Table 2.
ALMA 3-mm flux densities of the known stars detected in these observations.
Source | RA | Dec | Flux density (mJy) |
α |
Sp. Type | Comments | ||
---|---|---|---|---|---|---|---|---|
J2000 | J2000 | 3 mm | 3.6 cm | Radio | 3 mm–3.6 cm | |||
WR stars and hybrids | ||||||||
WR J | 47 2.472 | 50 59.976 | 0.18 ± 0.04 | – | – | > 0.03 | WN5h | No RV data, Not obvious Binary (NoB) |
WR R | 47 6.090 | 50 22.535 | 0.35 ± 0.07 | – | – | > 0.30 | WN5o | No RV data, X-ray suggests binary |
WR O | 47 7.651 | 52 36.182 | 0.48 ± 0.06 | – | – | > 0.42 | WN6o | X-ray suggests binary |
WR U | 47 6.538 | 50 39.184 | 0.40 ± 0.05 | – | – | > 0.35 | WN6o | X-ray suggests binary |
WR Q | 46 55.528 | 51 34.608 | 0.40 ± 0.06 | – | – | > 0.35 | WN6o | No RV data, NoB |
WR A | 47 8.347 | 50 45.571 | 3.98 ± 0.21 | 0.50 ± 0.06 | 0.00 ± 0.04 | 0.85 | WN7b+OB? | 7.63d binary |
WR D | 47 6.245 | 51 26.525 | 0.76 ± 0.07 | – | – | > 0.61 | WN7o | X-ray suggests CWB |
WR B | 47 5.367 | 51 5.016 | 1.82 ± 0.12b | > − 0.35b | WN7o+OB? | 3.52d binary | ||
3.40 ± 0.17a | 4.30 ± 0.04a | +0.04 ± 0.07a | −0.10 ± 0.02a | |||||
WR G | 47 4.005 | 51 25.176 | 0.83 ± 0.07 | – | – | > 0.65 | WN7o | X-ray suggests CWB |
WR P | 47 1.584 | 51 45.425 | 0.68 ± 0.06 | – | – | > 0.57 | WN7o | No RV data, NoB |
WR I | 47 0.878 | 51 20.674 | 2.16 ± 0.12 | – | – | >1.04 | WN8o | No RV data, NoB |
WR V | 47 3.799 | 50 38.916 | 1.25 ± 0.08 | 0.40 ± 0.06 | 0.00 ± 0.50 | 0.46 ± 0.07 | WN8o | No RV data, NoB |
WR L | 47 4.195 | 51 7.356 | 3.65 ± 0.19 | 0.40 ± 0.06 | > 0.5 | 0.90 ± 0.07 | WN9h+OB? | RV binary |
WR S | 47 2.972 | 50 19.836 | 0.51 ± 0.06 | 0.30 ± 0.06 | > 0.0 | 0.22 ± 0.10 | WN10-11h/BHG | Runaway, single |
W13 | 47 6.451 | 50 26.224 | 0.37 ± 0.05 | – | – | > 0.32 | WNVL/BHG | Eclipsing binary |
WR K | 47 3.230 | 50 43.956 | 0.32 ± 0.06 | – | – | > 0.25 | WC8 | NoB |
WR E | 47 6.048 | 52 8.465 | 0.91 ± 0.07 | – | – | > 0.69 | WC9 | RV variable 10–20 km s−1 |
WR F | 47 5.203 | 52 25.116 | 1.44 ± 0.09 | 0.30 ± 0.06 | +0.66 ± 0.09 | 0.64 ± 0.09 | WC9d+OB? | 5.05d Binary |
WR C | 47 4.402 | 51 3.756 | 0.39 ± 0.05 | – | – | > 0.34 | WC9d | Dust production suggests binary |
WR H | 47 4.204 | 51 19.956 | 0.49 ± 0.06 | – | – | > 0.43 | WC9d | Dust suggests binary |
WR M | 47 3.954 | 51 37.776 | 0.55 ± 0.06 | – | – | > 0.48 | WC9d | RV shift suggests binary |
Yellow hypergiants and red supergiants | ||||||||
W16a | 47 6.607 | 50 42.334 | 0.69 ± 0.07b | – | – | > − 0.34b | A5Ia+ | |
1.46 ± 0.15a | 1.60 ± 0.30a | −0.33 ± 0.09a | −0.04 ± 0.09a | |||||
W12a | 47 2.205 | 50 59.166 | 1.00 ± 0.10b | – | – | > − 0.44b | F1Ia+ | |
1.63 ± 0.14a | 2.90 ± 0.30a | −0.06 ± 0.08a | −0.23 ± 0.06a | |||||
W4 | 47 1.422 | 50 37.385 | 1.66 ± 0.11b | 0.78 ± 0.07b | 0.49 ± 0.31b | 0.30 ± 0.05b | F3Ia+ | |
2.03 ± 0.25c | 0.80 ± 0.08c | −0.23 ± 0.07c | 0.00 ± 0.07c | |||||
W32 | 47 3.678 | 50 43.686 | 0.38 ± 0.07 | 0.40 ± 0.06 | 0.00 ± 0.05 | −0.03 ± 0.10 | F5Ia+ | |
W237 | 47 3.101 | 52 19.086 | – | 1.80 ± 0.20b | −0.06 ± 0.10b | – | M3Ia | |
1.60 ± 0.14a | 7.40 ± 2.21a | −0.35 ± 0.19a | −0.05 ± 0.14a | |||||
W75 | 47 8.914 | 49 58.589 | 0.45 ± 0.07 | 0.30 ± 0.06 | > 0.0 | 0.16 ± 0.11 | M4Ia | |
