What is the nature of Little Red Dots and what is not, MIRI SMILES edition

We study little red dots (LRD) detected by JADES and covered by the SMILES MIRI survey. Our sample contains 31 sources, ∼70 bluest MIRI bands, 40 z=6.9_5.9^7.7 (55 through near/mid-infrared spectral energy distributions of LRDs combining NIRCam and MIRI observations, using a variety of modeling techniques that include emission from stars, dust, and (un)obscured active galactic nuclei (AGN). The NIRCam-MIRI colors, for ≥10 μm, are bluer than direct pure emission from AGN tori; the spectral slope flattens in the rest-frame near-infrared, consistent with a 1.6 μm stellar bump. Both observations imply that stellar emission makes the dominant contribution at these wavelengths, expediting a stellar mass estimation: the median/quartiles are logM_⋆/M_⊙=9.4_9.1^9.7. The number density of LRDs is 10^-4.0±0.1 Mpc^-3, accounting for 14±3 of galaxies with similar redshifts and masses. The flat ultraviolet spectral range is dominated by young stars. The rest-frame near/mid-infrared (2-4 μm) spectral slope reveals significant amounts of dust (bolometric stellar attenuation ∼3-4 mag) heated by strong radiation fields arising from highly embedded compact sources. Our models imply <0.4 kpc heating knots, containing dust-enshrouded OB stars or an AGN producing a similar radiation field, obscured by A(V)>10 mag. We conclude that LRDs are extremely intense and compact starburst galaxies with mass-weighted ages 5-10 Myr, very efficient in producing dust, their global energy output dominated by the direct and dust-recycled emission from OB stars, with some contribution from obscured AGN in the mid-infrared.