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Table 7

Two-segment fits to the IMFs.

Distance Age Γ1 Mass Reduced Γ2 Mass Reduced Γ3 b Mass Upper
modulus range χ 2 range χ 2 range mass
(mag) (Myr) (M⊙) (M⊙) (M⊙) (M⊙)
Star selection: reddening interval 3.2 <AV< 15
11.15 1 − 1.7 ± 0.2 6–80 1.1 − 0.21 ± 0.03 0.1–1.5 0.7 − 1.9 ± 0.2 6–77 78
11.15 3 − 2.0 ± 0.1 4–80 2.4 − 0.25 ± 0.05 0.4–1.7 1.6 − 2.0 ± 0.2 4–77 77
11.15 1a − 1.5 ± 0.1 3–80 0.4 – – – − 1.8 ± 0.1 2–53c 53
11.15 1a − 1.57 ± 0.04 0.6–80 0.8 – – – – – –
12 1 − 1.7 ± 0.1 6–124 1.3 − 0.10 ± 0.04 0.4–2 0.5 − 1.8 ± 0.2 6–138 138
12 3 − 2.1 ± 0.1 4–124 3.8 0.08 ± 0.07 0.8–2 2.8 − 2.1 ± 0.1 4–138 138
Star selection: reddening interval 3.2 <AV< 7.8
11.15 1 − 1.2 ± 0.3 6–80 0.1 − 0.3 ± 0.1 0.2–1.5 0.9 − 1.3 ± 0.4 6–77 79
11.15 3 − 1.1 ± 0.2 3–80 0.1 − 0.3 ± 0.2 0.4–1.7 0.1 − 1.2 ± 0.2 4–77 79
11.15 1a − 1.0 ± 0.2 5–80 0.07 – – – − 0.9 ± 0.2 4–53c 54
11.15 1a − 1.4 ± 0.1 1–100 1.2 – – – – – –
12 1 − 0.8 ± 0.2 5–160 0.3 − 0.3 ± 0.2 0.5–2 0.2 − 1.0 ± 0.2 6.5–138 142
12 3 − 1.1 ± 0.2 3–160 0.5 − 0.2 ± 0.2 0.6–2 0.3 − 1.1 ± 0.2 4–138 140

Notes.

(a)

Main Sequence tracks of Lejeune & Schaerer (2001);

(b)

modified Maximum Likelihood estimator (Maschberger & Kroupa 2009).

(c)

The upper limit is the mass of the actual second most massive stars, whereas for Γ1 the midpoint of the bin containing the second most massive star is used.

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