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Table 2

Spectral classification for the brightest cluster members.

# RA Dec V V–I M V a EW EW EW EW EW EW EW E(B–V) E(B–V) SpT Remark
Hα Hβ CaII8542 OI7774 NaI5889 DIB5781 DIB5797 B . D . b SpT c
(h m s) (°′′′) (mag) (mag) (mag) (Å) (Å) (Å) (Å) (Å) (Å) (Å) (mag) (mag)
1 6 18 45.52 15 16 52.25 11.95 1.64 −7.23 −611.71 −71.67 – −2.29 0.27 0.75 0.37 1.5 ~1.8 sgB[e]d MWC 137
2 6 18 43.31 15 16 42.44 14.76 0.71 −2.56 6.57 6.72 – 0.33 0.68 0.80 0.24 1.5 1.2 B2–4V He I abs.
3 6 18 44.64 15 17 13.36 16.09 0.64 −1.23 7.45 8.67 – 0.43 0.64 0.82 0.26 1.2 1.2 B3–5V He I abs.
4 6 18 45.50 15 16 58.29 16.91 0.85 −1.03 −9.38 11.71 – 0.70 0.81 0.76 0.25 1.5 1.4 B8–9V Hα em.
5 6 18 46.30 15 16 54.97 17.20 0.77 −0.12 9.71 8.71 – 0.04 0.77 0.78 0.26 1.5 1.2 B6–8V
6 6 18 45.24 15 16 50.75 17.35 1.01 0.03 12.15 9.15 – 0.37 0.89 0.77 0.23 1.4 1.2 B7–8V
7 6 18 46.10 15 16 43.25 17.70 0.94 0.38 10.68 10.00 – 0.40 0.81 0.74 0.25 1.5 1.2 B8–9V
8 6 18 45.19 15 16 52.34 17.70 1.22 −0.24 7.38 8.69 – 0.25 0.74 0.83 0.24 1.5 1.4 B7–8V
9 6 18 48.40 15 16 51.23 17.83 1.02 0.51 8.99 11.32 – 0.64 0.81 0.75 0.23 1.5 1.2 B8–9V
10 6 18 45.08 15 16 51.74 17.93 1.01 0.61 12.94 11.56 – 0.49 0.64 0.74 0.25 1.4 1.2 B8–9V
11 6 18 42.52 15 16 54.46 18.03 0.84 1.33 14.55 16.18 – 0.83 0.78 0.82 0.24 1.4 1.0 A1–3V
12 6 18 47.50 15 17 16.17 18.12 1.36 –0.44 8.89 9.56 – 0.57 0.86 0.81 0.22 1.6 1.6 B8–9V
13 6 18 45.19 15 16 55.79 18.16 0.88 0.22 6.73 12.45 – 0.23 0.75 0.88 0.28 1.5 1.4 B8–9V
14 6 18 42.10 15 16 56.77 18.36 0.84 1.66 13.41 15.74 – 1.12 0.34 0.75 0.23 1.4 1.0 A3–4V
15 6 18 45.68 15 17 12.01 18.51 0.82 1.19 10.58 13.62 – 0.94 0.64 0.79 0.27 1.5 1.2 B9–A0V
16 6 18 46.34 15 16 51.53 18.62 1.06 0.99 2.86 13.58 – 0.49 0.87 0.76 0.20 1.4 1.3 B9–A1V Hα em.e
17 6 18 44.48 15 16 16.53 18.66 1.05 1.96 14.30 15.18 – 0.39 0.64 0.75 0.25 1.5 1.0 A0–4V
18 6 18 45.99 15 16 49.14 18.70 1.19 0.76 13.22 15.18 – 0.31 0.99 0.94 0.20 1.4 1.4 A0–4V
19 6 18 44.33 15 17 00.82 19.03 1.23 1.71 11.64 9.95 – 0.35 0.84 0.66 0.22 1.3 1.2 A7–9V
20 6 18 47.19 15 17 33.87 19.10 1.21 1.78 15.78 16.36 – 1.01 0.64 0.64 0.26 1.6 1.2 A1–2V
21 6 18 46.42 15 16 43.23 19.25 1.90 0.07 12.23 10.68 – 0.78 1.08 1.00 0.35 1.4 1.8 A1–2V
22 6 18 46.39 15 16 57.66 19.34 1.10 2.02 16.68 13.61 – 1.14 0.91 0.71 0.13 1.5 1.2 A1–3V
