A comparative study of high-mass cluster forming clumps

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Table 1:

Details of the 1.2 mm surveys from which our source sample has been selected.
Author	Instrument-Telescope	# sources	Dec	HPBW ('')	$T_{\rm D}$ ?^a	M?^a
Beuther et al. (2002a)	MAMBO - IRAM-30 m	69	> $-20^{\circ}$	11	Y	Y^b
Faúndez et al. (2004)	SIMBA - SEST-15 m	146	${<}9^{\circ}$	24	Y	Y
Hill et al. (2005)	SIMBA - SEST-15 m	404	${<}24^{\circ}$	24	20 K^c	Y
Rathborne et al. (2006)	MAMBO - IRAM-30 m	190	$(-16^{\circ},+18^{\circ})$	11	15 K^c	Y

Notes. ^(a) Y: quantities provided by the authors; N: quantities not provided by the authors; ^(b) masses recomputed according to the authors' Erratum (Beuther et al. 2005) and assuming a dust opacity of 1 cm² g^-1 (Ossenkopf & Henning 1994); ^(c) dust temperature adopted by the authors to compute clump masses.

Source LaTeX | All tables | In the text

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