W20 | 47 4.686 | 51 24.096 | 1.45 ± 0.11b | – | – | > 0.00b | M5Ia | |
3.66 ± 0.19a | 3.80 ± 0.40a | −0.11 ± 0.07a | −0.02 ± 0.05a | |||||
W26 | 47 5.375 | 50 36.486 | 114.75 ± 5.76 | 20.10 ± 2.00 | 0.07 ± 0.11 | 0.71 ± 0.05 | M5-6Ia | |
Blue hypergiants, LBVs, OB supergiants and the sgB[e] star | ||||||||
W25 | 47 5.831 | 50 33.785 | 0.18 ± 0.01 | – | – | > 0.01 | O9Iab | Faint X-ray, no RV data |
W17 | 47 6.167 | 50 49.355 | 0.75 ± 0.04 | 1.70 ± 0.20 | −0.42 ± 0.11 | −0.33 ± 0.06 | 09.5Ia | Faint X-ray, no RV data |
W43a | 47 3.549 | 50 57.816 | 0.17 ± 0.05 | – | – | > 0.01 | B0Ia | 16.27d binary from RV shifts |
W61a | 47 2.300 | 51 41.826 | 0.10 ± 0.05 | – | – | > − 0.22 | B0.5Ia | No RV data, NoB, 4.5σ |
W46a | 47 3.911 | 51 19.866 | 0.35 ± 0.06 | – | – | > 0.30 | B1Ia | No RV data, NoB |
W56a | 46 58.939 | 51 49.110 | 0.11 ± 0.05 | – | – | > − 0.18 | B1.5Ia | No RV data, NoB |
W52 | 47 1.843 | 51 29.495 | 0.11 ± 0.05 | – | – | > − 0.16 | B1.5Ia | 6.7d ellipsoidal modulation |
W8b | 47 4.953 | 50 26.856 | 0.15 ± 0.05 | – | – | > − 0.06 | B1.5Ia | No RV data, NoB |
W243 | 47 7.496 | 52 29.252 | 9.96 ± 0.50 | 1.50 ± 0.20 | 0.87 ± 0.30 | 0.77 ± 0.13 | B2Ia (LBV) | RV pulsator, NoB |
W28 | 47 4.660 | 50 38.646 | 0.20 ± 0.05 | – | – | > 0.07 | B2Ia | No RV data, NoB |
W2a | 46 59.707 | 50 51.332 | 0.12 ± 0.05 | – | – | > − 0.16 | B2Ia | RV pulsator, NoB, 4.5σ |
W11 | 47 2.231 | 50 47.286 | 0.11 ± 0.05 | – | – | > − 0.19 | B2Ia | No RV data or X-ray detection, 4.5σ |
W23a | 47 2.567 | 51 9.066 | 0.23 ± 0.05 | – | – | > 0.12 | B2Ia+OB | RV data, NoB |
W71 | 47 8.450 | 50 49.530 | 0.27 ± 0.07 | – | – | > 0.19 | B2.5Ia | RV pulsator, NoB |
W33 | 47 4.117 | 50 48.636 | 0.23 ± 0.05 | – | – | > 0.13 | B5Ia+ | No RV data, NoB |
W7 | 47 3.618 | 50 14.526 | 0.37 ± 0.05 | – | – | > 0.31 | B5Ia+ | RV pulsator, NoB |
W42a | 47 3.239 | 50 52.326 | 0.25 ± 0.06 | – | – | > 0.16 | B9Ia+ | No RV data, NoB |
W9 | 47 4.140 | 50 31.430 | 152.92 ± 0.08b | 24.90 ± 2.50b | 0.68 ± 0.70b | 0.74 ± 0.04b | SgB[e] | X-ray suggests CWB |
16.15 ± 0.90c | 30.50 ± 3.00c | 0.16 ± 0.17c | −0.26 ± 0.05c | |||||
D09-R1 | 47 9.071 | 51 10.139 | 1.05 ± 0.12 | 0.70 ± 0.07b | −0.23 ± 0.27b | 0.17 ± 0.09a | BSG | |
6.5 ± 1.2c | −0.61 ± 0.11c | |||||||
D09-R2 | 47 6.908 | 50 37.204 | 0.68 ± 0.08 | 0.70 ± 0.06 | −0.43 ± 0.11 | −0.01 ± 0.06 | BSG | |
W30 | 47 4.117 | 50 39.456 | 0.17 ± 0.06 | – | – | > 0.00 | O+O | X-ray suggests CWB |
Notes. 3.6 cm flux densities and spectral indices taken from Do10 are also listed. Radio to mm spectral indices have been calculated using the total flux density unless both core and resolved components are separated in both the radio and ALMA images. Where no flux density is reported for a source in D010, we find a limiting spectral index based on a 3.6 cm flux density limit of 170 μ Jy beam−1 (see Do10 for details). Spectral type identifications have been taken from Crowther et al. (2006a) for WR stars, Clark et al. (2010) for the YHGs and RSGs, Negueruela et al. (2010) for the OB stars and Do10 for the two D09 sources,
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