Table 2.
Observed far-IR properties of our target galaxy and clumps.
| ID | RA | Dec | z[C II] | μF[C I] | Δv | μFcont | μFUV | μ |
|---|---|---|---|---|---|---|---|---|
| (deg) | (deg) | (mJy) | (km s−1) | (μJy) | (10−31 erg s−1 cm−2 Hz−1) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| Galaxy-integrated | 01:18:11.184 | −26:58:03.826 | 3.39548 ± 0.00007 | 7.5 ± 0.7 | 122 | < 585.9 | 63.3 ± 3.2 | 5.4 ± 0.3 |
| Clump NE | 01:18:11.196 | −26:58:03.674 | – | 2.4 ± 0.6 | 61 | < 190.0 | 13.2 ± 1.2 | 5.1 ± 0.1 |
| Clump SW | 01:18:11.169 | −26:58:03.952 | – | 2.5 ± 0.6 | 81 | < 190.0 | < 2.1 | 5.8 ± 0.2 |
| Clump C (tentative) | 01:18:11.175 | −26:58:03.712 | – | 2.4 ± 0.6 | 41 | < 190.0 | < 2.1 | 5.3 ± 0.1 |
| Clump UV-C1 | 01:18:11.1882 | −26:58:03.866 | – | – | – | – | 6.6 ± 0.6 | 5.4 ± 0.1 |
| Clump UV-C2 | 01:18:11.1892 | −26:58:04.045 | – | – | – | – | 3.1 ± 0.3 | 5.7 ± 0.1 |
| Clump UV-SE | 01:18:11.2028 | −26:58:04.290 | – | – | – | – | 10.6 ± 1.0 | 5.9 ± 0.1 |
Notes. Columns: (1) Component: galaxy-integrated and individual clump measurements are reported. All the reported measurements refer to M1. While clumps NE, SW, and C are detected in [C II], clumps UV-C1, UV-C2, and UV-SE are only detected in the UV. (2) Right ascension; (3) Declination; (4) Redshift estimated by fitting the [C II] emission line with a Gaussian in our 1D ALMA spectra. The uncertainty that we report is the formal error obtained from the fit; (5) Observed [C II] emission line flux (i.e., not corrected for lensing amplification); (6) Velocity width of the line estimated considering the channels that maximize the S/N of the detection (see Sect. 3.3); (7) 5σ upper limits on the continuum emission flux (not corrected for lensing amplification). The upper limit associated to the galaxy-integrated measurement has been obtained by considering a Gaussian model with the same structural parameters used to estimate the integrated [C II] flux (Sect. 3.3). The upper limit associated to the clump measurements has instead been obtained by considering a point-spread function (PSF) model, for consistency with the [C II] flux estimates; (8) Observed UV continuum flux density. Upper limits are 5σ; (9) Average magnification (Livermore et al. 2015; Iani et al. 2021). The coordinates of the [C II] clumps are estimated as the centroid position of 2D fit performed in the uv plane with GILDAS (Sect. 3.3). We note that, when fitting relatively low S/N sources, GILDAS centroid positions might be affected by offsets, as reported by Tan et al. (2024). However, the symmetry of the M1 and M2 images due to lensing makes the comparison of the relative position of the [C II] and UV clumps robust (see Sect. 3.7.2).
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