Table A.2.
Properties of distant BCG (candidates) observed in CO.
| (Proto-)cluster | Galaxy | z | Transition | Telescope | rJ1 | αCO |  |
M⋆ | SFR | SFRMS |
|---|---|---|---|---|---|---|---|---|---|---|
 |
(1010 K km s−1 pc2) | (1010 M⊙) | (M⊙/yr) | (M⊙/yr) | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| SpARCS1049+56 at z = 1.71 | ||||||||||
| (Webb et al. 2015b, 2017) | J104922.6+564033 | 1.709 | 2 → 1 | LMT | 0.85 | 0.80 |
 |
45.0 | 856 ± 128 | 281.6 |
| Cl J1449+0856 at z = 1.99 | ||||||||||
| (Gobat et al. 2011, | ||||||||||
| Coogan et al. 2018) | A1 | 1.990 | 4 → 3 | ALMA | 0.36 | 3.60 |
 |
 |
227 ± 22 | 379.2 |
| Spider Web proto-cluster at z = 2.16 | ||||||||||
| (Emonts et al. 2013, 2016) | ||||||||||
| (Hatch et al. 2008, 2009) | MRC 1138-262 | 2.161 | 1 → 0 | ATCA | 1.00 | 4.00 |
 |
 |
 |
765.2 |
| Candels-5001 at z = 3.473 | ||||||||||
| (Ginolfi et al. 2017) | Candels-5001 | 3.473 | 4 → 3 | ALMA | 0.33 | 10.00 |
 |
 |
 |
55.6 |
| DES-RG 399 at z = 0.3 | ||||||||||
| (Castignani et al. 2019) | DES-RG 399 | 0.388 | 3 → 2 | IRAM 30 m | 0.55 | 4.36 | < 0.2 | 9.1 |
 |
9.8 |
| DES-RG 708 at z = 0.6 | ||||||||||
| (Castignani et al. 2019) | DES-RG 708 | 0.606 | 3 → 2 | IRAM 30 m | 0.55 | 4.36 | < 0.6 | 28.2 |
 |
37.0 |
| COSMOS-FRI 16 at z = 0.9 | ||||||||||
| (Castignani et al. 2019) | COSMOS-FRI 16 | 0.969 | 4 → 3 | IRAM 30 m | 0.40 | 4.36 | < 4.3 | 12.3 |
 |
46.2 |
| COSMOS-FRI 31 at z = 0.9 | ||||||||||
| (Castignani et al. 2019) | COSMOS-FRI 31 | 0.912 | 4 → 3 | IRAM 30 m | 0.40 | 4.36 | < 3.6 | 8.7 | < 42 | 33.3 |
| COSMOS-FRI 70 at z = 2.6 | ||||||||||
| (Castignani et al. 2019) | COSMOS-FRI 70 | 2.625 | 7 → 6 | IRAM 30 m | 0.39 | 4.36 | < 1.5 | 22.9 |
 |
298.0 |
| SpARCS J1033+58 at z = 0.43 | ||||||||||
| (This work) | 3C 244.1 | 0.430 | 2 → 1 | IRAM 30 m | 0.80 | 4.36 | < 0.2 | 10.0 | 281 ± 218 | 11.8 |
| SpARCS J1611+55 at z = 0.91 | ||||||||||
| (This work) | SDSS J161112.65+550823.5 | 0.907 | 4 → 3 | IRAM 30 m | 0.40 | 4.36 | < 0.6 | 18.0 | 766 ± 275 | 53.7 |
Notes. For the Cl J1449+0856 BCG the reported SFR is derived from the 870 μm observer frame flux (Coogan et al. 2018); to estimate 
, an excitation ratio r41 = 0.36 is assumed, equal to the mean between the ratios of the two Coogan et al. (2018) sources (ID 6, B1) with both CO(1 → 0) and CO(4 → 3) detections. The reported values for αCO and 
imply a molecular gas mass ∼1010.8 M⊙, while Coogan et al. (2018) find a dynamical mass equal to 1010.3 ± 0.3 M⊙. The two estimates are fairly consistent with each other within the uncertainties. For MRC 1138–262 we report the SFR = 142 M⊙ yr−1 (Emonts et al. 2016), with uncertainties derived assuming maximum and minimum values equal to SFR = 1400 M⊙ yr−1 (Emonts et al. 2013) and SFR = 57 M⊙ yr−1 (Hatch et al. 2008), respectively.
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