Star Formation History of FUDS0 galaxies

HI mass upper limits are also calculated for 134 non-detections in the field. Stellar masses (M*), star formation rates (SFRs), and star formation histories are computed by fitting spectral energy distributions using ProSpect.

The results show that HI-selected galaxies prefer recent long-lasting, but mild star formation activity, while HI non-detections have earlier and more intense star formation activity. Based on their distribution on the SFR versus M* diagram, the typical evolution of HI-selected galaxies follows three distinct stages: (i) early stage: the total SFR increases, though the specific SFR decreases from 10^-8^ to 10^-9^/yr; (ii) mass accumulation stage: the SFR is steady, and stellar mass increase linearly with time; (iii) quenching stage: star formation activity quenches on a rapid timescale and at constant stellar mass. 37 non-detections are located on the star-forming main sequence, but are not detected in HI due to low sensitivity close to the field edges or close to strong radio frequency interference.