Table 2.
Properties of the different clumps detected with ALMA.
| Clump | ∫SHCO+dv | FWHM | vpeak | ∫SCOdv | ∫SHCNdv | ∫SSiOdv | IHCO+/ICO | IHCO+/IHCN | IHCN/ICO |
|---|---|---|---|---|---|---|---|---|---|
| (mJy km s−1) | (km s−1) | (km s−1) | (Jy km s−1) | (mJy km s−1) | (mJy km s−1) | ||||
| 1 | 41.8 ± 7.2 | 37 ± 7 | ∼ − 206 | 1.23 ± 0.04 | < 32.3 | < 37.9 | 0.057 ± 0.012 | > 1.28 | < 0.044 |
| 2 | 20.0 ± 3.3 | 28 ± 5 | ∼ − 237 | 0.43 ± 0.03 | < 15.7 | < 15.9 | 0.078 ± 0.018 | > 1.26 | < 0.062 |
| 3 | 22.9 ± 4.8 | 24 ± 8 | ∼ − 239 | 0.53 ± 0.03 | < 17.0 | < 16.2 | 0.072 ± 0.019 | > 1.33 | < 0.054 |
| 4 | 42.3 ± 6.9 | 36 ± 5 | ∼ − 247 | 2.35 ± 0.07 | < 38.2 | < 36.3 | 0.030 ± 0.006 | > 1.09 | < 0.027 |
| 5 | 71.3 ± 8.7 | 56 ± 8 | ∼ − 257 | 3.38 ± 0.11 | < 52.5 | < 64.3 | 0.035 ± 0.005 | > 1.34 | < 0.026 |
| 6 | 75.6 ± 5.2 | 16 ± 1 | ∼ − 224 | 1.97 ± 0.08 | < 13.3 | < 15.8 | 0.064 ± 0.007 | > 5.61 | < 0.011 |
| 7 | 41.0 ± 4.8 | 23 ± 3 | ∼ − 234 | 1.63 ± 0.07 | < 17.9 | < 14.9 | 0.042 ± 0.007 | > 2.26 | < 0.019 |
| 8 | 194.1 ± 12.7 | 54 ± 3 | ∼ − 291 | 11.93 ± 0.26 | < 89.4 | < 104.0 | 0.027 ± 0.002 | > 2.14 | < 0.013 |
| 9 | 40.6 ± 6.6 | 47 ± 12 | ∼ − 267 | 1.91 ± 0.06 | < 37.9 | < 41.0 | 0.036 ± 0.007 | > 1.06 | < 0.034 |
| Total | 549.6 ± 21.5 | 25.36 ± 0.32 | < 314.2 | < 346.3 | 0.036 ± 0.002 | > 1.73 | < 0.021 | ||
| Average | 0.043 ± 0.018 | > 1.51 | < 0.029 | ||||||
Notes. The clump numbers are the same as those indicated in Fig. 1. The integrated flux densities were derived by summing the channels where emission is detected, multiplied by the channel width. The velocity (relative to Centaurus A) and FWHM were estimated by fitting the spectrum with a single Gaussian profile. For the HCN(1–0) and SiO(2–1) emission, upper limits at 3σ were derived assuming the same FWHM and the same area as for HCO+(1–0). The last three columns report the line ratios of the integrated intensities in K.km.s−1 and are therefore corrected by the ratio of the rest frequencies (see Sect. 4).
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