Table 3.
Molecular lines studied in this paper.
| Lines |
Observations |
||||||
|---|---|---|---|---|---|---|---|
| Name | νrest |  |
θB | σchannel | Telescope | Ref. | |
| (GHz) | (cm−3) | (″) | (mK) | ||||
| HCN(3–2) | 265.89 | 7.3 × 104 | 6 | 1.8–2.2 | ALMA (7 m) | 1 | |
| HCO+(3–2) | 267.56 | 6.8 × 103 | 6 | 1.8–2.0 | ALMA (7 m) | 1 | |
| HCN(1–0) | 88.63 | 4.5 × 103 | 5 | 2.4–5.0 | ALMA (12 m) + IRAM30 m | 2 | |
| HCO+(1–0) | 89.19 | 5.3 × 102 | 5 | 4.2–6.6 | ALMA (12 m) + IRAM30 m | 2 | |
| CO(1–0) | 115.27 | ∼102(†) | 8 | – | BIMA+NRAO12m or ALMA (12 m+7 m+TP) | 3 | |
| CO(2–1) | 230.54 | ∼102(†) | 1.5–1.7 | 5.6–16.7 | ALMA (12 m+7 m+TP) | 4 | |
Notes. Column description: Line name; rest frequency; effective excitation density from Shirley (2015) at TK = 20 K ((†) CO lines are not included, so we quote a reasonable guess); native angular resolution of the data products; RMS noise per channel at the phase centre of each convolved and reprojected cubes (6″ × 10 km s−1); telescope; and reference (see Sect. 3.1.2 for details).
References. (1) This paper; (2) Gallagher et al. (2018b) and Jiménez-Donaire et al. (2019; 3) Helfer et al. (2003) for NGC 3351 and NGC 3627 and ALMA Verification Program for NGC 4321; (4) Leroy et al. (2021b).
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