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Table 4

Analysis of the hot star 2–17.

N [Fe/H] from Teff (K) log g Excitation Δ [Fe/H]a Δ(B − V)0b Δ(V − I)0b Δlog gc assuming 2–17 belongs to M(M⊙)f
FeI FeII slope? BSS(1.92 M⊙)d BHB(0.6 M⊙)e
1  + 0.54  + 0.51 7400 4.18 NO  + 0.25  − 0.05  − 0.06  + 0.29  + 0.80 3.75
2  + 0.47  + 0.44 7300 4.03 NO  + 0.18  − 0.04  − 0.04  + 0.17  + 0.67 2.81
3  + 0.48  + 0.47 7200 3.91 NO  + 0.19 -0.02 -0.02  + 0.07  + 0.57 2.25
4  + 0.32  + 0.30 7100 3.68  + 1.1σ  + 0.03 -0.02  + 0.00  − 0.13  + 0.37 1.42
5  + 0.26  + 0.27 7000 3.62  + 1.6σ -0.03  − 0.01  + 0.02  − 0.16  + 0.34 1.31
6  + 0.18  + 0.18 6920 3.58  + 2.5σ  − 0.11  + 0.00  + 0.04  − 0.18  + 0.33 1.27

Notes. Table shows spectroscopic solutions N = 1–6. Boldface marks for a given indicator the solutions which are preferred. Italics mark the two solutions between which the highest amount of consistency can be obtained.

(a)

Measured [Fe/H] – mean cluster [Fe/H] from Paper I.

(b)

Difference between the colour predicted using the spectroscopic Teff with MARCS colour-temperature relations and the observed photometric colour dereddened assuming E(B − V) = 0.14 and E(V − I)/E(B − V) = 1.244.

(c)

Difference between the spectroscopic log g and log g calculated from the spectroscopic Teff and the luminosity obtained using the observed V-magnitude, (m − M)V = 13.51, MARCS BC and different assumptions of the mass.

(d)

Mass for an assumed BSS star obtained from the extended ZAMS and evolutionary tracks in Fig. 9.

(e)

Mass for an assumed BHB star. A mass of about 0.52 M⊙ is implied when comparing the colour of 2–17 to the model ZAHB. However, since in this scenario 2–17 does not lie on the ZAHB in Fig. 9, a somewhat higher mass of 0.6 M⊙ was chosen to be sure that the mass is not underestimated.

(f)

The mass of 2–17 derived from the spectroscopic Teff and log g in combination with luminosity obtained from the observed V-magnitude, (m − M)V = 13.51, and a MARCS BC.

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