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Table B.1

Properties of the analyzed LMC stars.

Star Number T eff M evol τ H t N t isochrone Binary Class
km s-1 K M ⊙ dex Myr Myr Myr
N 11–34 L1 203 25 500 20 7.12 7.5 1.00 – 7.8 yes 1
N 11–37 L2 100 28 100 23  ≤7.17 6.2 0.76  ≥ 0.76 6.2 6.8 yes 2
N 11–46 L3 205 33 500 28  ≤7.71 5.1 0.88  ≥ 0.88 5.1-2.5 4.8 yes 2
N 11–77 L4 117 21 500 12 6.96 16.0 0.90 0.89 16.0-16.0 15.4 yes 2
N 11–88 L5 240 24 150 14  ≤6.96 12.6 1.00 – 12.6 – 1
N 11–89 L6 117 21 700 12 6.91 16.0 1.00 – 16.4 yes 1
N 11–95 L7 267 26 800 15 7.46 11.4 1.00 – 10.4 – 1
N 11–102 L8 218 31 000 18  ≤7.58 8.6 1.00 – 7.0 – 1
N 11–104 L9 153 25 700 14  ≤7.20 12.5 0.99  ≥0.97 12.5-4.2 11.8 – 2
N 11–111 L10 101 22 950 12 6.93 16.0 0.83 0.81 16.0-16.0 15.4 – 2
N 11–114 L11 299 32 500 19  ≤7.92 8.2 0.91  ≥0.90 8.2-4.7 5.8 – 2
N 11–116 L12 160 21 700 11 6.98 18.6 1.00 – 18.4 – 1
N 11–117 L13 247 26 800 13  ≤7.06 14.2 1.00 – 11.2 – 1
N 11–118 L14 150 25 700 13 7.39 14.1 0.83 0.79 14.1 12.6 yes 2
N 11–120 L15 207 31 500 17  ≤7.56 9.3 1.00 0.91 6.4 – 1
N 11–121 L16 265 27 000 14  ≤7.48 12.6 1.00 – 11.2 – 1
N 11–122 L17 173 33 000 18  ≤7.72 8.6 0.68  ≥ 0.61 8.6 4.6 – 2
NGC 2004–20 L18 145 22 950 18 7.46 8.6 0.83 0.83 8.6 9.6 yes 2
NGC 2004–30 L19 123 29 000 19 7.43 7.9 0.71 0.71 7.9 7.6 yes 2
NGC 2004–47 L20 133 21 700 12 7.03 16.0 0.94 0.94 16.0-16.0 16.4 yes 2
NGC 2004–50 L21 109 20 450 11 7.10 18.6 0.71 0.68 18.6-18.6 17.0 yes 2
NGC 2004–54 L22 114 21 700 12 6.97 16.0 0.86 0.86 16.0-16.0 16.4 yes 2
NGC 2004–62 L23 106 31 750 17  ≤7.33 9.3 0.67  ≥ 0.61 9.3 7.6 – 2
NGC 2004–63 L24 107 21 700 11 6.97 18.6 0.79 0.79 18.6-18.6 18.0 – 2
NGC 2004–65 L25 223 20 450 11  ≤7.19 18.7 1.00 – 19.8 – 1
NGC 2004–66 L26 238 25 700 13 7.98 14.2 0.60 0.59 14.2 12.0 – 2
NGC 2004–69 L27 178 28 000 15 7.84 11.2 0.57 0.56 11.2 9.8 – 2
NGC 2004–74 L28 130 27 375 14  ≤7.42 12.5 0.72  ≥ 0.67 12.5 10.6 yes 2
NGC 2004–75 L29 116 21 700 11 7.06 18.6 0.78 0.77 18.4-18.6 18.0 – 2
NGC 2004–77 L30 215 29 500 16 7.65 10.2 0.93 0.90 10.2-3.6 8.4 – 2
NGC 2004–79 L31 165 21 700 11 7.60 18.6 0.70 0.70 18.6 18.4 yes 2
NGC 2004–81 L32 105 26 800 13 7.14 14.0 0.70 0.63 14.0 11.2 – 2
NGC 2004–82 L33 161 25 700 13 7.47 14.1 0.83 0.79 14.1 12.6 – 2
NGC 2004–85 L34 150 20 450 10 7.25 22.0 0.85 0.84 22.0 21.4 – 2
NGC 2004–88 L35 200 20 450 10  ≤7.18 22.0 1.00 – 21.6 yes 1
NGC 2004–95 L36 138 25 700 13 7.13 14.1 0.92 0.89 14.1-4.8 12.8 – 2
NGC 2004–99 L37 119 21 700 10 7.06 22.0 0.78 0.74 22.0-22.0 19.6 – 2
NGC 2004–100 L38 323 26 800 13  ≤7.29 14.5 1.00 – 11.6 – 1
NGC 2004–101 L39 131 21 700 10 7.59 22.0 0.55 0.53 22.0 19.6 – 2
NGC 2004–104 L40 274 25 700 12  ≤7.28 16.3 1.00 – 13.2 – 1
NGC 2004–105 L41 235 25 700 12  ≤7.11 16.2 1.00 – 13.2 – 1
NGC 2004–107 L42 146 28 500 14  ≤7.12 12.5 1.00 0.88 9.4 yes 1
NGC 2004–110 L43 121 21 700 10 6.95 22.0 0.91 0.87 22.0-22.0 19.4 – 2
NGC 2004–113 L44 307 20 450 9  ≤7.29 27.1 1.00 – 22.2 – 1

Notes. From left to right: the table includes catalogue number (Evans et al. 2005), reference number used in this paper, projected surface rotational velocity, effective temperature, evolutionary mass and surface nitrogen abundance (all from Hunter et al. 2008b, 2009), main sequence lifetime, nitrogen inclination angle, inclination angle derived using the nitrogen abundance and the isochrone age, maximum age based on the surface nitrogen abundance, isochrone age, identification of binarity and class. For Class 2 stars, adopting an error in the nitrogen abundance does not lead to an increased upper age limit, and in many cases also not to an decreased lower age limit.

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