Gas and Star Formation from HD and Dust Emission in a Strongly Lensed Galaxy

TL;DR

This study investigates the molecular gas and dust properties of a high-redshift galaxy using multiple tracers, setting limits on gas mass and star formation, and providing detailed spectral energy distribution analysis.

Contribution

It introduces the use of hydrogen deuteride (HD) emission as a new molecular gas tracer at high redshift and provides comprehensive SED fitting for a strongly lensed galaxy.

Findings

Upper limit on H2 gas mass: <6.4×10^11 M_sun

Dust mass: 10^8.92 M_sun, temperature: 78.6 K

Star formation rate: 3800 M_sun/year

Abstract

The molecular gas content of high-redshift galaxies is a highly sought-after property. However, H$_2$ is not directly observable in most environments, so its mass is probed through other emission lines (e.g., CO, [CI], [CII]), or through a gas-to-dust ratio. Each of these methods depends on several assumptions, and are best used in parallel. In this work, we extend an additional molecular gas tracer to high-redshift studies by observing hydrogen deuteride (HD) emission in the strongly lensed $z=5.656$ galaxy SPT0346-52 with ALMA. While no HD(1-0) emission is detected, we are able to place an upper limit on the gas mass of $\rm M_{H_2}<6.4\times10^{11} M_{\odot}$. This is used to find a limit on the $\rm L'_{CO}$ conversion factor of $\rm\alpha_{CO}<5.8$ M$_{\odot}$(K km s$^{-1}$ pc$^2$)$^{-1}$. In addition, we construct the most complete spectral energy distribution (SED) of this source to date, and fit it with a single-temperature modified blackbody using the nested sampling code MultiNest, yielding a best-fit dust mass $\rm M_{dust}=10^{8.92\pm0.02}$ M$_{\odot}$, dust temperature $78.6\pm0.5$ K, dust emissivity spectral index $\beta=1.81\pm0.03$, and star formation rate $\rm SFR=3800\pm100$ M$_{\odot}$ year$^{-1}$. Using the continuum flux densities to estimate the total gas mass of the source, we find $\rm M_{H_2}<2.4\times10^{11}$ M$_{\odot}$, assuming sub-solar metallicity. This implies a CO conversion factor of $\rm \alpha_{CO}<2.2$, which is between the standard values for MW-like galaxies and starbursts. These properties confirm that SPT0346-52 is a heavily starbursting, gas rich galaxy.