Heteronuclear diatomics in diffuse and translucent clouds

Abstract

Diffuse and translucent molecular clouds fill a vast majority of the interstellar space in the galactic disk being thus the most typical objects of the Interstellar Medium (ISM). Recent advances in observational techniques of modern optical and ultraviolet spectroscopy led to detection of many features of atomic and molecular origin in spectra of such clouds. Molecular spectra of heteronuclear diatomic molecules, ie. OH, OH+, CH CH+, CN, NH, CO play an important role in understanding chemistry and physical conditions in environments they do populate. A historical review of astronomical observations of interstellar molecules is presented. Recent results based on visual and ultraviolet observations of molecular features in spectra of reddened, early type OB-stars are presented and discussed. Appearance of vibrational-rotational spectra with observed transitions based on high-quality spectra, are also presented. Relations between column densities of heteronuclear diatomics (based on the recommended oscillator strengths) and intensities of diffuse interstellar bands (DIBs) are also presented and discussed.

arXiv comment21 pages, 8 figures, 3 tables

References in corpus (4)

• Ultraviolet Survey of CO and H_2 in Diffuse Molecular Clouds: The Reflection of Two Photochemistry Regimes in Abundance Relationships
• The Diffuse Interstellar Bands: A Major Problem in Astronomical Spectroscopy
• The relation between column densities of interstellar OH and CH molecules
• Centrosymmetric molecules as possible carriers of diffuse interstellar bands