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

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 ${\mathrm{M}}_{{\mathrm{H}}_2}<6.4\times 10^{11}{\mathrm{M}}_{\odot }$. This is used to find a limit on the ${\mathrm{L}}_{\mathrm{CO}}^{\prime }$ conversion factor of ${\alpha }_{\mathrm{CO}}<5.8$ 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 ${\mathrm{M}}_{\mathrm{dust}}=10^{8.92\pm 0.02}$ M${}_{\odot }$, dust temperature $78.6\pm 0.5$ K, dust emissivity spectral index $\beta =1.81\pm 0.03$, and star formation rate $\mathrm{SFR}=3800\pm 100$ M${}_{\odot }$ year${}^{-1}$. Using the continuum flux densities to estimate the total gas mass of the source, we find ${\mathrm{M}}_{{\mathrm{H}}_2}<2.4\times 10^{11}$ M${}_{\odot }$, assuming sub-solar metallicity. This implies a CO conversion factor of ${\alpha }_{\mathrm{CO}}<2.2$, 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.

arXiv comment11 pages, 6 figures. Accepted for publication in MNRAS

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