Multimolecular studies of Galactic star-forming regions

• Published in: Monthly notices of the Royal Astronomical Society 2014-12, Vol.445 (4), p.3331-3344
• Main Authors: Baan, W. A., Loenen, A. F., Spaans, M.
• Format: Article
• Language: English
• Subjects: Astroparticle Physics; Astropartikelfysik; Cosmic rays; Density; Flux; Heating; ISM: abundances; ISM: jets and outflows; ISM: molecules; Mathematical models; Molecules; Physical properties; radio lines: ISM; Redundancy; Signatures; Star formation; Stars & galaxies; stars: formation; surveys; Symbols
• ISSN: 0035-8711; 1365-2966; 1365-2966
• DOI: 10.1093/mnras/stu1897

Molecular emission-line observations of isolated Galactic star-forming regions are used to model the physical properties of the molecular interstellar medium in these systems. Observed line ratios are compared with the results predicted by models that incorporate gas-phase chemistry and the heating by stellar radiation and non-radiative feedback processes. The line ratios of characteristic tracer molecules may be interpreted using the contributions of two distinct components: a cold (40–50 K) and high-density (105–105.5 cm−3) photon-dominated region (PDR) with a nominal UV flux density and a warm (∼300 K) mechanical heating-dominated region (MHDR) with a slightly lower density (104.5–105 cm−3). The relative contributions of these structural components are used to model the observed line ratios. Ionized species may be better modelled by adopting an increase of the cosmic ray flux towards the Galactic Centre and the sulphur abundance should depleted by a factor of 200–400 relative to solar values. The line ratios of the Galactic sample are found to be very similar to those of the integrated signature of prominent (ultra)luminous IR Galaxies. The PDRs and MHDRs in the isolated Galactic regions may be modelled with slightly higher mean densities than in extragalactic systems and a higher MHDR temperature resulting from non-radiative mechanical heating. Multimolecular studies are effective in determining the physical and chemical properties of star formation regions by using characteristic line ratios to diagnose their environment. The addition of more molecular species will reduce the existing modelling redundancy.