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Late bloomers are massive ($M_* >10^{10}\,M_\odot$) galaxies at $z<1$ thatformed the majority of their stars within $\sim$2 Gyr of the epoch ofobservation. Our improved methodology for deriving star formation histories(SFHs) of galaxies at redshifts $0.45 < z < 0.75$ from theCarnegie-Spitzer-IMACS Survey includes confidence intervals that robustlydistinguish late bloomers from "old" galaxies. We use simulated SFHs to testfor "false positives" and contamination from old galaxies to demonstrate thatthe late bloomer population is not an artifact of our template modelingtechnique. We show that late bloomers account for $\sim$20% of $z\sim0.6$galaxies with masses of the modern Milky Way, with a moderate dependence onmass. We take advantage of a 1% overlap of our sample with HST (CANDELS)imaging to construct a "gold standard" catalog of 74 galaxies withhigh-confidence SFHs, SEDs, basic data, and HST images to facilitate comparisonwith future studies by others. This small subset suggests that galaxies withboth old and young SFHs cover the full range of morphology and environment(excluding rich groups or clusters), albeit with a mild but suggestivecorrelation with local environment. We begin the investigation of whether latebloomers of sufficient mass and frequency are produced in current-generation$\Lambda$CDM-based semi-analytic models of galaxy formation. In terms of halogrowth, we find a late-assembling halo fraction within a factor-of-two of ourlate bloomer fraction. However, sufficiently delaying star formation in suchhalos may be a challenge for the baryon component of such models.

Late Bloomer Galaxies: Growing Up in Cosmic Autumn