Table C.2.
Comparison sample of extended radio sources (ECS). Only the first six rows of the table are shown here for illustration. Uncertain data are indicated by a colon. The full list is available in electronic form from the VizieR Service of the CDS Strasbourg.
| SDSS name | RA | DEC | z | Ri | SDSS class | log Lr | LLS | FR | αr | e_αr | |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | |
| 1 | J005727.88+020934.5 | 14.36620 | 2.15960 | 0.292 | 3.86 | GAL | 25.9 | 182 | I | −0.80 | 0.03 |
| 2 | J022507.93−003532.9 | 36.28307 | −0.59248 | 0.685 | 4.08 | QSO | 27.3 | 97 | II | −0.69 | 0.07 |
| 3 | J073050.66+445600.8 | 112.71112 | 44.93359 | 0.072 | 1.33 | GAL | 24.0 | 47 | II: | −0.78 | 0.11 |
| 4 | J074919.08+200753.7 | 117.32951 | 20.13160 | 0.368 | 3.00 | GAL | 25.7 | 178 | II | −0.91 | 0.11 |
| 5 | J075529.95+520450.6 | 118.87473 | 52.08079 | 0.140 | 2.47 | GAL | 24.7 | 61 | II | −0.97 | 0.11 |
| 6 | J075628.79+501716.3 | 119.11996 | 50.28787 | 0.134 | 1.79 | GAL | 24.8 | 148 | II | −0.59 | 0.09 |
| tWHAN | tSED | tWISE | D4000n | e_D4000n | log SFR | log ℳ* | f_S | tm | SDSS name of PSS-CSO | ||
| (12) | (13) | (14) | (15) | (16) | (17) | (18) | (19) | (20) | (21) | ||
| 1 | - | 2 | pass | 1.86 | 0.61 | - | - | - | 0.00 | J002225.42+001456.1 | |
| 2 | - | 3 | QSO | - | - | - | - | - | - | J154609.52+002624.6 | |
| 3 | RG+P | 1 | pass | 2.00 | 0.03 | −3.67 | 11.29 | 0.00 | 0.00 | J083411.09+580321.4 | |
| 4 | - | 2 | inter | 1.88 | 0.97 | - | - | - | - | J084856.57+013647.8 | |
| 5 | SF | 2 | inter | 1.43 | 0.04 | 0.24 | 10.57 | 1 | 0.00 | J092405.30+141021.4 | |
| 6 | RG+P | 1 | pass | 1.93 | 0.07 | −3.20 | 11.77 | 1 | 3.00 | J083139.79+460800.8 | |
Notes. (1) SDSS name; (2)-(3) right ascension and declination (degrees); (4) redshift; (5) radio loudness parameter (Sect. 2); (6) SDSS spectral class; (7) 1.4 GHz radio luminosity (W Hz−1); (8) projected largest linear size (kpc); (9) FR type; (10) - (11) radio slope at ν > 1 GHz and uncertainty; (12) type based on WHAN diagram; (13) spectral type from MBSED (Table 4); (14) type based on WISE W1 − W2 vs. W2 − W3 diagram (Fig. 12); (15) - (16) 4000 Å break and uncertainty; (17) - (19) SFR (ℳ⊙ yr−1), stellar mass (ℳ⊙) and uncertainty flag from Chang et al. (2015); (20) merger index based on images from the DESI Legacy Surveys; (21) counterpart in the PSS-CSO sample.
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