Table 2.
H I properties of the detected sources.
| Source | FHI | MHI | Vel. range |
|---|---|---|---|
| (Jy km s−1) | (107 M⊙) | ( km s−1) | |
| NGC 1316 | 0.45 ± 0.04 | 4.3 ± 0.4 | 1500–1860 |
| EELR | 0.33 ± 0.03 | 3.1 ± 0.3 | 1780–1820 |
| SH2 | 0.30 ± 0.02 | 2.8 ± 0.2 | 1680 |
| CN, 1 | 0.39 ± 0.04 | 3.7 ± 0.3 | 1770–1860 |
| CN, 2 | 0.29 ± 0.03 | 2.7 ± 0.3 | 1770 |
| TN | 1.56 ± 0.08 | 14.7 ± 0.8 | 1780–1860 |
| TS | 4.29 ± 0.10 | 40.4 ± 1.0 | 1590–1640 |
| NGC 1310 | 5.09 ± 0.09 | 48.0 ± 0.9 | 1780–1910 |
| NGC 1317 | 2.80 ± 0.06 | 26.4 ± 0.6 | 1860–2040 |
| PGC 12706 | 1.46 ± 0.06 | 13.7 ± 0.6 | 1370–1460 |
Notes. The H I flux FHI is derived from the primary-beam-corrected image. The H I mass MHI is calculated from FHI using the equations in Meyer et al. (2017) assuming a distance of 20 Mpc. The statistical errors are obtained propagating the noise of the primary-beam-corrected H I cube to the 3D regions within which we integrate the flux. Velocities are in the barycentric reference frame (optical definition).
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