Table 3.
Analysis of the HCN(1–0) and HCO+(1–0) outflowing clumps.
| ID | Spectral fit (Gaussian) |
uv visibility fit (point source model) |
|||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| v | σv |
 |
 |
S/N | ∫SHCNdv | Mmol (‡) | δRA | δDec | S/N | ∫SHCNdv | |
| [km s−1] | [km s−1] | [mJy] | [mJy] | (HCN) | [Jy km s−1] | [108 M⊙] | [″] | [″] | [Jy km s−1] | ||
| A1 | −465 ± 2 | 9 ± 2 | 2.4 ± 0.8 | 4.4 ± 0.9 | 4.9 | 0.10 ± 0.03 | 0.5–3.6 | −0.05 ± 0.13 | 0.17 ± 0.12 | 4.8 | 0.11 ± 0.02 |
| A2 | −406 ± 2 | 7 ± 2 | 1.6 ± 0.9 | 3.9 ± 1.0 | 3.9 | 0.07 ± 0.03 | 0.3–2.4 | 0.03 ± 0.15 | 0.09 ± 0.13 | 4.4 | 0.08 ± 0.02 |
| A3 | 313 ± 3 | 11 ± 3 | 2.2 ± 0.8 | 3.6 ± 0.8 | 4.5 | 0.10 ± 0.03 | 0.4–3.4 | 0.11 ± 0.10 | −0.23 ± 0.09 | 6.2 | 0.15 ± 0.03 |
| B1 | −665 ± 4 | 14 ± 4 | < 2.1 (†) | 3.0 ± 0.7 | 4.3 | 0.11 ± 0.04 | 0.5–3.7 | −0.28 ± 0.10 | −0.16 ± 0.09 | 6.6 | 0.17 ± 0.03 |
| B2 | −349 ± 6 | 20 ± 6 | < 2.1 (†) | 2.8 ± 0.7 | 4.0 | 0.14 ± 0.05 | 0.6–4.9 | −0.12 ± 0.09 | 0.12 ± 0.08 | 7.1 | 0.24 ± 0.03 |
| B3 | 526 ± 3 | 11 ± 3 | < 2.7 (†) | 4.1 ± 0.9 | 4.6 | 0.11 ± 0.04 | 0.5–3.9 | −0.11 ± 0.09 | 0.10 ± 0.08 | 7.4 | 0.16 ± 0.02 |
| C1 | −297 ± 6 | 13 ± 6 | 2.1 ± 0.8 | < 2.4 (†) | < 3 | < 0.07 (†) | < 2.0 (†) | ||||
Notes.
range of dense molecular gas masses estimated from the HCN(1–0) line luminosity following 
, assuming αHCN ∈ [3.1, 24] M⊙ (K km s−1 pc2)−1, where the lower αHCN value has been proposed by García-Burillo et al. (2012) for (U)LIRGs, and the higher αHCN has been measured by Leroy et al. (2015) for individual GMCs in the starburst region of NGC 253. We note that both Gao & Solomon (2004), based on integrated observations of local galaxies and on the assumption that HCN traces very dense gas, and Shimajiri et al. (2017), based on observations of Galactic GMCs (see also Kauffmann et al. 2017) proposed an intermediate value of αHCN = 10 M⊙ (K km s−1 pc2)−1.
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