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Neutral Atomic Phases of the Interstellar Medium in the Galaxy
Much of the interstellar medium in disk galaxies is in the form of neutral atomic hydrogen, H i. This gas can be in thermal equilibrium at relatively low temperatures, Td300 K (the cold neutralExpand
The Physics and Chemistry of the Interstellar Medium
1. The galactic ecosystem 2. Cooling processes 3. Heating processes 4. Chemical processes 5. Interstellar dust 6. Interstellar polycyclic aromatic hydrocarbon molecules 7. HII regions 8. The phasesExpand
Photodissociation regions. I - Basic model. II - A model for the Orion photodissociation region
A theoretical parameter study of the temperature and chemical structure of dense photodissociation regions and their resultant spectrum is presented. Models are discussed which are relevant not onlyExpand
The neutral atomic phases of the interstellar medium
We calculate the thermal equilibrium gas temperature of the diffuse interstellar medium. Our method incorporates a new photoelectric heating rate from small grains and polycyclic aromaticExpand
Interstellar Polycyclic Aromatic Hydrocarbon Molecules
Large polycyclic aromatic hydrocarbon (PAH) molecules carry the infrared (IR) emission features that dominate the spectra of most galactic and extragalactic sources. This review surveys the observedExpand
Interstellar polycyclic aromatic hydrocarbons: the infrared emission bands, the excitation/emission mechanism, and the astrophysical implications.
The spectroscopic structure these PAHs and PAH-related materials produce in the UV portion of the interstellar extinction curve lie just below current detection limits but fall in the range detectable by the Hubble Space Telescope. Expand
The rich 6 to 9 vec mu m spectrum of interstellar PAHs
IR spectroscopy provides a valuable tool for the characterisation and identification of interstellar molecular species. Here, we present 6-9 mum spectra of a sample of reflection nebulae, HIIExpand
Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE). I. Overview and Initial Results
We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7° × 7°) using the IRAC (3.6, 4.5, 5.8, and 8 μm) and MIPS (24, 70, and 160 μm) instruments on board theExpand