HI-to-H2 transitions in the Perseus Molecular Cloud

Abstract

We apply the Sternberg et al. (2014) theoretical model to analyze HI and H2 observations in the Perseus molecular cloud. We constrain the physical properties of the HI shielding envelopes and the nature of the HI-to-H2 transitions. Our analysis (Bialy et al. 2015) implies that in addition to cold neutral gas (CNM), less dense thermally-unstable gas (UNM) significantly contributes to the shielding of the H2 cores in Perseus.

4 pages, 1 figure. To appear in proceedings of "The 6th Zermatt ISM Symposium: Conditions and Impact of Star Formation From Lab to Space", eds. R. Simon and M. Rollig

References in corpus (5)

• The Atomic to Molecular Transition in Galaxies. II: HI and H_2 Column Densities
• The COMPLETE Survey of Star-Forming Regions: Phase I Data
• HI-to-H2 Transitions and H I Column Densities in Galaxy Star-Forming Regions
• Cold and Warm Atomic Gas around the Perseus Molecular Cloud. II. The Impact of High Optical Depth on the HI Column Density Distribution and Its Implication for the HI-to-H2 Transition
• HI-to-H2 Transitions in the Perseus Molecular Cloud