0 Assigned ID: 6329 ----- Attempting Submission 1 (Thu Apr 10 00:35:06 GMT 2025) ----- HST Phase I Proposal 6329 successfully submitted. Receipt: # 6329-1 ----- Attempting Submission 2 (Thu Apr 10 23:57:15 GMT 2025) ----- 0 ----- Attempting Submission 1 (Thu Jul 24 14:22:01 GMT 2025) ----- ----- Attempting Submission 2 (Mon Dec 01 22:55:48 GMT 2025) ----- The most-massive globular cluster in the Fornax dSph to shed light on the mass-budget problem of multiple populations. This proposal is aimed at constraining the mass budget problem related to the multiple populations (MPs) in globular clusters (GCs). Discoveries, largely made by HST, have clarified that MPs are ubiquitous in Milky Way and in Fornax GCs. One of the most acknowledged scenarios predicts that MPs are different stellar generations. To account for the low fractions of first-population stars (1P), which is the mass-budget problem, proto-GCs must have been significantly more massive, with the missing 1P stars lost in the assembly of the Galactic Halo. While MPs have been found in Fornax GCs, there could not be enough stars in the field of this galaxy to account for much more massive proto-GCs. Unless high fractions of 1P stars will suggest that Fornax GCs did not lose significant mass, MPs in Fornax will challenge the multiple-generation scenario. We propose to analyze the MPs in Fornax 3 and obtain, for the first time, the proper photometric diagrams to disentangle 1P and 2P stars and to infer accurate population fractions. With a mass comparable to Galactic GCs, Fornax 3 is ideal to constrain the mass-budget problem. The multiple-generation scenario predicts that the amount of lost 1P stars is higher in massive GCs. Moreover, it is placed in the low-metallicity tail of the field distribution, which comprises a small number of stars. In the end, a low fraction of 1P stars, similar to Milky Way GCs, will challenge the multiple generations scenario. On the contrary, if this scenario is correct, we expect a predominance of 1P stars. In both cases, our results will help in solving the mass budget conundrum. We propose UVIS/WFC3 observations of the distant globular cluster Fornax 3 in the filters F336W, F343N, F438W, and F814W. We centered the cluster in the middle of the UVIS2 detector and dithered the exposures. Observations are split intoo 15 visits to maximize flexibillity. Our team comprises internationally distinguished scientists who have made substantial contribution to the field of multiple populations in GCs. The strength of the present proposal is to put together the potentials of experts in observational techniques such as photometry, astrometry and spectroscopy with stellar evolution models to investigate a key topic of outstanding interest in stellar and Galactic astronomy. We have all the necessary personnel, experience and tools to perform a timely and careful data reduction and analysis of the results. Indeed, our team includes scientists who are spearheads in the analysis of HST data, in stellar models and in the scenarios on the formation of multiple populations: -- G. Cordoni, E. Dondoglio, M. Legnardi, E. Lagioia, C. Li, M. Carlos, A. F. Marino, A. P. Milone, and A. Mohandasan have a long experience in photometric, spectroscopic and astrometric data analysis. They have developed the methods for data analysis that are the state-of-the-art for studies on multiple populations in GCs, including the method for the determination of the incidence of binaries among multiple populations. This dataset will be of foundamental importance for the thesis of F. Muratore and E. Bortolan who are working on photometry of multiple stellar populations. -- A. Dotter, S. Jang, M. Tailo are among the major experts on kinematics and photometry in stellar evolution and dynamical models crucial to understand how multiple populations formed and evolved. Stellar Populations and the Interstellar Medium 6 false false false false false false SUPPORTED STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F343N WFC3/UVIS Imaging No No F336W /tmp/OPVisit13249043991855239103.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. 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