Importance of source structure on complex organics emission - I. Observations of CH3OH from low-mass to high-mass protostars

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Table 1

Disk and estimated 100 K radii for sources with both a disk and CH₃OH detection.

Source	R_disk (au)	R_100K (au)	Normalized
Per-emb 27	20 ⁽¹⁾	147	6.6 ± 3.5(5)
Per-emb 35A	20 ⁽¹⁾	49	2.3 ± 2.2(5)
IRAS 4A1 (VLA)	35 ⁽¹⁾	46	>4.4(6)
Per-emb 26	37 ⁽²⁾	49	1.4 ± 0.6(5)
Per-emb 1	30 ⁽³⁾	30	1.8 ± 1.7(6)
Per-emb 11A	40 ⁽²⁾	30	8.8 ± 8.7(7)
HH 212	60 ⁽⁴⁾	46	8.5 ± 3.9(7)
L1551 IRS5	140 ⁽⁵⁾	91	>5.0(7)
V883 Ori	320 ⁽⁶⁾	227	1.2 ± 0.3(6)

Notes. a(b) represents a × 10^b. The 100 K radius was determined using the relation derived by Bisschop et al. (2007) for high-mass hot cores, au, which also seems to hold for low-mass protostars (van’t Hoff et al. 2022).

References. ⁽¹⁾Segura-Cox et al. (2018). ⁽²⁾Maury et al. (2019). ⁽³⁾Lee et al. (2018).⁽⁴⁾Lee et al. (2017a).⁽⁵⁾Cruz-Sáenz de Miera et al. (2019). ⁽⁶⁾Cieza et al. (2016).

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