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Table 2

Average fraction of the integrated intensity that the narrow (envelope) and broad (cavity shock or entrained outflowing material) components contribute to the total integrated intensity of the H2O 202–111 (988 GHz), 211–202 (752 GHz), 312–303 (1097 GHz) and 12CO J = 10–9 lines.

H2O 202–111 H2O 211–202 H2O 312–303 12CO J = 10–9
Wenvelope/Wtota   Wcavity shock/Wtot Wenvelope/Wtota   Wcavity shock/Wtot Wenvelope/Wtota   Wcavity shock/Wtot Wenvelope/Wtota   Wentrainment/Wtot

LM0 0.0 ± 0.1 0.7 ± 0.1 0.0 ± 0.1 0.7 ± 0.1 0.0 ± 0.1 0.8 ± 0.1 0.5 ± 0.1 0.5 ± 0.1
LMI 0.2 ± 0.1 0.8 ± 0.1 0.3 ± 0.2 0.7 ± 0.2 0.0 ± 0.1 1.0 ± 0.1 0.9 ± 0.1 0.1 ± 0.1
IM 0.3 ± 0.1 0.6 ± 0.2 0.4 ± 0.2 0.6 ± 0.2 0.3 ± 0.1 0.6 ± 0.1 0.5 ± 0.1 0.5 ± 0.1
HM 0.4 ± 0.2 0.6 ± 0.2 0.4 ± 0.2 0.6 ± 0.2 0.4 ± 0.1 0.6 ± 0.1 0.5 ± 0.1 0.5 ± 0.1

Notes. LM0: low-mass Class 0 protostars; LMI: low-mass Class I sources; IM: intermediate-mass YSOs; HM: high-mass objects.

(a)

As in Mottram et al. (2014), the envelope fraction, Wenvelope, is calculated subtracting the cavity shock (entrained outflowing contribution in the case of 12CO) and spot shock contribution from the total integrated intensity, Wtot, for each water and CO line, i.e., Wenvelope = WtotWbroadWspot shock, where Wbroad = Wcavity shock for H2O and Wbroad = Wentrainment for 12CO J = 10–9.

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