Estimating dust temperature and Far-IR luminosity of high-redshift galaxies using ALMA single-band continuum observations

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(clp) = -1.02 +/- 0.41 may accurately represent the ISM of high-redshift star-forming galaxies. By assuming a value of xi(clp), our method enables the deri v ation 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-d = 95(-17)(+ 13) K) of a z similar to 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 multiband 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.