A new census of dust and polycyclic aromatic hydrocarbons at z=0.7-2 with JWST MIRI

Irene Shivaei, Stacey Alberts, Michael Florian, George Rieke, Stijn Wuyts, Sarah Bodansky, Andrew J. Bunker, Alex J. Cameron, Mirko Curti, Francesco D'Eugenio, Ugne Dudzeviciute, Ivan Kramarenko, Zhiyuan Ji, Benjamin D. Johnson, Jianwei Lyu, Jorryt Matthee, Jane Morrison, Rohan Naidu, Naveen Reddy, Brant Robertson, Pablo G. Pérez-González, Yang Sun, Sandro Tacchella, Katherine Whitaker, Christina C. Williams, Christopher N. A. Willmer, Joris Witstok, Mengyuan Xiao, Yongda Zhu

Published 2024-02-12, updated 2024-09-08Version 2

This paper utilizes the JWST MIRI multi-band imaging data from the SMILES survey (5-25micron), complemented with HST and NIRCam photometric and spectroscopic data from the JADES and FRESCO surveys for 443 star-forming (non-AGN) galaxies at z=0.7-2.0 to extend the study of dust and PAH emission to a new mass and SFR parameter space beyond our local universe. We find a strong correlation between the fraction of dust in PAHs (PAH fraction, q_PAH) with stellar mass. Moreover, the PAH fraction behavior as a function of gas-phase metallicity is similar to that at z~0 from previous studies, suggesting a universal relation: q_PAH is constant (~3.4%) above a metallicity of ~ 0.5$Z_{\odot}$ and decreases to <1% at metallicities $<0.3Z_{\odot}$. This indicates that metallicity is a good indicator of the ISM properties that affect the balance between the formation and destruction of PAHs. The lack of a redshift evolution from z~0-2 also implies that above $0.5\,Z_{\odot}$, the PAH emission effectively traces obscured luminosity and the previous locally-calibrated PAH-SFR calibrations remain applicable in this metallicity regime. We observe a strong correlation between obscured UV luminosity fraction (ratio of obscured to total luminosity) and stellar mass. Above the stellar mass of $>5\times 10^9M_{\odot}$, on average, more than half of the emitted luminosity is obscured, while there exists a non-negligible population of lower mass galaxies with >50% obscured fractions. At a fixed mass, the obscured fraction correlates with SFR surface density. This is a result of higher dust covering fractions in galaxies with more compact star forming regions. Similarly, galaxies with high IRX (IR to UV luminosity) at a given mass or UV continuum slope tend to have higher SFR surface density and shallower attenuation curves, owing to their higher effective dust optical depths and more compact star forming regions.