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Abstract Some recent literature has claimed there to be an evolution in galaxies’ dust temperatures toward warmer (or colder) spectral energy distributions (SEDs) between low and high redshift. These conclusions are driven by both theoretical models and empirical measurement. Such claims sometimes contradict one another and are prone to biases in samples or SED fitting techniques. What has made direct comparisons difficult is that there is no uniform approach to fitting galaxies’ infrared/millimeter SEDs. Here we aim to standardize the measurement of galaxies’ dust temperatures with a python-based SED fitting procedure, MCIRSED. 1 1 Publicly available at github.com/pdrew32/mcirsed . We draw on reference data sets observed by Infrared Astronomical Satellite, Herschel, and Scuba-2 to test for redshift evolution out to z ∼ 2. We anchor our work to the L IR – λ peak plane, where there is an empirically observed anticorrelation between IR luminosity and rest-frame peak wavelength (an observational proxy for luminosity-weighted dust temperature) such that λ peak = λ t ( L IR / L t ) η where η = −0.09 ± 0.01, L t = 10 12 L ⊙ , and λ t = 92 ± 2 μ m. We find no evidence for redshift evolution of galaxies’ temperatures, or λ peak , at fixed L IR from 0 99.99% confidence. Our finding does not preclude evolution in dust temperatures at fixed stellar mass, which is expected from a nonevolving L IR – λ peak relation and a strongly evolving SFR–M ⋆ relation. The breadth of dust temperatures ( σ log λ peak ) at a given L IR is likely driven by variation in galaxies’ dust geometries and sizes, and it does not evolve. Testing for L IR – λ peak evolution toward higher redshift ( z ∼ 5−6) requires better sampling of galaxies’ dust SEDs near their peaks (observed ∼200–600 μ m) with ≲1 mJy sensitivity. This poses a significant challenge to current instrumentation.
Drew et al. (Sun,) studied this question.