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We constrain the stellar population properties of a sample of 52 massivegalaxies, with stellar mass log Ms>10.5, over the redshift range 0.5<z<2 by useof observer-frame optical and near-infrared slitless spectra from HST's ACS andWFC3 grisms. The deep exposures (~100 ks) allow us to target individual spectraof massive galaxies to F160W=22.5AB. Our spectral fitting approach uses a setof six base models adapted to the redshift and spectral resolution of eachobservation, and fits the weights of the base models, including potential dustattenuation, via an MCMC method. Our sample comprises a mixed distribution ofquiescent (19) and star-forming galaxies (33). We quantify the width of the agedistribution (Dt) that is found to dominate the variance of the retrievedparameters according to Principal Component Analysis. The population parametersfollow the expected trend towards older ages with increasing mass, and Dtappears to weakly anti-correlate with stellar mass, suggesting a more efficientstar formation at the massive end. As expected, the redshift dependence of therelative stellar age (measured in units of the age of the Universe at thesource) in the quiescent sample rejects the hypothesis of a single burst (akamonolithic collapse). Radial colour gradients within each galaxy are alsoexplored, finding a wider scatter in the star-forming subsample, but noconclusive trend with respect to the population parameters.

FIGS: Spectral fitting constraints on the star formation history of massive galaxies since Cosmic Noon