Table 1
Extinction properties measured in the sightlines towards M17.
| Identifier | Sp.type | B | V | Ka | RV | RV | AV | AV | E(B–V) | E(B–V) | AK |
|---|---|---|---|---|---|---|---|---|---|---|---|
| mag | mag | mag | SED | Fitzp. | SED (mag) | V − V0 | SED |  |
mag | ||
| B111 | O4.5 V | 12.24b | 11.21b | 7.475 |  |
3.86 |  |
5.17 | 1.47 ± 0.13 | 1.35 | 0.50 |
| B164 | O6 Vz | 16.85c | 15.41c | 8.758 |  |
4.87 |  |
9.03 | 2.2 ± 0.10 | 1.76 | 1.44 |
| B215 | B0-B1 V | − | 16.10d | 10.00 |  |
− |  |
8.17 | 1.85 ± 0.06 | − | 1.15 |
| B243 | B8 V | 19.10c | 17.80c | 9.544 |  |
4.64 |  |
6.52 | 1.82 ± 0.22 | 1.41 | 0.72 |
| B253 | B3-B5 III | 17.11c | 15.74c | 10.31 |  |
4.29 |  |
6.22 | 1.59 ± 0.06 | 1.52 | 0.41 |
| B268 | B9-A0 | 18.40c | 17.10c | 9.494 |  |
3.47 |  |
4.71 | 1.75 ± 0.25 | 1.34 | 0.52 |
| B275 | B7 III | 17.02c | 15.55c | 7.947 |  |
3.35 |  |
5.44 | 1.77 ± 0.26 | 1.59 | 0.61 |
| B289 | O9.7 V | 16.97c | 15.55c | 9.178 |  |
4.80 |  |
8.13 | 2.23 ± 0.17 | 1.73 | 0.78 |
| B311 | O8.5 Vz | 14.99c | 13.69c | 8.884 |  |
4.00 |  |
6.51 | 1.85 ± 0.11 | 1.62 | 0.71 |
| B331 | late-B | − | 20.10c | 8.946 |  |
− |  |
− | 2.89 ± 0.13 | − | − |
| B337 | late-B | − | − | 9.343 |  |
− |  |
− | 3.66 ± 0.25 | − | − |
Notes. Column 1 lists the star’s identifier, Col. 2 the spectral type as reported in Paper I. Columns 3–5 show the B, V, and K-band magnitudes,respectively. Columns 6, 8, and 10 list the extinction parameters (RV, AV, and E(B–V) = AV∕RV) derived by fitting the spectral energy distribution to Kurucz models. We list the RV and AK values derived using Eq. (1) (see Sect. 3 for more information on objects with circumstellar disks) in Cols. 7 and 12. Column 9 lists the V -band excess AV, and Col. 11 shows the colour excess (B − V)-(B − V)0, where the intrinsic colour (B − V)0 is taken from Pecaut & Mamajek (2013) and Wegner (2000, 2014). (a) 2MASS catalogue (Cutri et al. 2003).(b)AAVSO Photometric all sky survey (APASS) catalog: https://www.aavso.org/apass (c) Chini et al. (1980). (d) Hoffmeister et al. (2008).
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