Skip to main content

Cloud formation in the atomic and molecular phase: H I self absorption (HISA) towards a giant molecular filament

Wang, Y, Bihr, S., Beuther, H., Rugel, M.R., Soler, J.D., Ott, J., Kainulainen, J., Schneider, N., Klessen, R.S., Glover, S.C.O., and others. (2020) Cloud formation in the atomic and molecular phase: H I self absorption (HISA) towards a giant molecular filament. Astronomy and Astrophysics, . ISSN 0004-6361. E-ISSN 1432-0746. (doi:10.1051/0004-6361/201935866) (KAR id:79480)

PDF Author's Accepted Manuscript
Language: English
Download (26MB) Preview
[img]
Preview
Official URL
https://doi.org/10.1051/0004-6361/201935866

Abstract

Molecular clouds form from the atomic phase of the interstellar medium. However, characterizing the transition between the atomic and the molecular interstellar medium (ISM) is a difficult observational task. Here we address cloud formation processes by combining H I self absorption (HISA) with molecular line data. Column density probability density functions (N-PDFs) are a common tool to examine molecular clouds. One scenario proposed by numerical simulations is that the N-PDF evolves from a log-normal shape at early times to a power-law-like shape at later times. To date, investigations of N-PDFs are mostly limited to the molecular component of the cloud. In this paper, we study the cold atomic component of the giant molecular filament GMF38.1-32.4a (GMF38a, distance=3.4 kpc, length∼ 230 pc), calculate its N-PDFs and study its kinematics. We identify an extended HISA feature, which is partly correlated with the \(^{13}\)CO emission. The peak velocities of the HISA and \(^{13}\)CO observations agree well on the eastern side of the filament, whereas a velocity offset of approximately 4 km s\(^{−1}\) is found on the western side. The sonic Mach number we derive from the linewidth measurements shows that a large fraction of the HISA, which is ascribed to the cold neutral medium (CNM), is at subsonic and transonic velocities. The column density of the CNM part is on the order of 10\(^{20}\) to 10\(^{21}\) cm\(^{−2}\). The column density of molecular hydrogen, traced by \(^{13}\)CO, is an order of magnitude higher. The N-PDFs from HISA (CNM), H I emission (the warm and cold neutral medium), and \(^{13}\)CO (molecular component) are well described by log-normal functions, which is in agreement with turbulent motions being the main driver of cloud dynamics. The N-PDF of the molecular component also shows a power law in the high column-density region, indicating self-gravity. We suggest that we are witnessing two different evolutionary stages within the filament. The eastern subregion seems to be forming a molecular cloud out of the atomic gas, whereas the western subregion already shows high column density peaks, active star formation and evidence of related feedback processes.

Item Type: Article
DOI/Identification number: 10.1051/0004-6361/201935866
Uncontrolled keywords: ISM clouds ISM, atoms ISM, molecules Radio lines, ISM – Stars, formation
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: James Urquhart
Date Deposited: 06 Jan 2020 09:37 UTC
Last Modified: 15 Jun 2020 09:22 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/79480 (The current URI for this page, for reference purposes)
Urquhart, J.S.: https://orcid.org/0000-0002-1605-8050
  • Depositors only (login required):

Downloads

Downloads per month over past year