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Table 2

Sample of unresolved multiple protostellar systems (separation <7).

System RA (J2000) Dec (J2000) Separationa ()

NGC 1333 IRAS 4A 03:29:10.51 +31:13:31.01 1.828
IRAS 03292+3039 03:32:17.95 +30:49:47.60 0.085
IRAS 03282+3035 03:31:21.00 +30:45:30.00 0.098
NGC 1333 IRAS 2A 03:28:55.57 +31:14:37.22 0.619
NGC 1333 IRAS 2B 03:28:57.35 +31:14:15.93 0.311
NGC 133 IRAS 7 Per18 03:29:11.26 +31:18:31.08 0.081
NGC 1333 IRAS 7 Per49 03:29:12.96 +31:18:14.31 0.313
L1448N C 03:25:35.53 +30:45:34.20 0.251
L1448N B 03:25:36.34 +30:45:14.94 0.226
Per17 03:27:39.09 +30:13:03.00 0.273
IC 348 MMS Per11 03:43:57.06 +32:03:04.60 2.950
NGC 1333 SVS13A 03:29:03.75 +31:16:03.76 0.3
L1448 IRS2 03:25:22.40 +30:45:12.00 0.751
L1455 FIR2 03:27:38.23 +30:13:58.80 0.346
B1-a 03:33:16.66 +31:07:55.20 0.391
EDJ2009-269 03:30:43.91 +30:32:46.28 0.539
IC 348 Per55 03:44:43.33 +32:01:31.41 0.613
EDJ2009-183 03:28:59.32 +31:15:48.14 1.022
L1448 IRS1 03:25:09.54 +30:46:21.96 1.424
NGC 1333 IRAS 1 03:28:37.00 +31:13:27.00 1.908
EDJ2009-156 03:28:51.11 +31:18:15.41 3.192
Per32 03:44:02.40 +32:02:04.89 5.910
HH211 03:43:56.80 +32:00:50.21 0.3b
Per62 03:44:12.98 +32:01:35.40 0.121c

Notes.

(a)

Separations obtained from Tobin et al. (2016). Typical uncertainties in position are <0.1.

(b)

The companion reported in Lee et al. (2009) appears to be substellar with an orbital period of 3000 yr, which could explain the jet precession. Lee et al. (2010) also argued for a third component at <30 AU, proposing that it is a very low-mass system.

(c)

Possibly unresolved binary.

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