Table 1.
Summary of the four VLBA-AGN’s properties.
| IDVLBA | RA | Dec | z | log(M★/M⊙) | rmsVLBA | SVLBA | log LVLBA | log LVLA | log(LIR/L⊙) | qIR |
|---|---|---|---|---|---|---|---|---|---|---|
| [deg] | [deg] | [μJy/beam] | [μJy] | [W/Hz] | [W/Hz] | |||||
| 338 | 150.28249 | 2.34445 | 1.48 | 10.85 ± 0.04 | 5.6 | 50.2 ± 12.9 | 23.77 ± 0.13 | 24.19 ± 0.02 | 12.14 ± 0.04 | 1.95 ± 0.04 |
| 351 | 150.25549 | 2.36649 | 2.92 | 10.80 ± 0.04 | 6.1 | 41.4 ± 9.3 | 23.88 ± 0.11 | 24.80 ± 0.02 | 12.62 ± 0.15 | 1.84 ± 0.15 |
| 408 | 150.38951 | 2.25589 | 1.30 | 11.10 ± 0.04 | 5.6 | 58.2 ± 13.4 | 23.69 ± 0.11 | 24.20 ± 0.08 | 11.87 ± 0.05 | 1.68 ± 0.09 |
| 498 | 150.22804 | 2.26971 | 0.68 | 10.65 ± 0.04 | 6.7 | 37.2 ± 7.8 | 22.79 ± 0.10 | 23.32 ± 0.03 | 11.69 ± 0.03 | 2.37 ± 0.04 |
Notes. Columns are (1) VLBA identification number; (2) and (3) VLBA centroid coordinates; (4) spectroscopic redshifts: z = 1.48 (Kashino et al. 2022), z = 2.92 (Horowitz et al. 2022), z = 1.30 (Kartaltepe et al. 2022), z = 0.68 (van der Wel et al. 2022); (5) stellar mass in Chabrier IMF (Shuntov et al. 2025); (6) average VLBA rms (μJy/beam); (7) rest-frame VLBA 1.4 GHz flux density in μJy (SVLBA); (8) rest-frame VLBA 1.4 GHz luminosity; (9) VLA 1.4 GHz rest-frame radio luminosity; (10) total IR luminosity (rest-frame 8−1000 μm) obtained from SED-fitting with deblended IR fluxes; (11) IR-to-radio luminosity ratio (see Eq. 1).
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