Chemical Analysis of a Diffuse Cloud along a Line of Sight Toward W51: Molecular Fraction and Cosmic-Ray Ionization Rate

TL;DR

This study combines observations of OH+, H2O+, and H3+ molecules to analyze the chemical composition and cosmic-ray ionization rates in a diffuse cloud near W51, revealing lower-than-expected formation efficiencies.

Contribution

First comprehensive chemical analysis using all three molecules to determine molecular hydrogen fraction and cosmic-ray ionization rates in a diffuse cloud.

Findings

Cosmic-ray ionization rate of H in the cloud: (4.8±3.4)×10^-16 s^-1

Efficiency factor for OH+ formation: 0.07±0.04, lower than models predict

Combined molecular data improve understanding of cosmic-ray interactions in diffuse clouds

Abstract

Absorption lines from the molecules OH+, H2O+, and H3+ have been observed in a diffuse molecular cloud along a line of sight near W51 IRS2. We present the first chemical analysis that combines the information provided by all three of these species. Together, OH+ and H2O+ are used to determine the molecular hydrogen fraction in the outskirts of the observed cloud, as well as the cosmic-ray ionization rate of atomic hydrogen. H3+ is used to infer the cosmic-ray ionization rate of H2 in the molecular interior of the cloud, which we find to be zeta_2=(4.8+-3.4)x10^-16 per second. Combining the results from all three species we find an efficiency factor---defined as the ratio of the formation rate of OH+ to the cosmic-ray ionization rate of H---of epsilon=0.07+-0.04, much lower than predicted by chemical models. This is an important step in the future use of OH+ and H2O+ on their own as tracers of the cosmic-ray ionization rate.