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Table 1

Physical components seen in water and high-J CO emission lines profiles.

Source type Velocity FWHM(a) CO excitation Possible origin(b)
Characteristics (km s−1) (K)
Pre-stellar Narrow <5 <10 Quiescent, infall
         
Low mass Class 0 Broad, 24 300 Warm outflow (cavity shocks, disk wind, turbulent mixing layers)
Medium/offset 18 700 Hot spot shock
Medium/EHV 700 Hot EHV bullets
Narrow 3.5 <100 Quiescent, infall, expansion
         
Low mass Class I Broad 15 300 Warm outflow (cavity shocks, disk wind, turbulent mixing layers)
Narrow 2.6 <100 Quiescent, infall, expansion
         
Intermediate mass Broad 32 300 Warm outflow (cavity shocks, disk wind, turbulent mixing layers)
Narrow 4.6 <100 Quiescent, infall, expansion
         
High mass Broad 24 300 Warm outflow (cavity shocks, disk wind, turbulent mixing layers)
Narrow 5.6 <100 Quiescent, infall, expansion
         
Disks Narrow <4 20–300 Rotating disk

Notes. (a) Median width (FWHM) of water lines at the source position, taken from San José-García et al. (2016) and Table 5.4 of San José-García (2015). Values refer to the median of the WISH sample; those including other samples, such as the WILL sample, are similar within the uncertainties of a few km s−1. (b) Based on Table 1 of Kristensen et al. (2017b).

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