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Near-ultraviolet (NUV) spectroscopic studies have suggested that passivelyevolving massive, early-type galaxies host sub-one percent fractions of youngstars in their innermost regions. We shed light on the origin of these stars byanalysing NGC 1277, a widely studied nearby prototypical massive compact relicgalaxy. These are rare galaxies that have survived without experiencingsignificant size evolution via accretion and mergers since their formation athigh redshift. We obtain a spectrum in the UV range within the central 1 kpcregion of NGC 1277. We compare a carefully selected set of optical and NUVline-strengths to model predictions with star formation historiescharacteristic of massive galaxies. We find a 0.8% mass fraction of young starsin the centre of NGC 1277, similar to that found in massive early-typegalaxies. Given the limited accretion history of NGC 1277, these results favouran intrinsic, in-situ, process triggering star formation at later epochs. Ourresults suggest a general constraint on the amount of young stars in the coresof massive early-type galaxies. This amount should be assumed as an upper limitfor the young stellar contribution in massive galaxies, as there might bepresent other contributions from evolved stars.

Lessons from the massive relic NGC 1277: remaining in-situ star formation in the cores of massive galaxies