Cloud formation in the atomic and molecular phase: H I self absorption (HISA) towards a giant molecular filament
Journal article, 2020

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 complex observational task. Here we address cloud formation processes by combining HI self absorption (HISA) with molecular line data. Column density probability density functions (N-PDFs) are a common tool for examining 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 have been 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 similar to 230 pc), calculate its N-PDFs, and study its kinematics. We identify an extended HISA feature, which is partly correlated with the (CO)-C-13 emission. The peak velocities of the HISA and (CO)-C-13 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 (CO)-C-13, is an order of magnitude higher. The N-PDFs from HISA (CNM), HI emission (the warm and cold neutral medium), and (CO)-C-13 (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.

ISM: clouds

stars: formation

radio lines: ISM

ISM: molecules

ISM: atoms


Y. Wang

Max Planck Society

S. Bihr

Max Planck Society

H. Beuther

Max Planck Society

M. R. Rugel

Max Planck Society

J. D. Soler

Max Planck Society

J. Ott

National Radio Astronomy Observatory Socorro

Jouni Kainulainen

Chalmers, Space, Earth and Environment, Astronomy and Plasmaphysics, Galactic Astrophysics

N. Schneider

University of Cologne

R. S. Klessen

Heidelberg University

S. C. O. Glover

Heidelberg University

N. M. McClure-Griffiths

Australian National University

P. F. Goldsmith

California Institute of Technology (Caltech)

K. G. Johnston

University of Leeds

K. M. Menten

Max Planck Society

S. Ragan

Cardiff University

L. D. Anderson

Green Bank Observ, POB 2

West Virginia University

J. S. Urquhart

University Of Kent

H. Linz

Max Planck Society

N. Roy

Indian Institute of Science

R. J. Smith

University of Manchester

F. Bigiel

Argelander-Institut für Astronomie

T. Henning

Max Planck Society

S. N. Longmore

Liverpool John Moores University

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 634 A139

Subject Categories

Physical Chemistry

Astronomy, Astrophysics and Cosmology

Theoretical Chemistry



More information

Latest update