23 6 18 46.86 15 17 49.45 19.57 1.52 2.25 6.25 8.82 – 0.50 0.96 0.56 0.12 1.4 1.2 A9–F0V
24 6 18 48.50 15 16 46.19 14.80 0.86 0.27 2.16 5.05 2.89 0.01 0.95 0.44 0.11 1.5 0.3 F6–8V fgf
25 6 18 46.05 15 17 48.30 14.85 0.75 0.01 4.09 4.45 2.83 0.10 1.11 0.46 0.13 1.2 0.4 F6–8V fgf
26 6 18 43.80 15 16 14.30 15.85 0.68 1.01 5.87 6.39 2.07 0.35 0.79 0.33 0.11 1.6 0.4 F1–3V
27 6 18 46.69 15 16 38.95 16.59 0.69 1.75 8.86 6.71 2.25 0.05 0.84 0.38 0.11 1.5 0.4 F1–3V
28 6 18 43.89 15 16 05.99 17.90 0.88 3.06 2.18 4.32 2.98 0.14 1.38 0.37 0.07 1.6 0.4 F6–8V
29 6 18 46.64 15 17 40.73 18.08 0.84 2.93 4.88 5.93 2.16 0.30 1.01 0.48 0.16 1.4 0.5 F1–3V
30 6 18 47.00 15 17 31.31 18.27 1.69 0.95 3.89 6.15 1.87 0.33 1.01 0.80 0.23 1.6 1.2 F1–3V
31 6 18 47.42 15 17 12.06 18.38 1.91 0.72 2.74 4.93 2.21 0.19 1.12 0.85 0.24 1.5 1.4 F2–5V
32 6 18 45.89 15 16 34.89 19.21 1.05 3.13 – – 2.23 0.34 1.05 0.46 0.15 1.5 0.8 F2–3V
33 6 18 42.62 15 17 10.38 19.22 1.08 3.45 2.13 4.04 2.94 – 1.59 0.52 0.10 1.3 0.7 F7–8V
34 6 18 47.57 15 16 40.20 19.26 1.39 3.49 – – 3.00 – 4.22 0.60 0.15 1.4 0.7 ~G5V
35 6 18 42.41 15 17 16.94 19.27 1.65 3.19 – – 2.99 – 6.26 0.60 0.06 1.2 0.8 ~G5V fgf
36 6 18 48.84 15 16 37.04 19.29 1.51 3.21 – – 2.93 – 4.81 0.49 0.07 0.8 0.8 ~G5V
37 6 18 46.96 15 17 23.71 19.34 0.99 4.50 – – 2.78 – 2.01 0.34 0.05 1.4 0.4 ~G5V
38 6 18 44.03 15 15 56.55 19.46 1.42 3.69 – – 2.71 – 2.79 0.34 0.07 1.6 0.7 ~G5V
39 6 18 46.43 15 16 21.13 19.59 1.18 3.82 – – 2.53 – 2.18 0.44 0.14 1.5 0.7 ~G5V

Notes. The rms error for the V band magnitude is ΔV = 0.67 mag, for Δ(V–I) = 0.38 mag.

(a)

Based on their individual extinctions listed in the second to last column of this table and assuming a distance modulus μ = 13.6 mag.

(b)

Determined via the Balmer emission lines decrement (Sect. 3.1).

(c)

Determined via the spectral energy distribution (Sect. 3.2). Most F- and G-type stars are either foreground stars or lie at the front side of the cluster, because of their lower E(B–V)SpT (consistent with DIB measurements) and bright V-band magnitudes.

(d)

Most studies assigned a spectral type ranging from late O to early B (Brand & Wouterloot 1994; Rudolph et al. 1996; Miroshnichenko 1994).

(e)

Could be due to poor subtraction of the ambient nebular spectrum.

(f)

Likely a foreground star, based on its radial velocity.

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