![]() ![]() For β Sco, we find that the derived column density of the J'' = 1 rotational level differs by a factor of 2–3 when compared to the previous observations. These results are compared to previous values that were measured using the damping wings of low J'' H absorption features. We present flight results of interstellar molecular hydrogen excitation on the sightlines, including measurements of the column densities and temperatures. The final two flights of the instrument observed Scorpii ( β Sco) and γ Arae. The Colorado High-resolution Echelle Stellar Spectrograph is a far-ultraviolet rocket-borne instrument designed to study the atomic-to-molecular transitions within diffuse molecular and translucent cloud regions. Measuring the temperature and abundance patterns of clouds in the interstellar medium (ISM) provides an observational basis for models of the physical conditions within the clouds, which play an important role in studies of star and planet formation.
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