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Table B.2

Photometric properties of all the W-R stars in 30 Dor.

ID Star Spectral Ref. m v b − v Ref. Wλ(4686) Wλ(5808) Ref. (b − v)0 R v a A v ΔMv
# BAT99 VFTS Alias Type [mag] [mag] [Å] [Å] [mag] [mag] [mag] [mag] [mag]

24 86 019 Br 69 WN 3(h) (1)b 16.68 0.11 (11) 110 (1) −0.27 4.6 1.7 −3.6
92 88 079 Br 70a WN 4b/WCE (2) 17.75 0.46 (12) 225 1660 (1,12) −0.23 4.6 3.2 −3.9
117 89 108 Br 71 WN 7h (3) 14.13 0.22 (3) 96 (1) −0.28 4.6 2.3 −6.7
144 90 136 Br 74 WC 4 (4) 15.42 0.12 (12) 1451 (12) −0.16 4.6 1.3 −4.4
155 91 147 Br 73-1A WN 6(h) (1) 14.98 0.15 (13) 39 (1) −0.30 4.6 2.1 −5.6
185 92 Br 72, R130 WCE/WN+B1 I (5) 11.47 0.03 (11) 14 73 (14,18) −0.31 4.6 1.6 −8.6 + 3.2c −5.4
375 95 402 Br 80, R135 WN 7h+OB (1) 13.04 0.09 (3,14) 80 (1) −0.28 4.6 1.7 −7.2 −3.5 −7.2
402 96 427 Br 81 WN 8(h) (3) 13.82 0.49 (3) 40 (1) −0.30 4.6 3.6 −8.3
443 98 Br 79, Mk 49 WN 6(h) (6) 13.37 0.10 (3) 19 (18) −0.31 4.6 1.9 −7.0
493 100 1001 Br75, R134 WN 7h (3) 12.40 0.14 (3) 27 (18) −0.31 5.4 2.4 −8.5
543 101 507 Br 87, R140a1 WC 4(+WN 6+O) (7) { 12.50 0.03 (16,17) 170d (1) –0.32 4.6 1.6 −7.6 +2.0 −5.5
544 102 507 Br 87, R140a2 WN 6+(O) (8) 12.50 0.03 (16,17) 53 (1) −0.31 4.6 1.6 −7.6 −1.0 −7.2
545 103 509 Br 87, R140b WN 5(h)+O(+early O) (1) 12.80 0.03 (16,17) 42 (1) −0.30 4.6 1.5 −7.2 −0.3 −6.6
613 106 Br 82, R136a3 WN 5h (6) 13.02 0.05 (15) 55 (15) −0.29 5.4 1.8 −7.3
630 108 Br 82, R136a1 WN 5h (6) 12.23 0.03 (15) 37 (15) −0.30 5.4 1.8 −8.1
633 109 Br 82, R136a2 WN 5h (6) 12.77 0.06 (15) 41 (15) −0.30 5.4 2.0 −7.7
706 112 1025 Br 82, R136c WN 5h (6) 13.39 0.20 (9,17) 54 (15) −0.30 5.4 2.7 −7.8
762 115 Br 83, Mk33Sb WC 5 (9) 15.23 0.12 (9) 1100d (9) –0.28 5.4 2.2 −5.4
770 116 Br 84, Mk34 WN 5h (6) 13.10 0.14 (9,17) 30 (18) −0.33 5.4 2.6 −7.9
862 117 617 Br 88, R146 WN 5ha (2) 12.95 −0.16 (12) 37 (1) −0.30 4.6 0.6 −6.2
916 118 Br 89 WN 6he (10) 11.20 −0.17 (11) 60 (18) −0.29 4.6 0.6 −7.8
928 118a 682 WN 5h (1) 16.30 0.60 (1,16) 39 (1) −0.30 4.6 4.1 −6.3f
938 119 695 Br 90, R145 WN 6h+? (1) 12.06 0.03 (11) 39 (1) −0.30 4.6 1.5 −7.9 −0.1 −7.2
973 121 731 Br 90a WC 4 (4) 17.21 0.31 (12) 1258 (12) −0.28 4.6 2.8 −4.1
1001 122 758 Br 92, R147 WN 5h (1) 12.75 0.03 (12) 76 (1) −0.29 4.6 1.5 −7.2

Notes. Values in italic indicate where magnitudes or colours have been assumed. The Wλ of the He ii λ4686 line for WN stars or C iv λ5808 line for WC stars, is listed with references. For multiple systems, a magnitude correction is given, where . Note that the template W-R stars will have had different Av and values derived from their CMFGEN models, as listed in Table B.1, and that the properties given in that table are adopted for the star. Similarly, for comparison, this table gives photometry for stars BAT99-90, 106, 108, 109, 112 but their stellar properties were equivalently adopted from Crowther et al. (2002) or Crowther et al. (2010) and were not derived from the values in this table. See text for more details. The photometric data given for stars BAT99-101 and 102 are for the combined R140a system.

(a)

Narrow band Rv derived from average broadband RV determined for each region (see Appendix C).

(b)

SpT is amended from WN 3o to WN 3(h) following further inspection of the Pickering series.

(c)

Based on Wλ dilution of C iv λ5808 line.

(d)

Wλ of C iv λ4650 line (undiluted Wλ(4650) ≈ 1200) based on BAT99-90.

(e)

Revealed as a WN 5-6+WN 6-7 binary system by Sana et al. (2013b).

(f)

was estimated using broad band photometry and v − V ≈ 0.2 mag relation from Breysacher (1986). However, high reddening allows for a large uncertainty and the star is thought to be more comparable to BAT99-106 (F. Najarro).

Reference. (1) Paper I; (2) Foellmi et al. (2003); (3) Crowther & Smith (1997); (4) Smith et al. (1990); (5) Conti & Massey (1989); (6) Crowther & Dessart (1998); (7) Bartzakos et al. (2001); (8) Moffat et al. (1987); (9) Massey & Hunter (1998); (10) Smith et al. (1996); (11) Schmutz & Vacca (1991); (12) Crowther & Hadfield (2006); (13) Walborn et al. (1999); (14) Torres-Dodgen & Massey (1988); (15) de Koter et al. (1997), (16) Breysacher (1986); (17) De Marchi et al. (2011); (18) Schnurr et al. (2008).

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