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Table 7

Properties of observed embedded RSDs.

Source M ⋆ M disk R K a M⋆/Mtotb Mdisk/M⋆ Θdiskc Θrotationd λ eff e References
[M⊙] [M⊙] [AU] [deg] [deg]
Class 0
NGC1333 IRAS4A2 0.08 0.25 310 0.02 3.1 108.9 ... ... 1,2,3
L1527 0.19 0.029–0.075 90 0.2 0.13–0.34 0 –177 ... 1, 2, 4, 5
VLA1623 0.20 0.02 150 0.4–0.6 0.1 –145 ... ... 6,7
Class I
R CrA IRS7B 1.7 0.024 50 0.43 0.01 –65 ... ... 8
L1551 NE 0.8 0.026 300 0.65 0.032 167 ... ... 9
L1489-IRS 1.3 0.004 200 0.83–0.93 0.0030 –120 110 ... 1, 2, 10
IRS43 1.9 0.004 190 0.89 0.002 107 ... ... 1, 12
IRS63 0.8 0.099 165 0.83 0.12 –10 ... ... 11, 12
Elias29 2.5 0.011 200 0.98 <0.003 ... ... ... 11
TMC1A 0.53 0.045–0.075 100 0.75–0.78 0.08–0.14 –115 25 >10 13
TMC1 0.54 0.005–0.024 100 0.76–0.79 0.01–0.06 –90 35 4 13
TMR1 0.7 0.01–0.015 <50 0.72f 0.02–0.03 ... ... ... 13
L1536g 0.4 0.007–0.024 80 0.95–0.97 0.02–0.06 –95 –7 ... 13

Notes.

(a)

Outer radius of the Keplerian disk.

(b)

Mtot = M⋆ + Mdisk + Menv.

(c)

Direction of the disk rotation from blue to red.

(d)

Direction of the envelope rotation associated to or near the sources from Caselli et al. (2002) except for L1527 whose value is from Goodman et al. (1993).

(e)

Effective mass-to-flux ratio scaled from the average value in Troland & Crutcher (2008) with magnetic field strengths from Crutcher et al. (2010).

(f)

Stellar mass adopted from Hogerheijde et al. (1998), which assumes that all of the luminosity is due the star.

(g)

The stellar mass is sum of the two stars in the binary.

Reference. (1) Jørgensen et al. (2009); (2) Kristensen et al. (2012); (3) Choi et al. (2010); (4) Tobin et al. (2012); (5) Tobin et al. (2013); (6) Murillo & Lai (2013); (7) Murillo et al. (2013); (8) Lindberg et al. (2014); (9) Takakuwa et al. (2012); (10) Brinch et al. (2007); (11) Lommen et al. (2008); (12) Brinch & Jørgensen (2013); (13) This work.

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