2007/07/31 by P. Gnaciński, P. Gnacinski, M. Krogulec
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #astro-ph
paper · pdf · doi:10.1051/0004-6361:20078602
published as Astron.Astrophys.477:543,2008 · Changed content, figure added
arxiv created 2007/10/01 · openalex publication_date 2007/11/06 · arxiv updated 2010/04/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
Interstellar clouds that exhibit strong Ca I and Fe I lines are called CaFe clouds. Ionisation equilibrium equations were used to model the column densities of Ca II, Ca I, K I, Na I, Fe I and Ti II in CaFe clouds. We find that the chemical composition of CaFe clouds is solar and that there is no depletion into dust grains. CaFe clouds have high electron densities, ne≈1 cm-3, that lead to high column densities of neutral Ca and Fe.