Table 3
Estimated critical densities (at 15 K) and maximum radii for the three ALMA pre-BD core candidates to be gravitationally unstable.
| APEX/LABOCA | ALMA | |||||||||
| ncrita | nobsb | Rmaxc | Robsd | Dynamical | ncrita | nobsb | Rmaxc | Robsd | Dynamical | |
| Core | [cm-3] | [cm-3] | [AU] | [AU] | state | [cm-3] | [cm-3] | [AU] | [AU] | state |
|
|
||||||||||
| LB08 | 3.3 × 106 | 2.5 × 104 | 971 | 5400 | stable/transient | 5.0 × 108 | >1.3 × 108 | 82 | <140 | infalling? |
| LB10 | 1.7 × 107 | >1.0 × 104 | 421 | 1200∗–5520 | stable? | 3.4 × 109 | >4.9 × 107 | 28 | <140 | infalling? |
| LB31 | 5.5 × 106 | >1.8 × 104 | 751 | 1200∗–5520 | stable? | 4.5 × 1010 | >1.3× 107 | 8 | <140 | infalling? |
Notes.
Critical density estimated following Eq. (3), and using the corresponding APEX/LABOCA or ALMA mass for a temperature of 15 K, as given in Table 1;
Measured density using the APEX/LABOCA or ALMA masses given in Table 1, obtained for a temperature of 15 K, and using the measured size or the beam size as upper limit if the source is unresolved;
Maximum radii corresponding to the critical density given in this table, and using the mass used to obtain the critical density;
Measured radii in the APEX/LABOCA or ALMA observations. If the sources are unresolved we give half of the beam size as un upper limit for the radius. The lower limit of the radius in the APEX/LABOCA column corresponds to half the LAS. We adopted this value as a lower limit for the radius of the APEX/LABOCA core given that >90% of the flux is filtered out by ALMA.
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