| Source | RA (1950) | Dec (1950) | L | d | N(H2) |
| (h m s) | (
 ) |
(104  ) |
(kpc) | (1023 cm-2) | |
| W3 IRS5 | 02 21 53.1 | +61 52 20 | 17 | 2.2 | 2.3 |
| MonR2 IRS3 | 06 05 21.5 | -06 22 26 | 1.3 | 0.95 | 1.8 |
| NGC 6334 IRS1 | 17 17 32.0 | -35 44 05 | 11 | 1.7 | 11.3 |
| W33A | 18 11 43.7 | -17 53 02 | 10 | 4 | 6.2 |
| AFGL 2136 | 18 19 36.6 | -13 31 40 | 7 | 2 | 1.2 |
| AFGL 2591 | 20 27 35.8 | +40 01 14 | 2 | 1 | 2.3 |
| S140 IRS1 | 22 17 41.1 | +63 03 42 | 2 | 0.9 | 1.4 |
| NGC 7538 IRS1 | 23 11 36.7 | +61 11 51 | 13 | 2.8 | 6.5 |
| NGC 7538 IRS9 | 23 11 52.8 | +61 10 59 | 4 | 2.8 | 3.3 |
| a Luminosity and distance from Henning et al. (1992) and Giannakopoulou et al. (1997) (MonR2 IRS3) and from van der Tak et al. (2000b) (other sources); H2 column density from this work (MonR2 IRS3) and from van der Tak et al. (2000b) (other sources). Column densities are 15'' averages and strongly beam dependent. |