Table 1.
Physical properties of the ten DSFG members in the Spiderweb protocluster.
| ID | RA | Dec | z | log(M*) | SFR1.2 mm | LABOCA | HAE | CO emitter | Paβ emitter | X-ray |
|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) | (M⊙ yr−1) | ID | ID | ID | ID | ID | ||||
| 04 | 11:40:53.21 | −26:29:11.1 | 2.188 | 10.94 ± 0.08 | 447 ± 66 | 02 | – | – | – | – |
| 05 | 11:40:46.06 | −26:29:11.3 | 2.149 | 11.37 ± 0.12 | 481 ± 74 | – | 902 | 01ext | – | – |
| 12 | 11:40:46.66 | −26:29:10.2 | 2.166 | 10.90 ± 0.11 | 214 ± 38 | – | 880 | 15ext | – | 87 |
| 14 | 11:40:40.86 | −26:29:46.8 | 2.163 | 10.29 ± 0.28 | 307 ± 50 | – | – | 23ext | – | – |
| 17 | 11:40:48.34 | −26:29:08.5 | 2.162 | 12.42 ± 0.07 | 378 ± 65 | 07 | 73 | 02ext | 30 | 58 |
| 20 | 11:40:51.27 | −26:29:38.6 | 2.151 | 10.90 ± 0.10 | 285 ± 59 | – | 1300 | 09 | – | – |
| 23 | 11:40:54.56 | −26:28:23.8 | 2.161 | 10.73 ± 0.10 | 179 ± 42 | – | 1162 | 45 | – | – |
| 28 | 11:40:54.74 | −26:28:03.1 | 2.152 | 10.83 ± 0.09 | 151 ± 36 | 15 | 1181 | – | – | – |
| 29 | 11:40:38.58 | −26:30:25.5 | 2.121 | 10.05 ± 0.15 | 113 ± 36 | – | – | 34 | – | – |
| 47 | 11:40:51.11 | −26:29:05.1 | 2.146 | 10.46 ± 0.26 | 182 ± 44 | – | – | 38ext | – | – |
Notes. Stellar masses are adopted from Pérez-Martínez et al. (2023) and Shimakawa et al. (2024b), or derived from NIR luminosities measured by JWST/NIRCam (see Sect. 3.4.2). SMG, HAE, and CO emitter IDs follow Dannerbauer et al. (2014), Pérez-Martínez et al. (2023), Shimakawa et al. (2024b), and Jin et al. (2021), respectively, with extended gas reservoirs marked in boldface (Chen et al. 2024). Paβ and X-ray counterparts are cross-matched from Shimakawa et al. (2024a) and Tozzi et al. (2022a).
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