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Table 3

Brightness of CO clouds and associated stellar clusters.

ID  ⟨ I1 − 0 ⟩   ⟨ I2−1 ⟩  log log log M ∗ log A V
K km s-1 K km s-1 cm-2 erg s-1 erg s-1 M⊙ erg s-1 mag Notes
s1 0.300  ±  0.028 0.658  ±  0.037 2.19  < 20.4 36.11 38.13a ... ... ... Visible only at 8–24–70 μm
s2  < 0.150  < 0.200 ...  < 20.4  < 33.97 37.88a ... ... ... Visible only at 8–24 μm
s3 0.265  ±  0.025 0.306  ±  0.228 1.15  < 20.4 35.99 38.17a ... ... ... Visible only at 8–24 μm
s4  < 0.100  < 0.150 ... ... 34.56 (39.00)a (490) (37.1) 4.2 Visible only at 8–24–70 μm
s5 0.655  ±  0.038 0.718  ±  0.107 1.10 ... 35.88 38.64 258 36.4 0.4 Weak Hα, non isol.
s6 0.290  ±  0.022 0.571  ±  0.097 1.97  < 20.4 37.11 39.15 582 37.2 1.0
s7 1.060  ±  0.069 1.363  ±  0.035 1.29 21.02 36.74 38.98 431 37.0 0.9
s8 0.565  ±  0.115 0.947  ±  0.047 1.68 21.18 37.13 39.00 490 37.1 1.4
s9 1.229  ±  0.033 1.861  ±  0.085 1.51  < 20.4 37.32 39.30 794 37.4 0.3
s10 0.642  ±  0.023 1.765  ±  0.034 2.75 20.90 37.07 39.04 504 37.1 1.2
s11 1.087  ±  0.038 0.659  ±  0.064 0.61 ... 36.73 38.86 370 36.9 1.2
s12 1.282  ±  0.051 1.681  ±  0.283 1.31 20.65 36.83 39.30 794 37.4 2.3 No FUV, tail
s13 0.888  ±  0.112 1.000  ±  0.039 1.13 21.23 36.58 38.47 215 36.0 2.7 No FUV
s14 1.422  ±  0.135 1.263  ±  0.102 0.89 20.78 37.69 39.49 948 37.6 4.1 No FUV
s15 0.372  ±  0.020 0.352  ±  0.016 0.95  < 20.4 36.99 39.11 566 37.2 3.0 No FUV, weak Hα
s15 0.159  ±  0.020 0.315  ±  0.028 1.98  < 20.4 36.99 39.11 566 37.2 3.0 No FUV, weak Hα
s16  < 0.100  < 0.150 ...  < 20.4 36.41 38.98 431 37.0 2.3 Weak Hα
s17 1.159  ±  0.082 0.852  ±  0.058 0.74 21.13 36.29 38.72 313 36.5 2.5 Visible only at 8-24-70 μm
s18 1.012  ±  0.052 1.269  ±  0.036 1.25 20.60 36.93 39.03 500 37.1 1.0
s19 0.651  ±  0.067 0.637  ±  0.065 0.98 ... 36.48 38.38 206 35.8 0.9 IR weak
s20 0.353  ±  0.050 0.172  ±  0.044 0.49 ... 36.48 38.54 241 36.3 0.04 IR weak

Notes. In Cols. 2 and 3 we give the value of the CO J = 1–0 and 2–1 line intensity averaged between that derived from Gaussian fits and that obtained by summing the flux in each channel. The ratio between the two CO line intensities is shown in Col. 4. In Col. 5 we give the H2 column densities derived from FCRAO observations and in Cols. 6 and 7 the Hα luminosity (corrected for extinction) and the bolometric luminosity of the sources. In the last three Cols. we show the estimated mass, expected Hα luminosity (see text for details), and visual extinction of the stellar clusters.

(a)

Luminosity as from Eq. (3), because the source is an AGB star.

(b)

Source of unknown nature, luminosity computed according to Eq. (1).

(c)

HII region next to an AGB star, luminosity computed according to Eq. (1).

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