Estimating Dust Temperature and Far-IR Luminosity of High-Redshift Galaxies using ALMA Single-Band Continuum Observations

Abstract

We present a method that derives the dust temperatures and infrared (IR) luminosities of high-redshift galaxies assuming radiation equilibrium in a simple dust and stellar distribution geometry. Using public data from the Atacama Large Millimeter/submillimeter Array (ALMA) archive, we studied dust temperatures assuming a clumpy interstellar medium (ISM) model for high-redshift galaxies, then tested the consistency of our results with those obtained using other methods. We find that a dust distribution model assuming a clumpiness of $\log {\xi }_{\mathrm{clp}}=-1.02\pm 0.41$ may accurately represent the ISM of high-redshift star-forming galaxies. By assuming a value of ${\xi }_{\mathrm{clp}}$, our method enables the derivation of dust temperatures and IR luminosities of high-redshift galaxies from dust continuum fluxes and emission sizes obtained from single-band ALMA observations. to demonstrate the method proposed herein, we determined the dust temperature ($T_{\mathrm{d}}=95_{-17}^{+13}\mathrm{K}$) of a $z\sim 8.3$ star-forming galaxy, MACS0416-Y1. Because the method only requires a single-band dust observation to derive a dust temperature, it is more easily accessible than multi-band observations or high-redshift emission line searches and can be applied to large samples of galaxies in future studies using high resolution interferometers such as ALMA.

Accepted for publication in MNRAS, 8 pages, 3 figures, For our public python scripts, see https://github.com/yfudamoto/FIS22sed.git

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• GA-NIFS: Multi-phase analysis of a star-forming galaxy at $z\sim 5.5$
• Behind the dust veil: A panchromatic view of an optically dark galaxy at z=4.82
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