Table 2.
Properties of the ALMA maps and measurement of FIR sizes and flux densities at rest-frame ∼260 μm.
| ID | Beam size | rms | S/N | Best model | F(260 μm) | Re | Re | Axial ratio | PA | fAGN | fsync | αr |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| [arcsec2] | [μJy beam−1] | [mJy] | [arcsec] | [kpc] | [deg.] | % | % | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | |
| X_N_81_44 | 0.23 × 0.22 | 31.44 | 22.7 | Exponential | 1.13 ± 0.16 | 0.10 ± 0.01 | 0.83 ± 0.10 | 1.00 ± 0.11* | – | < 1 | < 1 | –0.70 |
| XID36 | 0.22 × 0.21 | 26.62 | 21.5 | Exponential | 1.05 ± 0.13 | 0.12 ± 0.01 | 1.00 ± 0.10 | 1.22 ± 0.12* | – | 3 | < 1 | –1.25 |
| XID419 | 0.22 × 0.21 | 23.49 | 9.8 | Gaussian | 0.43 ± 0.05 | 0.10 ± 0.01 | 0.79 ± 0.12 | 2.9 ± 0.8 | 88 ± 5 | 4 | < 1 | –0.70 |
| cid_1057 | 0.18 × 0.16 | 16.34 | 3.6 ( ⋆ ) | Point | 0.06 ± 0.02 | – | – | – | – | 3 | < 1 | –0.70 |
| cid_346 | 0.27 × 0.22 | 31.40 | 29.0 | Gauss.+point | 2.58 ± 0.14 | 0.19 ± 0.01 | 1.61 ± 0.09 | 1.3 ± 0.1 | 2 ± 5 | < 1 | < 1 | –0.98 |
| cid_451 | 0.26 × 0.23 | 16.25 | 5.9 ( ⋆ ) | Exponential | 0.29 ± 0.09 | 0.24 ± 0.07 | 1.98 ± 0.55 | 3.1 ± 0.8 | –58 ± 5 | 6 | 21 | –0.99 |
| cid_1205 | 0.25 × 0.25 | 16.20 | 16.6 | Point | 0.27 ± 0.02 | < 0.12 | < 2.06 | – | – | < 1 | < 1 | –0.70 |
| cid_1143 | 0.25 × 0.23 | 14.76 | 12.1 | Exponential | 0.46 ± 0.11 | 0.25 ± 0.05 | 2.01 ± 0.41 | 4.6 ± 0.7 | 23 ± 2 | < 1 | < 1 | –0.70 |
Notes. (1) Synthesized beam size (FWHM) of the ALMA maps created with Briggs weighting with robust = 2. (2) rms noise (measured from the ‘clean’ maps). (3) Peak signal-to-noise in the ALMA map. (4) Best fit model to the uv-visibility data, according to the Bayesian Information Criterion (BIC). ( ⋆ )If the peak S/N < 8 in the ALMA maps, we do not consider the size measurements to be reliable. (5) Flux density at rest-frame ∼260 μm, measured from the uv-visibilities using the best model. (6) Half-light radius (deconvolved from the beam) in arcsec measured from the uv-visibilities using the best model. For cid_1057 the radius is not reported due to the low S/N. (7) Half-light radius in kpc. (8) Axial ratio measured using uvmodelfit (excluding point sources). Axial ratios consistent with one are marked with *. (9) Position angle (PA) measured using uvmodelfit for the objects with axial ratios significantly different from one. The PA measures the angle of the major axis with respect to the north in anti-clockwise direction. (10) AGN contribution to the rest-frame 260 μm ALMA flux, estimated from the SED fit. (11) Contribution from synchrotron emission to the rest-frame 260 μm ALMA flux. We model the synchrotron emission as a power law with a spectral index αr. (12) Spectral index αr used to estimate the synchrotron contribution, calculated from the 1.4, 3 and 5.5 GHz data (when available). In the cases where we could not constrain αr with the available data, we assume αr = −0.7 (see Sect. 5.1).
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