Protostellar accretion traced with chemistry - High-resolution C18O and continuum observations towards deeply embedded protostars in Perseus

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Volume 602 (June 2017)

A&A, 602 (2017) A120

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Table 4

Continuum fluxes and inferred masses.

Source	F _{1.3 mm}		M _compact		S _{850 μm}		M _env		Disk candidate^a	Ref.^a




	(mJy)		(M_⊙)		(Jy beam^-1)		(M_⊙)
	u	c	u	c	u	c	u	c

Per-emb 1	115	76	0.08	0.05	2.18	1.96	1.94	1.70	Y	1,2,6
Per-emb 2	415	387	0.30	0.28	2.50	1.38	2.93	1.43	Y	1,4,5
Per-emb 5	207	192	0.15	0.14	1.30	0.74	1.17	0.60	Y	1,5
Per-emb 11	203	179	0.15	0.13	1.72	1.20	1.55	1.01	Y	1,2
Per-emb 12	1690	1551	1.23	1.12	11.45	6.96	8.69	4.78	Y	7
Per-emb 13	725	654	0.53	0.47	5.46	3.57	4.37	2.62
Per-emb 14	79	59	0.06	0.04	1.18	1.01	1.30	1.08	Y	1,2,4
Per-emb 16	12	–4	0.01	–0.00	0.78	0.79	0.97	0.99
Per-emb 18	117	85	0.08	0.06	1.85	1.60	1.24	1.04	Y	1,5
Per-emb 19	10	1	0.01	0.00	0.46	0.46	0.53	0.53
Per-emb 21	44	8	0.03	0.01	1.85	1.83	1.24	1.22
Per-emb 22	75	50	0.05	0.04	1.41	1.27	0.89	0.78	Y	4
Per-emb 25	83	80	0.06	0.06	0.38	0.15	0.30	0.10
Per-emb 26	169	132	0.12	0.10	2.23	1.85	1.11	0.88
Per-emb 27	245	185	0.18	0.13	3.53	2.99	1.48	1.21	Y	1,3
Per-emb 28	8	–7	0.01	–0.00	0.71	0.73	0.71	0.73
Per-emb 29	132	85	0.10	0.06	2.60	2.35	1.84	1.64
Per-emb 33	513	429	0.37	0.31	5.46	4.22	3.36	2.47	Y	1,4
Per-emb 35	36	19	0.03	0.01	0.86	0.80	0.35	0.33	Y	1
Per-emb 42	...	...	...	...	2.23	...	1.11	...
Per-emb 44	305	220	0.22	0.16	4.87	4.23	1.79	1.51	Y	1
Per-emb 47	10	...	0.01	...	...	...	...	...
Per-emb 53	25	13	0.02	0.01	0.61	0.57	0.30	0.27	Y	1
Per-emb 61	10	6	0.01	0.00	0.21	0.19	0.24	0.22

Notes. Columns labelled “c” have been corrected using the method of Jørgensen et al. (2009), while columns labelled “u” contain the uncorrected values. Typical statistical uncertainties of the compact and extended flux densities, F_{1.3 mm} and S_{850 μm}, are 5 mJy and 0.05 Jy beam^-1, respectively. Absolute uncertainties are expected to be approximately 20%. Typical statistical uncertainties of the inferred masses, M_compact and M_env, are 0.01 M_⊙ and 0.1 M_⊙ respectively. Absolute uncertainties are expected to be on the order of magnitude scale.

^(a)

Disk candidate from resolved continuum observations.

Reference. (1) VANDAM survey, J. Tobin (priv. comm.); (2) Segura-Cox et al. (2016); (3) Tobin et al. (2015a); (4) Tobin et al. (2015b); (5) Tobin et al. (2016); (6) Lee et al. (2009); (7) Cox et al. (2015).

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