The interstellar medium of galaxies is the reservoir out of which stars are born and into
which stars inject newly created elements as they age. The physical properties of the …

▪ Abstract All neutral atomic hydrogen gas and a large fraction of the molecular gas in the
Milky Way Galaxy and external galaxies lie in PDRs, and PDRs are the origin of most of the …

This paper presents high-angular-resolution maps of the M17 SW cloud core in the C (O-18)
J= 2-1 (13 arcsec FWHM beam) and C (S-34) J= 2-1 (27 arcsec FWHM), 3-2 (17 arcsec …

Some of the aspects of submillimeter-wave astronomy which are relevant to the field of
heterodyne spectroscopy are reviewed. Most of the discussion concerns the dense …

The edges of molecular clouds - Fractal boundaries and density structure ADS Classic is
now deprecated. It will be completely retired in October 2019. This page will automatically …

Carbon monoxide (CO) is widely used as a tracer of molecular hydrogen (H2) in metal-rich
galaxies, but is known to become ineffective in low-metallicity dwarf galaxies. Atomic carbon …

To investigate the effects of the UV radiation on the chemistry of nitrogenated molecules, we
have carried out an observational study of the reflection nebula NGC 7023. We have …

We use detailed numerical simulations of a turbulent molecular cloud to study the
usefulness of the [C i] 609 and 370 μm fine structure emission lines as tracers of cloud …

Turbulence in molecular clouds is well recognized, but the resultant diffusive transport and
its effects on the chemical structure of the clouds have not been extensively investigated. We …

Context. The [C II] 158 μm far-infrared fine-structure line is one of the most important cooling
lines of the star-forming interstellar medium (ISM). It is used as a tracer of star formation …