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Home All issues Volume 503 / No 3 (September I 2009) A&A, 503 3 (2009) 801-816 Full HTML
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Table 2:

Results for cluster detection.

Sou.		 da $I_{\rm c}$ $N_{\rm obs}$ $R_{\rm clu}$ Pre-MS $M_{\rm gas}$ $L_{\rm bol}$ AV $_{\rm peak}$ Cluster Center
Mol kpc     pc % % $M_\odot$ 103$L_{\odot}$ mag $\alpha$(J2000) $\delta$(J2000)
          CC CM          
3 2.17 78 78 1.7 34 99 910 12.4 18 00:44:57.4 +55:47:20.0
8A 11.5 25 30 1.3 37 27 1650 57.0 18 05:17:13.8 +39:22:29.7
8B 11.5 27 24 1.3 9 4 1780 5.5 8 05:17:12.0 +39:21:51.8
9 6.2 7 7 0.6 16 -g - 24 - 05:20:16.9 +36:37:22.0
11 2.1 51 48 0.5 12 41 360 4.6 35 05:37:47.7 +31:59:24.0
12 1.6 12 13 0.3 0 30 72 1.6 46 05:40:24.4 +23:51:54.8
15 1.5 64 61 0.3 34 -g - 5.8 - 06:08:41.0 +21:31:00.0
28 4.5 75 75 1.0 58 95 220 9.1 4 07:00:51.5 -08:56:18.2
30 0.3 200e no cluster detectedb - 0.14 - - -
38 0.5 -5 no cluster detectedc -h 0.19 40 - -
45 4.3 28 27 0.5 68 19 1340 21.2 77 18:17:24.1 -17:22:12.3
50 4.9 46 43 0.6 36 41 80 17.3 25 18:19:07.6 -16:11:21.0
59 5.7 0 no cluster detectedc -h 11 29 - -
75 3.9 8 7 0.7 37 24 1310 13.3 38 18:53:38.1 +01:50:26.5
82 6.8 8 10 0.3 0 52 590 15.4 52 18:59:03.2 +03:53:16.7
84 2.2 21 21 0.3 0 54 28 4.3 15 18:59:14.3 +07:04:52.3
98 4.5 6 no cluster detectedf -h 9.2 68 - -
99 6.1 45 38 0.9 49 -g - 37.3 - 19:11:51.4 +09:49:35.4
103 4.1 105 107 0.7 46 87 510 28.2 42 19:23:36.2 +17:28:58.1
109 4.3 19 17 0.5 d d 1030 26.7 90 19:39:33.0 +24:00:21.3
110 4.3 23 20 0.5 d d 400 14.8 55 19:40:58.5 +24:04:36.3
136 3.6 21 19 0.6 18 52 230 4 21 21:32:31.4 +51:02:23.1
139 7.3 25 24 1.2 10 31 1870 1.35 20 21:53:39.2 +56:27:50.7
143 5.0 25 22 0.8 10 76 630 7.8 26 22:19:09.0 +56:04:58.7
148 5.1 43 41 0.9 43 64 22 7.8 13 22:32:23.4 +58:19:01.3
151 5.4 15 14 0.9 12 30 2020 25 40 22:52:38.3 +60:00:44.6
160 5.0 36 34 1.3 30 76 1830 16 32 23:40:53.1 +61:10:21.0
a Kinetic distance using the rotation curve from Brand & Blitz (1993).
b Stellar density analysis inconclusive due to extreme crowdedness of this field.
c Stellar density reveales no peaks close to the IRAS position or the submm peak.
d Only observed in $K_{\rm s}$.
e Detection refused due to extreme field complexity (see text).
f Detection refused because only 1 annulus in the radial density profile is above background (see text).
g No extinction estimate is available due to lack of submm information to evaluate de-reddening correction.
h Extinction estimate is available from single-pointing submillimeter data (Molinari et al. 2000) but not from maps, so that a reliable clump mass estimate is not possible.

Source LaTeX | All tables | In the text

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