Table 2.
Continuum properties.
| Source | RA | Dec | E(RA) | E(Dec) | FWHM | νObs | Sν, Obs |
|---|---|---|---|---|---|---|---|
| J2000 | J2000 | (arcsec) | (arcsec) | (arcsec) | (GHz) | (mJy) | |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| III Zw 035 | 01:44:30.538 | 17:06:08.68 | 0.01 | 0.01 | 0.43 ± 0.01 | 112.2 | 3.84 ± 0.03 |
| IRAS F05189−2524 | 05:21:01.401 | −25:21:45.28 | 0.01 | 0.01 | 0.17 ± 0.03 | 104.1 | 2.40 ± 0.03 |
| NGC 2623 | 08:38:24.087 | 25:45:16.67 | 0.01 | 0.02 | 1.22 ± 0.06 | 113.2 | 6.40 ± 0.08 |
| IRAS F09111−1007 W | 09:13:36.452 | −10:19:30.00 | 0.01 | 0.01 | 0.76 ± 0.11 | 102.3 | 1.33 ± 0.03 |
| IRAS F09111−1007 E | 09:13:38.829 | −10:19:19.98 | 0.01 | 0.01 | < 3.12 | 102.3 | 0.62 ± 0.12 |
| IRAS F10173+0828 | 10:20:00.203 | 08:13:33.93 | 0.01 | 0.01 | < 0.75 | 102.9 | 1.72 ± 0.03 |
| IRAS F12224−0624 | 12:25:03.909 | −06:40:52.63 | 0.01 | 0.01 | < 0.48 | 105.8 | 2.33 ± 0.33 |
| NGC 4418 | 12:26:54.610 | −00:52:39.45 | 0.01 | 0.01 | 0.17 ± 0.05 | 107.7 | 11.13 ± 0.04 |
| IC 860 | 13:15:03.505 | 24:37:07.70 | 0.01 | 0.01 | < 0.54 | 113.8 | 6.64 ± 0.08 |
| IRAS 13120−5453 | 13:15:06.328 | −55:09:22.80 | 0.01 | 0.01 | 0.89 ± 0.03 | 105.3 | 10.07 ± 0.16 |
| IRAS F14378−3651 | 14:40:59.013 | −37:04:31.91 | 0.01 | 0.01 | 0.37 ± 0.05 | 101.4 | 1.47 ± 0.06 |
| IRAS F17207−0014 | 17:23:21.959 | −00:17:00.91 | 0.01 | 0.01 | 0.66 ± 0.06 | 104.1 | 8.70 ± 0.06 |
| IRAS F20551−4250 | 20:58:26.792 | −42:39:00.29 | 0.01 | 0.01 | 0.25 ± 0.03 | 104.1 | 2.78 ± 0.05 |
| NGC 7469 | 23:04:56.634 | 12:19:22.67 | 0.04 | 0.04 | 0.89 ± 0.15 | 114.4 | 1.77 ± 0.09 |
Notes. Results are from UV fitting a Gaussian model to the NOEMA continuum visibilities, and from fitting a Gaussian model to the ALMA continuum image. IRAS F09111−1007E is not part of our sample but detected along with IRAS F09111−1007W. (1) Source name. (2), (3) Continuum position. (4), (5) Uncertainties of position. These include only the formal fit errors, to which 2–5% of the beam size should be added to account for phase calibration stability (Warmels et al. 2018). (6) Intrinsic source full width at half maximum FWHM (beam-deconvolved). (7) Observed frequency. (8) Total continuum flux density from Gaussian fit.
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