Ubiquitous argonium (ArH$^{+}$) in the diffuse interstellar medium: A molecular tracer of almost purely atomic gas
Journal article, 2014

Aims: We describe the assignment of a previously unidentified interstellar absorption line to ArH+ and discuss its relevance in the context of hydride absorption in diffuse gas with a low H2 fraction. The confidence of the assignment to ArH+ is discussed, and the column densities are determined toward several lines of sight. The results are then discussed in the framework of chemical models, with the aim of explaining the observed column densities. Methods: We fitted the spectral lines with multiple velocity components, and determined column densities from the line-to-continuum ratio. The column densities of ArH+ were compared to those of other species, tracing interstellar medium (ISM) components with different H2 abundances. We constructed chemical models that take UV radiation and cosmic ray ionization into account. Results: Thanks to the detection of two isotopologues, 36ArH+ and 38ArH+, we are confident about the carrier assignment to ArH+. NeH+ is not detected with a limit of [NeH+]/[ArH+] ≤ 0.1. The derived column densities agree well with the predictions of chemical models. ArH+ is a unique tracer of gas with a fractional H2 abundance of 10-4 - 10-3 and shows little correlation to H2O+, which traces gas with a fractional H2 abundance of ≈0.1. Conclusions: A careful analysis of variations in the ArH+, OH+, H2O+, and HF column densities promises to be a faithful tracer of the distribution of the H2 fractional abundance by providing unique information on a poorly known phase in the cycle of interstellar matter and on its transition from atomic diffuse gas to dense molecular gas traced by CO emission. Abundances of these species put strong observational constraints upon magnetohydrodynamical (MHD)simulations of the interstellar medium, and potentially could evolve into a tool characterizing the ISM. Paradoxically, the ArH+ molecule is a better tracer of almost purely atomic hydrogen gas than Hi itself, since Hi can also be present in gas with a significant molecular content, but ArH+ singles out gas that is >99.9% atomic.

interstellar molecules

astrochemistry

interstellar matter

Author

P. Schilke

University of Cologne

D. A. Neufeld

Johns Hopkins University

H. S. P. Müller

University of Cologne

C. Comito

University of Cologne

E. A. Bergin

University of Michigan

D. C. Lis

California Institute of Technology (Caltech)

Pierre and Marie Curie University (UPMC)

M. Gerin

LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres

John H Black

Chalmers, Earth and Space Sciences, Radio Astronomy and Astrophysics

M. Wolfire

University of Maryland

N. Indriolo

Johns Hopkins University

J. C. Pearson

Jet Propulsion Laboratory, California Institute of Technology

K. M. Menten

Max Planck Institute

B. Winkel

Max Planck Institute

A. Sánchez-Monge

University of Cologne

T. Moller

University of Cologne

B. Godard

LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres

E. Falgarone

LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres

Astronomy and Astrophysics

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

Vol. 566 June 1-12 44

Subject Categories

Astronomy, Astrophysics and Cosmology

Atom and Molecular Physics and Optics

Roots

Basic sciences

Infrastructure

Onsala Space Observatory

DOI

10.1051/0004-6361/201423727

More information

Latest update

5/29/2018