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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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