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Table 1:

Molecular cloud properties and the derived parameters.

Cloud 		Da $M_{\rm H2} \times 10^4$ $\overline{A_V}$ $\sigma_{\rm data}$ $\sigma_{\rm fit}$ $N_{\rm\rm YSO}$b
Star-forming clouds, physical resolution 0.1 pc  

Ophiuchus 		1191 0.6 2 4.3 0.48c 300
Taurus 1402 0.81 1.8 1.5 0.49 300
Serpens 2593 3.6 3 2.4 0.51 300
Cha I 1654 0.23 1.3 1.3 0.35 200
Cha II 1504 0.15 1.3 1.0 0.35 50
Lupus III 1551 0.11 1.3 0.9 0.35c 50
CrA cloud 1295 1.2 0.8 1.0 0.44 tens
Lupus I 1551 0.29 1.0 0.7 0.43 tens
LDN1228d 2006 0.23 1.1 0.7 0.32 tens
Pipe 1307 0.95 2.5 1.4 0.29c 15
LDN134 1008 0.13 1.2 0.6 0.39 a few
LDN204d 1191 0.43 1.9 0.8 0.41 a few
LDN1333d 1809 0.57 1.2 0.5 0.38 a few
Non-star-forming clouds, physical resolution 0.1 pc  

LDN1719d 		1204 0.53 0.6 0.7 0.50  
Musca 1504 0.07 1.0 0.7 0.45  
Cha III 1504 0.18 1.3 0.8 0.46  
Coalsack 15010 0.5 2.7 1.4 0.28  
Lupus V 1551 0.36 1.4 0.7 0.42  
Star-forming clouds, physical resolution 0.6 pc  

Ori A GMC 		45011 11 1.4 2.8 0.5 >2000
Per cloud 26012 2.0 1.7 1.7 0.49 >100
Ori B GMC 45011 9.0 1.2 1.7 0.59 >100
Cepheus A 73013 3.5 1.5 1.6 0.47 >100
California 45014 11 1.4 0.7 0.51 tens

a References: (1) Lombardi et al. (2008b); (2) Torres et al. (2007); (3) Straizys et al. (1996); (4) Knude & Hog (1998); (5) Casey et al. (1998); (6) Kun (1998); (7) Lombardi et al. (2006); (8) Mattila (1979); (9) Obayashi et al. (1998); (10) Corradi et al. (1997); (11) Burrows et al. (1993); (12) Cernis (1993); (13) Crawford et al. (1970); (14) Lada et al. (2009).
b An order-of-magnitude estimate of the pre-main-sequence star population in the clouds, based on Reipurth (2008).
c No good fit was achieved. A rough estimate is given for reference.
d The most prominent Lynds dark nebula in the region.

Source LaTeX | All tables | In the text

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