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Fundamental parameters and time-evolution of mass loss are investigated forpost-main-sequence stars in the Galactic globular cluster 47 Tucanae (NGC 104).This is accomplished by fitting spectral energy distributions (SEDs) toexisting optical and infrared photometry and spectroscopy, to produce a trueHertzsprung--Russell diagram. We confirm the cluster's distance as 4611 (+213,-200) pc and age as 12 +/- 1 Gyr. Horizontal branch models appear to confirmthat no more RGB mass loss occurs in 47 Tuc than in the more-metal-poor omegaCentauri, though difficulties arise due to inconsistencies between the models.Using our SEDs, we identify those stars which exhibit infrared excess, findingexcess only among the brightest giants: dusty mass loss begins at a luminosityof ~ 1000 Lsun, becoming ubiquitous above 2000 Lsun. Recent claims of dustproduction around lower-luminosity giants cannot be reproduced, despite usingthe same archival Spitzer imagery.

Fundamental parameters, integrated RGB mass loss and dust production in the Galactic globular cluster 47 Tucanae