements may be preferable for laboratory unstable species.

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