Table 8
Summary of COM properties of CALYPSO sources.
| Source | Class(a) | Lint (b) | Menv∕Lint (b) | Cand. | CH3OH(d) | ≥3 | Chem. | COM | rCOM | rCOM | COM |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (L⊙) | (M⊙∕L⊙) | disk(c) | COMs(e) | group(f) | ∥ jet(g) | ~rdisk (h) | ~r100−150K (i) | orig.(j) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) |
| L1448-2A | 0 | 4.7 | 0.27 | n | y | n | 3 | – | n | n | ? |
| L1448-2Ab | 0? | <4.7 | >0.13 | – | y | n | – | – | – | – | – |
| L1448-NA | I | 6.4 | 0.12 | – | t | n | – | – | – | – | – |
| L1448-NB1 | 0 | <3.9 | >0.8 | n | n | n | – | – | – | – | – |
| L1448-NB2 | 0? | 3.9 | 0.40 | – | n | n | – | – | – | – | – |
| L1448-C | 0 | 11 | 0.17 | y | y | y | 3 | n | n | t | hc? |
| L1448-CS | I | 3.6 | 0.043 | – | n | n | – | – | – | – | – |
| IRAS2A1 | 0 | 47 | 0.17 | <y | y | y | 1 | y | n | y | hc, o |
| SVS13B | 0 | 3.1 | 0.9 | <y | n | n | – | – | – | – | – |
| SVS13A | I | 44 | 0.018 | y | y | y | 2 | n | n | y | hc |
| IRAS4A1 | 0 | <4.7 | >2.1 | n | n | n | – | – | – | – | – |
| IRAS4A2 | I? | 4.7 | 0.5 | y | y | y | 2 | n | y | n | a |
| IRAS4B | 0 | 2.3 | 1.4 | y | y | y | 2 | y | y | n | o, a |
| IRAS4B2 | 0? | <0.16 | >9.0 | – | n | n | – | – | – | – | – |
| IRAM04191 | 0 | 0.05 | 10 | <y | n | n | – | – | – | – | – |
| L1521F | 0 | 0.035 | 20 | <y | n | n | – | – | – | – | – |
| L1527 | 0 | 0.9 | 1.3 | y | n | n | – | – | – | – | – |
| SerpM-S68N | 0 | 11 | 1.0 | n | y | y | 2 | – | – | n | ? |
| SerpM-S68Nb | 0 | 1.8 | – | – | n | n | – | – | – | – | – |
| SerpM-SMM4a | 0 | 2.2 | 3.0 | y | n | n | – | – | – | – | – |
| SerpM-SMM4b | 0? | – | – | – | y | n | – | – | – | – | – |
| SerpS-MM18a | 0 | 13 | 0.36 | <y | y | y | 3 | y | n | n | hc, o |
| SerpS-MM18b | 0? | 16 | 0.06 | – | y | n | – | – | – | – | – |
| SerpS-MM22 | 0 | 0.36 | 2.5 | y | n | n | – | – | – | – | – |
| L1157 | 0 | 4.0 | 0.7 | <y | y | y | 3 | – | ? | t | hc?, a? |
| GF9-2 | 0 | 1.7 | 1.7 | y | n | n | – | – | – | – | – |
Notes. (a) Class according to Table 3 of Maury et al. (2019). (b)Internal luminosity and ratio of envelope mass to internal luminosity (see Table 1 for references and uncertainties). (c) Candidate disk-like structure detected and resolved (y), detected but unresolved (<y), or not detected (n) in CALYPSO continuum data (Maury et al. 2019). (d) Methanol detected (y), tentatively detected (t), or not detected (n). (e)y stands for at least three COMs detected, n for less than three. (f) Chemical group (see Sect. 3.7, Fig. 6, and Table 5). (g) Elongation of COM emission parallel to jet/outflow (y) or not (n) (see Sect. 3.5). (h) y if radius of COM emission similar to radius of candidate disk reported by Maury et al. (2019), n if not (see Fig. 13). (i) Dust temperature at radius of COM emission within 100–150 K (y: yes, t: tentative) or not (n) (see Fig. 13). (j) COM possible origin: hot corino (hc), outflow (o), accretion shock/disk atmosphere (a) (see Sect. 5.1).
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