Radio wavelength observations of the L134N molecular core

Details Radio wavelength observations of the L134N molecular core Radio wavelength observations of the L134N molecular core

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apjs...71..219s&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 71, Oct. 1989, p. 219-244.

Astronomy and Astrophysics

Astrophysics

50

Abundance, Interstellar Matter, Molecular Clouds, Nebulae, Radio Spectroscopy, Emission Spectra, Molecular Spectra, Spatial Distribution, Spectrum Analysis, Tables (Data)

Scientific paper

A detailed study of the L134N dense molecular core through radio astronomical observations of spectral lines at millimeter and centimeter wavelengths is presented. The prototypical dark cloud was chosen for the following reasons: it is a nearby cloud at a distance of 160 pc, and thus radio observations have high spatial resolution; it resides out of the galactic disk, providing unobscured viewing along the line of sight; and it is known to be a rich source of molecular emission. The absence af any embedded infrared sources leads to the assumption that L134N is either in a stage of evolution prior to star formation or is a cloud in which internal support will prohibit a star from forming. A spectral line survey of 24 molecular transitions at up to seven positions in the L134N core, and observations of molecular emission from C18O, CSm, H13CO+, SO, NH3, and C3H2 are reviewed. Results indicate different spatial distributions for each species which may be attributed to variations in the excitation conditions for each transition or chemical abundance variations within the cloud core. Observational techniques and results are presented.

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