期刊
ASTROPHYSICAL JOURNAL
卷 881, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab2bf5
关键词
galaxies: fundamental parameters; galaxies: star formation; infrared: galaxies
The bulk of the star formation rate (SFR) density peak at cosmic noon was obscured by dust. How accurately we can assess the role of dust-obscured star formation is affected by inherent biases in our empirical methods-both those that rely on direct dust emission and those that rely on the inferred dust attenuation of starlight. We use a library of hydrodynamic simulations with radiative transfer to explore these biases. We find that for infrared (IR) luminous galaxies that are in rapidly quenching systems (e. g., post-coalescence), standard luminosity-to-SFR relations can strongly overestimate the true SFRs. We propose using the L-IR/L-1.6 color to both help identify such systems and provide more accurate SFRs. Conversely, we find that the diagnostic rest-frame U-V versus V-J (UVJ) color-color plot misidentifies a subset of dusty star-forming galaxies. This is due to variability in the effective attenuation curves, including being much grayer in the optical-to-near-IR regime than the Calzetti starburst law. This is in agreement with recent observations of IR-selected galaxies at cosmic noon. Our results support the view that we need a panchromatic approach from the rest-frame UV through the IR and spectral energy distribution modeling that includes realistic star formation histories and allows for variable attenuation curves if we want to fully account for dust-obscured star formation across the epochs of the greatest galaxy build-up.
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