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Table A.1.

Properties of distant z ≳ 0.2 cluster galaxies 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)
Abell 2192 at z = 0.188
(Cybulski et al. 2016) J162523.6+422740 0.187 1 → 0 LMT 1.00 4.60 1.8 17 1.9
J162644.6+422530 0.189 1 → 0 LMT 1.00 4.60 6.0 23 3.7
J162508.6+423400 0.190 1 → 0 LMT 1.00 4.60 10.1 14 4.9
Abell 963 at z = 0.206
(Cybulski et al. 2016) J101727.7+384628 0.201 1 → 0 LMT 1.00 4.60 7.2 8 4.3
J101540.2+384913 0.204 1 → 0 LMT 1.00 4.60 5.1 3 3.6
J101730.0+385831 0.204 1 → 0 LMT 1.00 4.60 3.0 24 2.7
J101611.1+384924 0.207 1 → 0 LMT 1.00 4.60 11.8 12 5.7
J101618.0+390613 0.208 1 → 0 LMT 1.00 4.60 6.4 42 4.1
Cl 0024+16 at z = 0.395
(Geach et al. 2011) MIPS J002652.5 0.380 1 → 0 PdBI 1.00 4.60 62 ± 19 9.8
MIPS J002703.6 0.396 1 → 0 PdBI 1.00 4.60 42 ± 12 9.8
MIPS J002715.0 0.381 1 → 0 PdBI 1.00 4.60 35 ± 11 10.7
MIPS J002621.7 0.380 1 → 0 PdBI 1.00 4.60 56 ± 16 10.8
MIPS J002721.0 0.396 1 → 0 PdBI 1.00 4.60 59 ± 16 10.5
Cl 1416+4446 at z = 0.397
(Jablonka et al. 2013) GAL1416+4446 0.396 1 → 0 PdBI 1.00 – 28 14.4
Cl 0926+1242 at z = 0.489
(Jablonka et al. 2013) GAL0926+1242-A 0.489 2 → 1 PdBI 1.00 – 17 14.1
GAL0926+1242-B 0.489 2 → 1 PdBI 1.00 – 8 1.9
ISCS J1432.4+3332 at z = 1.1
(Wagg et al. 2012) SST24 J143235.8+333632 1.115 2 → 1 PdBI 1.00 0.80 < 150 47.7
ISCS J1426.5+3339 at z = 1.2
(Castignani et al. 2018) J142626.1+333827/6 1.163 2 → 1 NOEMA 1.00 4.36 38.8
XMMXCS J2215.9-1738 at z = 1.46
(Hayashi et al. 2018) ALMA.01 1.466 2 → 1 ALMA 0.83 4.36 65.3
ALMA.02 1.450 2 → 1 ALMA 0.83 5.03 34.4
ALMA.03 1.453 2 → 1 ALMA 0.83 4.18 81.2
ALMA.04 1.466 2 → 1 ALMA 0.83 4.92 38.6
ALMA.05 1.467 2 → 1 ALMA 0.83 5.50 26.4
ALMA.06 1.467 2 → 1 ALMA 0.83 4.16 86.5
ALMA.07 1.452 2 → 1 ALMA 0.83 4.35 64.4
ALMA.08 1.457 2 → 1 ALMA 0.83 4.58 50.5
ALMA.09 1.468 2 → 1 ALMA 0.83 4.21 79.8
ALMA.10 1.454 2 → 1 ALMA 0.83 4.88 38.7
ALMA.11 1.451 2 → 1 ALMA 0.83 5.78 22.1
ALMA.12 1.445 2 → 1 ALMA 0.83 6.09 19.0
ALMA.13 1.471 2 → 1 ALMA 0.83 4.56 53.0
ALMA.14 1.451 2 → 1 ALMA 0.83 4.29 69.9
ALMA.15 1.465 2 → 1 ALMA 0.83 4.98 36.7
ALMA.16 1.465 2 → 1 ALMA 0.83 5.15 32.7
ALMA.17 1.460 2 → 1 ALMA 0.83 5.41 27.5
PLCK G073.4-57.5 at z = 1.5
(Kneissl et al. 2019) 3 1.543 5 → 4 ALMA 0.32 4.36, 0.80 41.3
8 1.545 5 → 4 ALMA 0.32 4.36, 0.80 90.2
COSMOS cluster candidate at z = 1.55
(Aravena et al. 2012) 51613 1.517 1 → 0 JVLA 1.00 3.60 114 ± 17 44.8
51858 1.556 1 → 0 JVLA 1.00 3.60 190 ± 28 57.1
SpARCS J022546-035517 at z = 1.59
(Noble et al. 2019) J0225-371 1.599 2 → 1 ALMA 0.77 4.36 173 ± 76 61.4
J0225-460 1.600 2 → 1 ALMA 0.77 4.36 116 ± 60 80.2
J0225-281 1.611 2 → 1 ALMA 0.77 4.36 120 ± 50 55.5
J0225-541 1.611 2 → 1 ALMA 0.77 4.36 82 ± 30 64.1
J0225-429 1.602 2 → 1 ALMA 0.77 4.36 178 ± 83 11.2
J0225-407 1.599 2 → 1 ALMA 0.77 4.36 84 ± 28 12.5
J0225-324 1.600 2 → 1 ALMA 0.77 4.36 48 ± 27 3.1
