Dense molecular cocoons in the massive protocluster W3 IRS5: a test case for models of massive star formation

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Volume 558 (October 2013)

A&A, 558 (2013) A69

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Table 1

Characteristics of the continuum emission in W3 IRS5 at 353.6 GHz.

Source	α(2000)	δ(2000)	I_ν^a	S_ν^b	N(H₂)^c	M(H₂)^d	n(H₂)^e	Associated cm-wave,
	(hh mm ss)	(dd mm ss)	(Jy beam^-1)	(Jy)	(×10²³ cm^-2)	(M_⊙)	(×10⁷ cm^-3)	IR, or mm source

SMM1	02 25 40.779	+62 05 52.55	0.41	0.43	4.4	0.6	3.2	D2^f, Q5^g, K7^g, MIR1^g, NIR1^h,
								MM-1ⁱ, SMS1-MM1^j
SMM2	02 25 40.679	+62 05 51.89	0.30	0.39	3.2	0.5	2.9	B^f, Q1-3^g, K2-4^g, MIR2^g, NIR2^h,
								MM-2/3ⁱ, MM-5ⁱ
SMM3	02 25 40.509	+62 05 50.41	0.16	0.24	1.7	0.3	1.8	SMS1-MM2^j
SMM4	02 25 40.431	+62 05 51.36	0.14	0.22	1.5	0.3	1.6	SMS1-MM2^j
SMM5	02 25 40.504	+62 05 52.99	0.09	0.13	1.0	0.2	1.0

Notes.

^(a)

Peak intensity measured from the image.

^(b)

Point source flux density measured from the visibility fit.

^(c)

H₂ column density. We assume T_d = 150 K for all submillimeter sources.

^(d)

H₂ mass. We assume T_d = 150 K for all submillimeter sources.

^(e)

H₂ volume density. We assume T_d = 150 K for all submillimeter sources. A spherical source with a diameter of 1″ or 1830 AU is assumed.

^(f)

Claussen et al. (1994) and Wilson et al. (2003).

^(g)

van der Tak et al. (2005).

^(h)

Megeath et al. (2005).

⁽ⁱ⁾

Rodón et al. (2008).

^(j)

Wang et al. (2012).

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