Table 1.
Candidate remnant radio sources.
| ID | Source name | Redshift | M* | Cluster |
|---|---|---|---|---|
| [×1011 M⊙] | flag | |||
| 1 | J102818+560811 | 0.52 ± 0.05p | 2 ± 1 | 0 |
| 2 | J102842+575122 | 0.4 ± 0.1p | 0.1 ± 0.1 | 0 |
| 3 | J102905+585721 | 0.53 ± 0.03p | 8 ± 3 | 0 |
| 4 | J102917+584208 | – | – | 0 |
| 5 | J103132+591549 | 1.8686 |
– | 0 |
| 7 | J103602+554007 | 0.68 ± 0.07p | 6 ± 4 | 0 |
| 8 | J103641+593702 | 0.47 ± 0.03p | – | 0 |
| 9 | J103805+601150 | 0.73 ± 0.05p | 27 ± 15 | 0 |
| 10 | J104208+592030 | 0.5099 ± 0.0001s | 12 ± 3 | 0 |
| 11 | J104516+563148 | 0.1092 |
0.57 |
0 |
| 12 | J104646+564744 | 0.3032 |
– | 0 |
| 13 | J104732+555007 | 0.57 ± 0.04p | 3 ± 2 | 0 |
| 14 | J105230+563602 | 0.25 ± 0.03p | 0.9 ± 0.3 | 0 |
| 15 | J105402+550554 | 0.38249 ± 0.00006s | – | 1 |
| 16 | J105554+563532 | 2.1752 |
– | 0 |
| 17 | J105703+584721 | 0.83053 ± 0.00005s | 4 ± 2 | 0 |
| 18 | J105729+591128 | 0.47 ± 0.02p | 6 ± 3 | 0 |
| 19 | J110108+560330 | 0.4 ± 0.1p | – | 0 |
| 20 | J110136+592602 | 0.49 ± 0.05p | 9 ± 11 | 0 |
| 21 | J110255+585740 | 0.3391 ± 0.0001s | 2.1 ± 0.8 | 1 |
| 22 | J110420+585409 | 0.66 ± 0.05p | 40 ± 50 | 0 |
| 23 | J110806+583144 | 0.15431 ± 0.00003s | 0.07 ± 0.06 | 1 |
Notes. ID listed in Col. 1 is used in the flow chart showing the process of the optical identification. In Col. 2 are the source names in J2000 coordinates; Col. 3 notes the redshift of the optical host galaxy, where ‘p’ indicates SDSS photometric and ‘s’ SDSS spectroscopic redshift, ‘LD’ and ‘lp’ come from the LoTSS Deep Fields catalogues, where ‘lp’ indicates that the redshift is obtained from the limited photometry – indicating less reliable redshifts; Col. 4 shows stellar masses; Col. 5 lists environment flags where ‘1’ means that the source is in a cluster. In the LoTSS Deep Fields catalogues, errors on the redshift are not symmetrical and therefore we quote minimum and maximum redshift values from the respective catalogues. The maximum and minimum value of the M* for the source J1045+5631 is calculated using the maximum and minimum redshift for this source. Sources without the optical and/or infrared identification do not have a measurement of the stellar mass (see Jurlin et al. 2020).
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