Table 1.
Mass limits for a selection of studies of the IMF outside the Milky Way with the Hubble Space Telescope.
| Galaxy | Target | Distance | Mass range | IMF slope(s) | Break mass | Reference |
|---|---|---|---|---|---|---|
| (kpc) | (M⊙) | (M⊙) | ||||
| LMC | R136 | 50 | 2.8–15 | 2.22 | 1 | |
| LMC | NGC 1818 | 50 | 0.85–9 | 2.23 | 2 | |
| LMC | R136 | 50 | 1.35–6.5 | 2.28, 1.27 | 2.1 | 3 |
| LMC | LH 95 | 50 | 0.43–20 | 2.05, 1.05 | 1.1 | 4 |
| SMC | NGC 330 | 62 | 1–7 | 2.3 | 5 | |
| SMC | NGC 602 | 62 | 1–45 | 2.2 | 6 | |
| SMC | 62 | 0.37–0.93 | 1.9 | 7 | ||
| Hercules | 135 | 0.52–0.78 | 1.2 | 8 | ||
| Leo IV | 156 | 0.54–0.77 | 1.3 | 8 | ||
| Leo I* | 250 | 0.6–30 | 2.3 | 9 | ||
Notes. For the study by Gallart et al. (1999), the estimated global star formation history was consistent with a Salpeter slope. The Salpeter slope was not extracted from the photometric data.
References. (1) Hunter et al. (1995); (2) Hunter et al. (1997); (3) Sirianni et al. (2000); (4) Da Rio et al. (2009); (5) Sirianni et al. (2002); (6) Schmalzl et al. (2008); (7) Kalirai et al. (2013); (8) Geha et al. (2013); (9) Gallart et al. (1999).
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