Not just PAH${}_{3.3}$: why galaxies turn red in the Near-Infrared

Abstract

We measure the spectral properties of a sample of 20 galaxies at z~0.35 selected for having surprisingly red JWST/NIRCAM F200W-F444W colors. 19 galaxies were observed with JWST/NIRSpec in the PRISM configuration, while one galaxy was observed with the high resolution gratings. 17/20 galaxies in our sample exhibit strong 3.3 $\mu m$ polycyclic aromatic hydrocarbon (PAH${}_{3.3}$) emission (equivalent width EW(PAH${}_{3.3}$)$>0.03\mu m$). In these galaxies, the strength of the color excess does not depend on environment and it correlates with EW(PAH${}_{3.3}$). Nonetheless, the presence of the PAH${}_{3.3}$ alone can not fully explain the color excess, as an equivalent width of ~0.1$\mu m$ is able to increase the color of galaxies by only 0.13 mag. A contribution from a hot dust component is required to explain the excess. Both the EW(PAH${}_{3.3}$) and flux correlate with the H$\alpha$ equivalent width and flux, suggesting that they are produced by the same mechanism. 5/20 galaxies showing PAH would be classified as passive based on broad band rest frame colors ((B-V) and/or UVJ diagrams) and are hence "faux-passive". Of these, 3 galaxies have a significantly lower EW(PAH${}_{3.3}$) given their color and also have low EW(H$\alpha$) and we tentatively conclude this behaviour is due to the presence of an AGN. The three galaxies with no PAH${}_{3.3}$ in emission have passive spectra, as do the 8 galaxies in our sample with normal F200W-F444W colors. We therefore conclude that the PAH${}_{3.3}$ feature is linked to dust-enshrouded star formation. The dust corrected SFR from PAH${}_{3.3}$ is a factor of 3.5 higher than the SFR obtained from H$\alpha$, suggesting that these galaxies are characterized by significant amounts of dust.

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