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Table 1

The stellar parameters of our sample of Herbig Be stars.

# Name Other Right Declination Spec. Ref. log Teff Distance Ref. AV log L∗ Radius Mass Group
Ascension Type [K] [kpc] [L⊙] [R⊙] [M⊙]
1 PDS 204 MWC 778 05 50 13.5  + 23 52 17 B1?e V03 4.41   ±   0.14 1.0   ±   0.3 H08 4.5  ±  0.4 3.67  ±  0.15 3.5  ±  0.7 10  ±  2 U
2 MWC 789 HD 250550 06 01 59.99  + 16 30 56.7 B9e H04 4.04  ±  0.03 0.7 F84 0.4  ±  0.1 2.14  ±  0.25 3.3  ±  0.5 3.1  ±  0.6 II
3 LkHα 208 HBC 193 06 07 49.46  + 18 39 26.3 A7e H04 3.91  ±  0.03 1.0 H92 0.9  ±  0.1 1.61  ±  0.11 3.2  ±  0.5 2.4  ±  0.4 U
4 LkHα 339 HBC 197 06 10 57.8  −06 14 37 A1e H04 3.97  ±  0.05 0.83  ±  0.05 H76 2.4  ±  0.1 1.36  ±  0.03 1.8  ±  0.1 2.1  ±  0.4 U
5 MWC 137 PK 195-00.1 06 18 45.50  + 15 16 52.4 B0e H92 4.49  ±  0.05 1.3 H92 4.5  ±  0.1 4.42  ±  0.11 5.7  ±  0.8 16  ±  1 II
6 LkHα 215 V699 Mon 06 32 41.80  + 10 09 33.6 B6e H04 4.14  ±  0.08 0.8 H82 2.0  ±  0.1 2.79  ±  0.10 4.3  ±  0.6 4.7  ±  0.9 G
7 MWC 147 HD 259431 06 33 05.19  + 10 19 20.0 B1Ve V98 4.41  ±  0.05 0.8 H82 1.6  ±  0.1 3.94  ±  0.11 4.8  ±  0.7 6.6  ±  1.3 U
8 R Mon BD+08 1427 06 39 09.95  + 08 44 10.7 B8IIIev M01 4.07  ±  0.05 0.8 J82 2.5  ±  0.1 2.12  ±  0.12 2.8  ±  0.4 3.4  ±  0.8 II
9 PDS 241# Ced 92 07 08 38.8  −04 19 08 B0e V03 4.48  ±  0.05 7.2 W89 2.9  ±  0.1 5.18  ±  0.11 14  ±  2 32  ±  6 G
10 PDS 27 DW CMa 07 19 35.94  −17 39 18.7 B2?e V03 4.34  ±  0.14 1.25 V03 4.8  ±  0.1 3.80  ±  0.11 5.5  ±  0.8 9.1  ±  1.8 II
11 Hilt 641 HD 64315 07 52 20.28  −26 25 46.7 O6Vne W82 4.60  ±  0.03 6.4 G06 – – – – –
12 Hen 3-331 HD 85567 09 50 28.54  −60 58 03.0 B2ne Mi01 4.32  ±  0.08 1.5  ±  0.5 Mi01 1.1  ±  0.1 4.17  ±  0.16 9  ±  2 12  ±  2 II
13 Hen 3-847 CPD-48 5215 13 01 17.80  −48 53 18.8 B5e V03 4.18  ±  0.03 1.66  ±  0.23 V11 0.8  ±  0.1 3.22  ±  0.08 5.9  ±  0.6 6.2  ±  1.2 II
14 Hen 3-1110 HD 141926 15 54 21.83  −55 19 44.8 B2IIIne V03 4.31  ±  0.05 0.65 V03 2.4  ±  0.1 3.88  ±  0.11 7.0  ±  1.0 14  ±  2 G
15 MCW 1264# HD 152291 16 54 24.16  −40 39 09.5 B2II:e T94 4.26 – – – – – – –
16 V921 Sco CD-42 11721 16 59 06.78  −42 42 08.4 B0?pe S90 4.45  ±  0.04 1.15  ±  0.15 B07 5.0  ±  0.1 4.83  ±  0.07 11  ±  1 21  ±  4 II
17 MWC 878 CPD-38 6814 17 24 44.69  −38 43 51.5 O9/B0e Mi01 4.48  ±  0.05 3.3  ±  0.4 Mi01 2.4  ±  0.1 4.77  ±  0.07 8.9  ±  0.8 20  ±  4 II
18 Hen 3-1418# HD 319896 17 31 05.85  −35 08 29.3 B4e V03 4.23  ±  0.04 1.4  ±  0.3 V03 – – – – –
19 Hen 3-1444⋄ HD 320156 17 37 58.50  −35 23 04.3 B0e N95 4.48 – – – – – – –
20 PDS 152# HD 316051 17 39 52.18  −27 23 44.1 B5e N95 4.18 - – – – – – –
21 MWC 593# CPD-24 5962 17 49 10.17  −24 14 21.3 B0Ia:e V93 4.41 - – – – – – –
22 PDS 477 – 18 00 30.10  −16 47 22.7 B1e V03 4.48  ±  0.06 6.7  ±  0.7 V11 4.4  ±  0.1 4.73  ±  0.08 8.5  ±  0.8 19  ±  4 II
23 AS 267 Hen 3-1559 18 01 56.65  −23 41 31.2 B5IV:ne T94 4.21 - – – – – – –
24 NGC 6530-45 V5098 Sgr 18 02 50.21  −24 16 19.2 B5e V97 4.18 1.8  ±  0.1 S90 – – – – –
25 LkHα 112 NGC 6530-180 18 04 22.74  −24 22 09.8 B2Ve V97 4.32 1.8  ±  0.1 S90 – – – – –
26 LkHα 115# NGC 6530-245 18 04 50.63  −24 25 41.9 B2Ve A07 4.32 1.8  ±  0.1 S90 – – – – –
27 LkHα 260 NGC 6611-494 18 19 09.39  −13 50 41.1 B6e DW97 4.15  ±  0.04 2.14  ±  0.1 B99 3.2  ±  0.1 2.65  ±  0.03 3.5  ±  0.1 4.4  ±  0.8 U
28 MWC 297 NZ Ser 18 27 39.60  −03 49 52.0 B1.5Ve D97 4.36  ±  0.03 0.25  ±  0.03 D97 7.7  ±  0.1 3.92  ±  0.06 5.8  ±  0.4 10.1  ±  2 II
29 AS 310 PK 026+01.1 18 33 21.17  −04 58 06.7 B1e H04 4.40  ±  0.07 2.5 B93 3.7  ±  0.1 4.23  ±  0.10 6.8  ±  1.0 12  ±  2 U
30 PDS 543 – 18 48 00.66  + 02 54 17.1 B1e V03 4.48  ±  0.06 2.8  ±  0.3 V11 4.4  ±  0.1 4.73  ±  0.08 8.5  ±  0.8 19  ±  4 U