J0225-303 1.596 2 → 1 ALMA 0.77 4.36 3 ± 3 47.2
XMM-LSS J02182-05102 at z = 1.62
(Rudnick et al. 2017) 30169 1.629 1 → 0 ALMA 1.00 4.36 127.1
30545 1.624 1 → 0 ALMA 1.00 4.36 110.7
SpARCS J033057-284300 at z = 1.63
(Noble et al. 2017) J0330-57 1.613 2 → 1 ALMA 0.77 4.36 36 ± 21 38.9
SpARCS J022426-032330 at z = 1.63
(Noble et al. 2017) J0224-3656 1.626 2 → 1 ALMA 0.77 4.36 43 ± 20 87.8
J0224-159 1.635 2 → 1 ALMA 0.77 4.36 217 ± 82 60.3
J0224-3680/3624 1.626 2 → 1 ALMA 0.77 4.36 68 ± 24 82.0
J0224-396/424 1.634 2 → 1 ALMA 0.77 4.36 166 ± 60 125.4
Cl J1449+0856 at z = 1.99
(Coogan et al. 2018) 13 1.994 4 → 3 ALMA/JVLA 0.36 4.50 38 ± 11 45.7
6 1.983 1 → 0 ALMA/JVLA 1.00 4.20 118 ± 12 69.7
N7 1.996 4 → 3 ALMA/JVLA 0.36 4.20 < 26 23.5
B1 1.988 1 → 0 ALMA/JVLA 1.00 3.90 57 ± 12 83.0
3 1.990 4 → 3 ALMA/JVLA 0.36 4.70 < 23 35.3
S7 1.982 4 → 3 ALMA/JVLA 0.36 – < 26 47.0
Spider Web proto-cluster at z = 2.16
(Tadaki et al. 2019) 1138.42 2.163 3 → 2 ALMA 0.56 10.81 41 ± 12 15.9
1138.48 2.157 3 → 2 ALMA 0.56 5.55 144 ± 66 69.4
1138.54 2.148 3 → 2 ALMA 0.56 4.41 466 ± 214 172.1
1138.56 2.144 3 → 2 ALMA 0.56 9.64 36 ± 11 18.9
USS 1558 003 at z = 2.53
(Tadaki et al. 2019) 1158.43 2.528 3 → 2 ALMA 0.56 6.59 66 ± 21 175.0
1158.54 2.515 3 → 2 ALMA 0.56 12.80 67 ± 20 48.6
1158.59 2.513 3 → 2 ALMA 0.56 8.69 88 ± 26 92.6
1158.64 2.529 3 → 2 ALMA 0.56 27.15 50 ± 15 19.7
1158.73 2.526 3 → 2 ALMA 0.56 13.22 106 ± 31 47.1
1158.137 2.525 3 → 2 ALMA 0.56 10.70 98 ± 29 64.5
HELAISS02 at z = 2.17
(Gómez-Guijarro et al. 2019) S0 2.173 3 → 2 ALMA 0.69 3.50 760 ± 120 52.0
S1 2.164 3 → 2 ALMA 0.69 9.70 269 ± 37 141.4
S2 2.169 3 → 2 ALMA 0.69 5.60 302 ± 49 171.3
S3 2.174 3 → 2 ALMA 0.69 6.70 200 ± 32 27.8
HXMM20 at z = 2.6
(Gómez-Guijarro et al. 2019) S0 2.602 1 → 0 VLA 1.00 2.90 661 ± 91 22.9
S1 2.598 1 → 0 VLA 1.00 3.70 380 ± 44 33.1
S2 2.602 1 → 0 VLA 1.00 2.40 347 ± 48 29.2
S4 2.597 1 → 0 VLA 1.00 0.80 100 ± 14 65.7
HATLAS J084933+021443 at z = 2.41
(Ivison et al. 2013) HATLAS J084933 W 2.407 1 → 0 JVLA 1.00 0.80 3400 279.4
HATLAS J084933 T 2.409 1 → 0 JVLA 1.00 0.80 1500 146.4
HATLAS J084933 M 2.418 1 → 0 JVLA 1.00 0.80 1.0 800 25.4
HATLAS J084933 C 2.414 1 → 0 JVLA 1.00 0.80 640 47.5
4C 23.56 proto-cluster at z = 2.49
(Lee et al. 2017) HAE3 2.486 3 → 2 ALMA 0.53 4.71 176 ± 78 182.3
HAE4 2.478 3 → 2 ALMA 0.53 4.41 414 ± 175 248.9
HAE5 2.487 3 → 2 ALMA 0.53 5.48 374 ± 140 102.7
HAE8 2.486 3 → 2 ALMA 0.53 5.19 156 ± 63 123.7
HAE9 2.486 3 → 2 ALMA 0.53 5.35 90 ± 40 111.5
HAE10 2.486 3 → 2 ALMA 0.53 5.72 115 ± 47 89.6
HAE16 2.483 3 → 2 ALMA 0.53 5.94 76 ± 32 80.0
CLJ001 at z = 2.51
(Wang et al. 2018) 01 2.503 1 → 0 JVLA 1.00 4.06 282.4
02 2.507 1 → 0 JVLA 1.00 4.06 278.0
03 2.514 1 → 0 JVLA 1.00 4.08 189.8
04 2.501 1 → 0 JVLA 1.00 4.08 167.0
05 2.508 1 → 0 JVLA 1.00 4.08 159.0
06 2.494 1 → 0 JVLA 1.00 4.09 132.6
07 2.505 1 → 0 JVLA 1.00 4.09 126.4
08 2.513 1 → 0 JVLA 1.00 4.10 112.3
