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Table 5

Comparison of envelope, photon-heated and outflow masses over the 30 × 30′′ area surrounding the central protostar.

Source M Envelope a M Envelope b M UV c M outflow d
Total ≤ 15′′ 13CO 6−5 12CO 6−5
L1448 mm 9.0 1.69 4.0 × 10-2 ...
NGC 1333-IRAS 2A 5.13 0.67 9.9 × 10-2 8.1 × 10-3
NGC 1333-IRAS 4A 5.59 2.56 8.2 × 10-2 1.4 × 10-2
NGC 1333-IRAS 4B 3.01 2.60 5.1 × 10-2 2.2 × 10-3
L1527 0.92 0.18 2.3 × 10-2 <5.5 × 10-4
Ced110-IRS4 0.17 0.07 2.4 × 10-2 3.3 × 10-4
IRAS 15398 0.47 0.28 6.0 × 10-3 5.5 × 10-4
L483 mm 4.4 0.25 3.9 × 10-2 1.5 × 10-3
Ser-SMM1 16.13 1.99 3.0 × 10-1 7.4 × 10-3
Ser-SMM4 2.11 3.17 2.2 × 10-1 8.9 × 10-3
Ser-SMM3 3.21 0.74 2.2 × 10-1 6.1 × 10-3
L723 mm 1.32 0.67 7.2 × 10-2 1.9 × 10-3
B335 1.2 0.79 4.0 × 10-2 9.8 × 10-4
L1489 0.18 0.04 1.4 × 10-2 1.5 × 10-4
TMR1 0.23 0.04 1.6 × 10-2 2.3 × 10-4
TMC1A 0.22 0.04 7.6 × 10-3 5.3 × 10-5
TMC1 0.2 0.04 7.7 × 10-3 3.6 × 10-4
HH46-IRS 4.36 1.21 2.5 × 10-1 1.2 × 10-2
DK Cha 0.82 0.26 2.2 × 10-2 2.2 × 10-4
GSS30-IRS1 0.6 0.03 3.1 × 10-1 2.5 × 10-3
Elias 29 0.3 0.01 7.8 × 10-2 5.6 × 10-4
Oph-IRS63 0.25 0.12 3.0 × 10-3 <1.2 × 10-4
RNO91 0.45 0.05 1.1 × 10-2 1.5 × 10-4
L1551-IRS5 22.2 0.23 2.0 × 10-2 ...

Notes. All masses are given in M⊙. All masses except the total envelope mass (a) are obtained over a ~30″× 30″ (Figs. A.5, A.6)

(a)

Total mass of the spherical envelope inferred from the continuum radiative-transfer modeling (Kristensen et al. 2012).

(b)

As a, but limited to the mass within the 15″ radius over which the UV-heated component is determined.

(c)

UV photon-heated gas mass (component (ii)) as calculated from the 13CO 6−5 spectra over the mapped area after subtracting the modeled envelope emission.

(d)

Outflow mass calculated from the 12CO 6−5 map for the same area as the 13CO maps.

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