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The epoch when low-mass star forming galaxies (LMSFGs) form the bulk of theirstellar mass is uncertain. While some models predict an early formation, othersfavor a delayed scenario until later ages of the universe. We presentconstraints on the star formation histories (SFHs) of a sample of LMSFGsobtained through the analysis of their spectral energy distributions using anovel approach that (1) consistently combines photometric (broadband) andspectroscopic (equivalent widths of emission lines) data, and (2) usesphysically motivated SFHs with non-uniform variations of the star formationrate (SFR) as a function of time. The sample includes 31 spectroscopicallyconfirmed LMSFGs (7.3 < log M*/Msun < 8.0) at 0.3 < z_spec < 0.9 in theExtended-Chandra Deep Field-South field (E-CDF-S). Among them, 24 were selectedwith photometric stellar mass log M*/Msun < 8.0, 0.3 < z_phot < 1.0, and NB816< 26 AB mag; the remaining 7 were selected as blue compact dwarfs (BCDs) withinthe same photometric redshift and magnitude ranges. We also study a secondarysample of 43 more massive spectroscopically confirmed galaxies (8.0 < logM*/Msun < 9.1), selected with the same criteria. The SFRs and stellar massesderived for both samples place our targets on the standard main sequence ofstar forming galaxies. The median SFH of LMSFGs at intermediate redshiftsappears to form 90% of the median stellar mass inferred for the sample in the0.5-1.8 Gyr immediately preceding the observation. These results suggest arecent stellar mass assembly for LMSFGs, consistent with the cosmologicaldownsizing trends. We find similar median SFH timescales for the more massivesecondary sample.

Recent stellar mass assembly of low-mass star-forming galaxies at redshifts 0.3 < z < 0.9