09 2.500 1 → 0 JVLA 1.00 4.10 106.0
10 2.506 1 → 0 JVLA 1.00 4.10 106.2
11 2.506 1 → 0 JVLA 1.00 4.10 94.0
12 2.515 1 → 0 JVLA 1.00 4.11 85.0
13 2.505 1 → 0 JVLA 1.00 4.11 84.6
14 2.515 1 → 0 JVLA 1.00 4.12 67.7
SSA22 at z = 3.09
(Bothwell et al. 2013,
Umehata et al. 2015) J221735.15+001537.3 3.096 3 → 2 PdBI 0.52 1.00 3.2 78.0
GN20 at z = 4.05
(Carilli et al. 2010; Tan et al. 2014) GN20 4.055 1 → 0 VLA 1.00 1.30 11.0 1860 ± 90 250.8
GN20.2a 4.051 2 → 1 EVLA 0.84 2.40 3.8 800 ± 70 108.6
GN20.2b 4.056 2 → 1 EVLA 0.84 2.80 11.0 690 ± 100 250.8
HDF850.1 proto-cluster at z = 5.2
(Walter et al. 2012,
Serjeant & Marchetti 2014) HDF850.1 5.183 2 → 1 JVLA 0.95 0.80 850 ± 255 339.2
AzTEC-3 proto-cluster at z = 5.3
(Riechers et al. 2010) AzTEC-3 5.298 2 → 1 EVLA 0.88 0.80 1800 43.8

Notes. Cybulski et al. (2016) report infrared luminosities for their z ∼ 0.2 cluster galaxies, which we have converted into SFR estimates using the Kennicutt (1998) relation. Jablonka et al. (2013) did not assume any value of αCO; these sources are flagged with “–” in the αCO column. In our previous work (Castignani et al. 2018) we detected in CO(2 → 1) two unresolved cluster galaxies, with the same redshift and M⋆ (Zeimann et al. 2013), that we show in the table. Consistently with Castignani et al. (2018) we also report and the SFR derived from the 24 μm observer frame flux, for each of two galaxies, assuming that they equally contribute to the observed (unresolved) emission. Consistently with the order of preference adopted by Hayashi et al. (2018), we report the SFR estimated using both UV and 24 μm observer frame emission, when available (i.e., for the sources with ID ALMA.01, 06, 08, 10, 12, 13, and 15). We report the SFR estimated from the mid-IR to optical SED for the remaining galaxies with ID: ALMA.02, 03, 04, 05, 07, 09, 11, 14, 16, and 17). Kneissl et al. (2019) report gas masses assuming two separate values of αCO, which are listed in this Table. For the Aravena et al. (2012) sources the reported SFRs are the average between those derived from infrared luminosity and from SED fitting. For the Coogan et al. (2018) Cl J1449+0856 galaxies with M⋆ estimates, reported in this table, we list the SFRs derived from the 870 μm observer frame flux. In the cases where the sources are not detected in CO(1 → 0), we have used the CO(4 → 3) detections to estimate , by assuming an excitation ratio r41 = 0.36, equal to the mean between the ratios of the two sources (ID 6, B1) with both CO(1 → 0) and CO(4 → 3) detections. Coogan et al. (2018) did not report any value of αCO for their source S7; this source is flagged with “–” in the αCO column. Wang et al. (2018) report infrared luminosities for their z ∼ 2.5 cluster galaxies, which we have converted into SFR estimates using the Kennicutt (1998) relation.

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