Renzini, A.Gennaro, M.Zoccali, M.Brown, T.M.Anderson, J.Minniti, D.Sahu, K.C.Valenti, E.Vandenberg, D.A.2019-11-282019-11-282018-08Astrophysical Journal, 863(1), art. no. 16.0004-637Xhttp://repositorio.unab.cl/xmlui/handle/ria/10877Indexación: Scopus.The Hubble Space Telescope/WFC3 multiband photometry spanning from the UV to the near-IR of four fields in the Galactic bulge, together with that for six template globular and open clusters, are used to photometrically tag the metallicity [Fe/H] of stars in these fields after proper-motion rejecting most foreground disk contaminants. Color-magnitude diagrams and luminosity functions (LF) are then constructed, in particular for the most metal-rich and most metal-poor stars in each field. We do not find any significant difference between the I-band and H-band LFs, hence turnoff luminosity and age of the metal-rich and metal-poor components therefore appear essentially coeval. In particular, we find that no more than ∼3% of the metal-rich component can be ∼5 Gyr old, or younger. Conversely, theoretical LFs match well to the observed ones for an age of ∼10 Gyr. Assuming this age is representative for the bulk of bulge stars, we then recall the observed properties of star-forming galaxies at 10 Gyr lookback time, i.e., at z ∼ 2, and speculate about bulge formation in that context. We argue that bar formation and buckling instabilities leading to the observed boxy/peanut, X-shaped bulge may have arisen late in the history of the Milky Way Galaxy, once its gas fraction had decreased compared to the high values typical of high-redshift galaxies. This paper follows the public release of the photometric and astrometric catalogs of the measured stars in the four fields. © 2018. The American Astronomical Society.enGalaxies: BulgesGalaxies: evolutionGalaxy: bulgeGalaxy: evolutionGlobular clusters: generalStars: AbundancesArtículo