Table 9.
Protoclusters in the Cosmos field at 2.0 < z < 2.5.
| Name | Redshift | N spec. | Mh(z = 0) | ΣSFR | Extent | N. DSFG (a) | Reference |
|---|---|---|---|---|---|---|---|
| [zmin − zmax] | members | (1014 M⊙) | (M⊙ yr−1) | (arcmin) | & AGN | ||
| ZFIRE | 2.085 [2.076–2.104] | 57 | 2.5 |
4002 | 7.4 × 10 | 9 & 4 | (1,2) |
| CC2.2 | 2.233 [2.122–2.247] | 47 | 9.2 | 2228 | 9.2 × 9.2 | 0 & 3 | (3) |
| COS1000+0215 | 2.444 [2.428–2.456] | 20 | 3.2 |
... | 5.0 × 3.1 | 0 & 4 | (4,5) |
| PCL 1002 | 2.472 [2.463–2.487] | 41 | 77 (b) |
4447 | 3.0 × 1.5 | 7 & 5 | (6) |
| CL J1001 | 2.507 [2.494–2.515] | 18 | 83 (b) |
2790 | 2.7 × 3.0 | 1 & 1 | (7,8) |
| G237 ss1 | 2.155 [2.150–2.164] | 20 | 6.6 |
1002 ± 58 | 9.5 × 9.3 | 3 & 4 | (This work) |
| G237 ss2 | 2.195 [2.190–2.199] | 8 | 5.1 |
429 ± 41 | 9.9 × 10.6 | 1 & 0 | (This work) |
Notes.
Here, we consider a DSFG a galaxy detected in the sub-mm by SPIRE, SCUBA-2, LABOCA, or AzTEC, even if it might comprise multiple galaxies as in the case of CL J1001 where ALMA finds five sources associated with a single SPIRE source (Wang et al. 2016).
For PCL 1002, and CL J1001, the z = 0 halo masses have been derived from the estimated halo mass at the observed redshift (Casey et al. 2015; Wang et al. 2016), these are (8 ± 3) × 1013 M⊙ for PCL 1002, and (7.9
) × 1013 M⊙ for CL J1001, and assuming the mass growth as formulated by Behroozi et al. (2013), to be consistent with the other structures analyzed here. These are larger than those derived by Casey et al. (2015), and Wang et al. (2016) assuming a mass-dependent exponential growth model (i.e., (2 ± 1) × 1015 M⊙).
References. (1) Yuan et al. (2014), (2) Hung et al. (2016), (3) Darvish et al. (2020), (4) Diener et al. (2015), (5) Chiang et al. (2015) (6) Casey et al. (2015), (7) Wang et al. (2016), (8) Wang et al. (2018).
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