Table 2.
Basic properties of the group galaxies and H I detected sources within the H I image field of view.
| Source | Integrated flux | H I mass | Morphological type | Stellar mass | g − r |
|---|---|---|---|---|---|
| (Jy km s−1) | (107 M⊙) | (109 M⊙) | (mag) | ||
| NGC 1310 | 5.13 ± 0.07 | 48.1 ± 0.6 | SBcII | 4.7 | 0.6 ± 0.1 |
| NGC 1316 | 0.72 ± 0.04 | 6.8 ± 0.4 | SAB0 | 600 | 0.72 ± 0.01 |
| NGC 1316C | 0.18 ± 0.02 | 1.7 ± 0.2 | SdIII pec | 1.4 | 0.7 ± 0.1 |
| NGC 1317 | 2.96 ± 0.02 | 27.8 ± 0.2 | Sa pec | 17.1 | 0.77 ± 0.02 |
| NGC 1326 | 24.3 ± 0.5 | 228 ± 4 | SBa(r) | 29.4 | 0.62 ± 0.04 |
| NGC 1326A | 15.2 ± 0.8 | 142 ± 8 | SBcIII | 1.7 | 0.5 ± 0.1 |
| NGC 1326B | 49 ± 1 | 455 ± 9 | SdIII | 1.8 | 0.3 ± 0.1 |
| ESO 301-IG 11 | 1.52 ± 0.04 | 14.3 ± 0.4 | SmIII | 2.9 | 0.57 ± 0.04 |
| FCC 19 | < 0.03 | < 0.17 | dS0 | 0.18 | 0.62 ± 0.04 |
| FCC 35 | 3.51 ± 0.09 | 33.0 ± 0.8 | SmIV | 0.17 | 0.2 ± 0.1 |
| FCC 40 | < 0.15 | < 0.72 | dE4 | 0.002 | 0.61 ± 0.04 |
| FCC 46 | 0.13 ± 0.03 | 1.2 ± 0.2 | dE4 | 0.58 | 0.46 ± 0.01 |
| TN | 2.24 ± 0.07 | 21.0 ± 0.7 | – | – | – |
| TS | 4.86 ± 0.08 | 45.6 ± 0.7 | – | – | – |
| CN, 1 | 0.75 ± 0.05 | 7.0 ± 0.5 | – | – | – |
| CN, 2 | 0.35 ± 0.03 | 3.3 ± 0.3 | – | – | – |
| EELR | 0.49 ± 0.02 | 4.6 ± 0.2 | – | – | – |
| SH2 | 0.31 ± 0.02 | 2.9 ± 0.2 | – | – | – |
| Remaining clouds | 3.0 ± 0.2 | 28 ± 2 | – | – | – |
Notes. The primary beam-corrected integrated H I flux, mass, and upper limits are included for all sources while the morphological type, stellar mass, and g − r colour is included for all the galaxies. The H I mass was calculated using a distance of 20 Mpc and the statistical uncertainty of the flux was measured and propagated to the H I mass. The 3σ upper limits of the H I flux and mass are calculated for non-detections using the local rms and a 100 km s−1 wide integrated flux for a point source. All previously known sources are individually identified and the remaining H I IGM detections are summed into the remaining clouds category. The galaxy morphologies are classified in Ferguson (1989), the photometry is used to estimate the stellar mass (with the method of Taylor et al. 2011), and g − r colours are measured in Raj et al. (2020) for the majority of the galaxies and in Venhola et al. (2018) for FCC 19 and FCC 40. The photometry, g − r colour, and stellar mass of NGC 1316 are measured independently in Iodice et al. (2017).
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