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Figure: a three-color image of a portion of the studied field of view (top-left). The right panels show the F322W2 (top) and F115W (bottom) stacked images for the region within the yellow box highlighted in the field of view on the left panel. The color-magnitude diagram is shown in the bottom panel. The arrows indicate the location of the possible gaps or discontinuities along the sequence of ultracool 47 Tucanae stars. Stars fainter than m F322W2 ∼ 25.3 mag and with colors redder than m F115W − m F322W2 ∼ 1.5 mag are probable brown dwarfs. The blue and red circles in the CMD highlight two of them, which are also marked in the top-right panel.
Brown dwarf detection
Brown dwarf detection
The JWST data enabled, for the first time in a globular cluster, the direct observation of objects at the hydrogen-burning limit and of bona fide brown dwarfs in 47 Tucanae. This represents a major observational benchmark for constraining stellar evolution models. Results have been published in Marino et al. 2024, ApJ, 965, 189.
https://ui.adsabs.harvard.edu/abs/2024ApJ...965..189M/abstract
Multiple stellar populations in globular clusters
Multiple stellar populations in globular clusters
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