Cold and Warm Atomic Gas around the Perseus Molecular Cloud. I. Basic Properties

Type Journal Article
Names Sne┼żana Stanimirovi─ç, Claire E. Murray, Min-Young Lee, Carl Heiles, Jesse Miller
Publication The Astrophysical Journal
Volume 793
Issue 2
Pages 132
Journal Abbreviation The Astrophysical Journal
Date October 1, 2014
DOI 10.1088/0004-637X/793/2/132
ISSN 0004-637X
URL http://adsabs.org/2014ApJ.793.132S
Library Catalog adslabs.org
Abstract Using the Arecibo Observatory, we have obtained neutral hydrogen (HI) absorption and emission spectral pairs in the direction of 26 background radio continuum sources in the vicinity of the Perseus molecular cloud. Strong absorption lines were detected in all cases, allowing us to estimate spin temperature (Ts ) and optical depth for 107 individual Gaussian components along these lines of sight. Basic properties of individual H I clouds (spin temperature, optical depth, and the column density of the cold and warm neutral medium (CNM and WNM), respectively) in and around Perseus are very similar to those found for random interstellar lines of sight sampled by the Millennium H I survey. This suggests that the neutral gas found in and around molecular clouds is not atypical. However, lines of sight in the vicinity of Perseus have, on average, a higher total H I column density and the CNM fraction, suggesting an enhanced amount of cold H I relative to an average interstellar field. Our estimated optical depth and spin temperature are in stark contrast with the recent attempt at using Planck data to estimate properties of the optically thick H I. Only ~15% of lines of sight in our study have a column density weighted average spin temperature lower than 50 K, in comparison with >~ 85% of Planck's sky coverage. The observed CNM fraction is inversely proportional to the optical depth weighted average spin temperature, in excellent agreement with the recent numerical simulations by Kim et al. While the CNM fraction is, on average, higher around Perseus relative to a random interstellar field, it is generally low, between 10%-50%. This suggests that extended WNM envelopes around molecular clouds and/or significant mixing of CNM and WNM throughout molecular clouds are present and should be considered in the models of molecule and star formation. Our detailed comparison of H I absorption with CO emission spectra shows that only 3 of the 26 directions are clear candidates for probing the CO-dark gas as they have N(H I)>1021 cm-2 yet no detectable CO emission.
Tags ISM: clouds, ISM: structure, Radio Lines: ISM
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