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Table 1.

Set of fictitious stars to be characterised by SPInS.

Star log(L/L) log(Teff) A (Gyr) M/M
SF1 0.00 3.76 7.12 ± 3.72 0.96 ± 0.05
SF2 0.25 3.80 1.76 ± 1.30 1.16 ± 0.04
SF3 0.25 3.77 8.30 ± 2.20 1.02 ± 0.04
SF4 0.50 3.80 3.20 ± 0.85 1.23 ± 0.04
SF5 0.50 3.75 7.54 ± 0.92 1.10 ± 0.04
SF6 0.50 3.70 9.34 ± 2.14 1.06 ± 0.06
SF7 0.83 3.80 2.49 ± 0.44 1.45 ± 0.06
SF8 1.00 3.90 0.50 ± 0.18 1.70 ± 0.04
SF9 1.00 3.80 2.00 ± 0.24 1.59 ± 0.06
SF10 1.00 3.70 4.80 ± 2.33 1.31 ± 0.15
SF11 1.50 4.00 0.15 ± 0.06 2.29 ± 0.05
SF12 1.50 3.90 0.74 ± 0.04 2.12 ± 0.05
SF13 1.50 3.70 1.82 ± 1.05 1.79 ± 0.27
SF14 2.00 4.10 0.04 ± 0.02 3.14 ± 0.06
SF15 2.00 4.00 0.33 ± 0.02 2.82 ± 0.06
SF16 2.00 3.70 0.53 ± 0.10 2.77 ± 0.13
SF17 3.00 4.25 0.02 ± 0.01 5.63 ± 0.09
SF18 3.00 4.15 0.08 ± 0.00 4.97 ± 0.11
SF19 3.00 3.90 0.11 ± 0.01 4.70 ± 0.13
SF20 3.00 3.70 0.13 ± 0.01 4.63 ± 0.13

Notes. Here, inputs to SPInS are log(L/L), log(Teff), and [M/H]. For all stars, we adopted a solar metallicity [M/H] = 0.00 ± 0.05 and the following uncertainties σlog(L/L) = 0.04 and σTeff = 100 K. The mass and age inferred by SPInS and their error bars are listed in Cols. 4 and 5.

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