Calibrating Column Density Tracers with Gamma-ray Observations of the $\rho$ Ophiuchi Molecular Cloud

TL;DR

This study evaluates various gas column density tracers using gamma-ray observations of the $ ho$ Ophiuchi cloud, confirming the importance of extit{HI} and H$_2$ tracers and identifying $ au_{353}$ as the most effective overall.

Contribution

It systematically compares column density tracers against gamma-ray data to improve gas mapping in molecular clouds, highlighting the effectiveness of $ au_{353}$ and infrared extinction.

Findings

$ au_{353}$ best reproduces gamma-ray data overall.

Both extit{HI} and H$_2$ tracers are necessary for accurate modeling.

Infrared stellar extinction performs well in dense regions.

Abstract

Diffuse gamma-ray emission from interstellar clouds results largely from cosmic ray (CR) proton collisions with ambient gas, regardless of the gas state, temperature, or dust properties of the cloud. The interstellar medium is predominantly transparent to both CRs and gamma-rays, so GeV emission is a unique probe of the total gas column density. The gamma-ray emissivity of a cloud of known column density is then a measure of the impinging CR population and may be used to map the kpc-scale CR distribution in the Galaxy. To this end, we test a number of commonly used column density tracers to evaluate their effectiveness in modeling the GeV emission from the relatively quiescent, nearby $\rho$ Ophiuchi molecular cloud. We confirm that both \hi\ and an appropriate H$_2$ tracer are required to reproduce the total gas column densities probed by diffuse gamma-ray emisison. We find that the optical depth at 353 GHz $\tau_{353}$ from Planck reproduces the gamma-ray data best overall based on the test statistic across the entire region of interest, but near infrared stellar extinction also performs very well, with smaller spatial residuals in the densest parts of the cloud.