Table A.2.
ALMA 3-mm upper limits for stars that are undetected.
| Spectral type | Source | Upper limits | |
|---|---|---|---|
| Flux density (Jy) | Mass-loss rate  |
||
| O9Iab | W24 | < 1.16e−04 | < 6.04e−06 |
| W35 | < 9.16e−05 | < 5.08e−06 | |
| W38 | < 1.23e−04 | < 6.33e−06 | |
| W41 | < 1.22e−04 | < 6.28e−06 | |
| O9Ib | W15 | < 1.04e−04 | < 5.68e−06 |
| W29 | < 9.38e−05 | < 5.26e−06 | |
| W37 | < 1.61e−04 | < 7.89e−06 | |
| W43c | < 6.92e−05 | < 4.19e−06 | |
| O9.5Iab | W61b | < 6.13e−05 | < 3.75e−06 |
| W74 | < 6.23e−05 | < 3.80e−06 | |
| W2019 | < 1.65e−04 | < 7.89e−06 | |
| O9.5Ib | W46b | < 7.20e−05 | < 4.13e−06 |
| W56b | < 6.06e−05 | < 3.63e−06 | |
| W65 | < 6.11e−05 | < 3.65e−06 | |
| W84 | < 6.91e−05 | < 4.00e−06 | |
| W86 | < 1.43e−04 | < 7.10e−06 | |
| W2017 | < 6.40e−05 | < 3.78e−06 | |
| W2028 | < 1.16e−04 | < 5.92e−06 | |
| W3005 | < 1.32e−04 | < 6.50e−06 | |
| B0Ia | W31 | < 1.02e−04 | < 4.00e−06 |
| W34 | < 8.76e−05 | < 3.57e−06 | |
| W43a | < 1.91e−04 | < 5.90e−06 | |
| W43b | < 1.46e−04 | < 4.82e−06 | |
| W55 | < 7.38e−05 | < 3.14e−06 | |
| B0Iab | W49 | < 6.24e−05 | < 2.77e−06 |
| W60 | < 8.15e−05 | < 3.38e−06 | |
| W63a | < 6.66e−05 | < 2.90e−06 | |
| W232 | < 1.28e−04 | < 4.74e−06 | |
| B0Ib | W2002 | < 7.82e−05 | < 3.28e−06 |
| W2011 | < 5.22e−05 | < 2.42e−05 | |
| W3024 | < 5.75e−05 | < 2.60e−05 | |
| B0.5Ia | W10 | < 1.50e−04 | < 4.83e−06 |
| W18 | < 1.27e−04 | < 4.25e−06 | |
| W21 | < 8.33e−06 | < 3.11e−06 | |
| B0.5Iab | W6a | < 1.08e−04 | < 3.78e−06 |
| W54 | < 4.45e−05 | < 1.94e−06 | |
| 62a | < 8.32e−05 | < 3.19e−06 | |
| B0.5Ib | W62a | < 8.29e−05 | < 3.10e−06 |
| B1Ia | W19 | < 1.04e−04 | < 2.02e−06 |
| W21 | < 5.80e−05 | < 1.31e−06 | |
| W43b | < 6.76e−05 | < 1.46e−06 | |
| W78 | < 1.15e−04 | < 2.18e−06 | |
| W3019 | < 3.26e−04 | < 4.77e−06 | |
| B1Iab | W49 | < 1.26e−04 | < 3.26e−06 |
| W238 | < 4.91e−05 | < 1.15e−06 | |
| B1.5Ia | W8b | < 2.76e−04 | < 2.91e−06 |
| W52 | < 1.32e−04 | < 1.68e−06 | |
| B2Ia | W2a | < 9.82e−05 | < 1.50e−06 |
| W11 | < 2.14e−04 | < 2.69e−06 | |
| B3Ia | W70 | < 1.21e−04 | < 2.18e−06 |
| B4Ia | W57a | < 9.39e−05 | < 1.11e−06 |
Notes. Samples from each spectral type have been included. The upper limit flux density is taken to be 3σ where σ is the rms noise level measured in the primary-beam corrected image using a 2″ circular region centred on the optical position. The mass-loss rate calculation was performed as outlined in Sect. 4.2.2.
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