Table 1
Sample stars and observing data in the L-band.
| Star | Spectral | Sp. type | Instr. | Obs. | Integr. | Previous investigations | |||
| type | reference | date | time | Pv | opt | H/K | IR/radio | ||
|
|
|||||||||
| Cyg OB2 7 | O3 If∗ | MT91 | S | 10, 11 Sep. 05 | 360 s, 400 s | – | 3, 6 | 7 | 8 |
| Cyg OB2 8A | O5.5 I(f) | MT91 | S | 11 Sep. 05 | 400 s | – | 3, 6 | 7 | 8 |
| Cyg OB2 8C | O5 If | MT91 | S | 10, 11 Sep. 05 | 360 s, 400 s | – | 3, 6 | 7 | 8 |
| HD 30614 (α Cam) | O9.5 Ia | W72 | S | 11 Sep. 06 | 200 s | 1 | 4, 5 | 7 | 8 |
| HD 36861 (λ Ori A) | O8 III((f)) | W72 | I | 08 Jan. 06 | 816 s(3.7 μm ), 1224 s(3.9 μm ) | 1 | 4 | – | 8 |
| HD 37128 (ϵ Ori) | B0 Ia | WF90 | I | 08 Jan. 06 | 102 s(3.7 μm ), 204 s(3.9 μm ) | – | 2 | 7 | – |
| S | 11 Sep. 05 | 80 s | |||||||
| HD 37468 (σ Ori) | O9.5 V | CA71 | I | 08 Jan. 06 | 306 s(3.7 μm ), 612 s(3.9 μm ); | – | – | 7 | – |
| S | 11 Sep. 05 | 320 s | |||||||
| HD 66811(ζ Pup) | O4 I(n)f | W72 | I | 08 Jan. 06 | 204 s(3.7 μm ), 408 s(3.9 μm ) | 1 | 4, 5 | 7 | 8 |
| HD 76341 | O9 Ib | M98 | I | 08 Jan. 06 | 826 s(3.7 μm ), 1656 s(3.9 μm ) | – | – | – | – |
| HD 217086 | O7 Vn | W73 | S | 10, 11 Sep. 05 | 420 s, 400 s | 1 | 5, 6 | 7 | – |
Notes. “S” and “I” correspond to the IRTF/SpeX and VLT/ISAAC spectrograph, respectively, where HD 37128 and HD 37468 have been observed with both instruments.
References. Spectral references: CA71, Conti & Alschuler (1971); M98, Mason et al. (1998); MT91, Massey & Thompson (1991); W72, Walborn (1972); W73, Walborn (1973); WF90, Walborn & Fitzpatrick (1990). Previous investigations refer to (1) the analysis of the Pvλλ 1118/28 doublet by Fullerton et al. (2006); (2) Kudritzki et al. (1999,unblanketed analysis); (3) Herrero et al. (2002); (4) the Hα mass-loss analysis by Markova et al. (2004) based on stellar parameters calibrated to the results from optical NLTE analyses by Repolust et al. (2004); (5) Repolust et al. (2004); (6) Mokiem et al. (2005); (7) the H/K-band analysis by Repolust et al. (2005); and (8) the combined Hα, IR, mm and radio continuum analysis by Puls et al. (2006).
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