Notes. Of a total of 30 targets, 19 were covered spectroscopically, 4 were not detected in the VISIR imaging mode (†), 6 were too faint for spectroscopic follow-up and 1 target was not spectroscopically covered due to a lack of observation time (⋄). The astrometry was taken from Simbad. The spectral types and distances were taken from the literature, with the references indicated in Cols. 7 and 10. The optical extinction, luminosity and radius followed from our analysis of the optical photometry. The masses were determined by comparing Teff and L∗ with PMS evolution tracks of Siess et al. (2000) and ZAMS positions of Meynet et al. (1994). The group classification is based on the IR SED, as explained in Sect. 7.1. Note that LkHα 208 and LkHα 339 are A stars. They entered the sample because of a previous misclassification and we kept them in the sample to facilitate the comparison of HBe with HAe stars.

References. (A07) Arias et al. 2007; (B99) Belikov et al. (1999); (B07) Borges Fernandes et al. (2007); (B93) Brooke et al. (1993); (DW97) de Winter et al. (1997); (D97) Drew et al. (1997); (F84) Finkenzeller & Mundt (1984); (G06) Gamen et al. (2006); (H08) Herbig & Vacca (2008); (H82) Herbst et al. (1982); (H76) Herbst & Racine (1976); (H04) Hernández et al. (2004); (H92) Hillenbrand et al. (1992); (J82) Jones & Herbig (1982); (Mi01) Miroshnichenko et al. (2001); (M01) Mora et al. (2001); (N95) Nesterov et al. (1995); (S90) Shore et al. (1990); (T94) Thé et al. (1994); (V97) van den Ancker et al. (1997); (V98) van den Ancker et al. (1998); (V03) Vieira et al. (2003); (V11) this paper; (V93) Vijapurkar & Drilling (1993); (W82) Walborn (1982); (W89) Wouterloot & Brand (1989).

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