SMA observations of polarized dust emission in solar-type Class 0 protostars: Magnetic field properties at envelope scales

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Volume 616 (August 2018)

A&A, 616 (2018) A139

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Table 4.

0.87 mm integrated flux densities, source sizes, polarization intensities, and fractions.

Name	On the 0.87 mm reconstructed maps					From the visibility amplitude curve
	Flux density^a	Mass	Peak intensity	Peak P_i^b	p_frac^c	0.87 mm flux density

	(Jy)	(M_⊙)	(Jy/beam)	(mJy/beam)	(%)	(Jy)
B335	0.21±0.04	0.02	0.24	25.3	10.5	0.51±0.05
SVS13	1.40±0.28	0.29	1.06	14.8	2.5	1.54±0.15^d
HH797	0.47±0.09	0.10	0.71	5.7	3.0	0.94±0.09
L1448C	0.57±0.11	0.11	0.65	12.5	–	1.00±0.01
L1448N	1.50±0.30	0.31	1.34	20.3	2.7	1.93±0.19^d
L1448-2A	0.34±0.07	0.07	0.27	5.7	–	0.48±0.05
IRAS03282	0.44±0.09	0.09	0.65	9.9	–	1.17±0.12
NGC 1333 IRAS4A	2.38±0.48	0.50	2.57	77.3	8.8	6.79±0.68
NGC 1333 IRAS4B	1.42±0.28	0.30	2.89	14.9	4.7	4.10±0.41
IRAS16293	4.81±0.96	0.26	3.83	39.2	1.7	5.96±0.60^d
L1157	0.43±0.09	0.10	0.71	31.4	4.5	1.07±0.11
CB230	0.22±0.04	0.09	0.37	14.3	6.4	0.58±0.06

Notes.

^(a)

Flux density estimated within the central 6000 au for SVS13, 3000 au for other sources.

^(b)

Not all the sources have an intensity peak co-spatial with the polarized intensity peak.

^(c)

Polarization fraction defined as the unweighted ratio of the median polarization to total flux.

^(d)

The visibility data allows us to separate the two components of wide binaries. The fluxes are those of the object located at the phase center, e.g., L1448N-B, SVS13-B and IRAS16293-A.

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