Exemplary QGCs from our final sample: Massive system on the left and a less massive one on the right. Top: CIGALE SEDs. Solid and dashed black lines show the best–fit SEDs for the same galaxy using the regulator SFH with and without JWST/MIRI photometry for the MIRI and no–MIRI runs, respectively. Blue circles are detections; triangles are 3σ upper limits. JWST cutouts are displayed above each SED. Shaded envelopes indicate the range of K–band–normalised SEDs for QGCs binned by median A_V; the legend lists the median A_V values and number of objects in each bin. Bottom: sSFHs for the same QGC from the MIRI run. The solid dark blue, dashed violet, and dash-dotted light blue lines correspond to the regulator, non-parametric, and delayedBQ models, respectively. The thick and thin dark-blue lines show the difference between MIRI and no-MIRI runs. The dotted black line marks the quiescent threshold and the dashed black line the star-forming threshold (following Pacifici et al. 2016). Arrows mark the quantities used in this work for the regulator model: the quenching time, T_q, the quenching moment, τ_q, the cosmic time at the observation redshift, τ(z_o), and the time since quenching, ΔT ≡ τ(z_o)−τ_q.