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We study the debated contribution from thermally pulsing asymptotic giantbranch (TP-AGB) stars in evolutionary population synthesis models. Weinvestigate the Spectral Energy Distributions (SEDs) of a sample of 51spectroscopically confirmed, high-z ($1.3<z_{\rm spec}<2.7$), galaxies usingthree evolutionary population synthesis models with strong, mild and lightTP-AGB. Our sample is the largest of spectroscopically confirmed galaxies onwhich such models are tested so far. Galaxies were selected as passive, but wemodel them using a variety of star formation histories in order not to bedependent on this pre-selection.  We find that the observed SEDs are best fitted with a significantcontribution of TP-AGB stars or with substantial dust attenuation. Withoutincluding reddening, TP-AGB-strong models perform better and deliver solutionsconsistent within $1\sigma$ from the best-fit ones in the vast majority ofcases. Including reddening, all models perform similarly. Using independentconstraints from observations in the mid- and far-IR, we show thatlow/negligible dust attenuation, i.e. $E(B-V)\lesssim 0.05$ , should bepreferred for the SEDs of passively-selected galaxies. Given that TP-AGB-lightmodels give systematically older ages for passive galaxies, we suggest numbercounts of passive galaxies at higher redshifts as a further test todiscriminate among stellar population models.

Revisiting the role of the Thermally-Pulsating Asymptotic Giant Branch phase in high-redshift galaxies