Table 2
Previously observed properties of the sample.
| Source | z | F 250 | F 350 | F 500 | F 880 | r half | ΣSFR | f 1.4 GHz | T d | μ | μ L IR |
| (mJy) | (mJy) | (mJy) | (mJy) | (kpc) | (103M⊙ yr-1 kpc-2) | (mJy) | (K) | (1013 L⊙) | |||
|
|
|||||||||||
| G09v1.97 | 3.634 | 260 ± 7 | 321 ± 8 | 269 ± 9 | 85.5 ± 4.0 | 0.85 | 0.91 ± 0.15 | ± 0.15 | 44 ± 1 | 6.9 ± 0.6 | 15.3 ± 4.3 |
| G12v2.43 | 3.127 | 290 ± 7 | 295 ± 8 | 216 ± 9 | 48.6 ± 2.3 | – | – | ± 0.15 | – | – | (8.3 ± 1.7) |
| NCv1.143 | 3.565 | 214 ± 7 | 291 ± 8 | 261 ± 9 | 97.2 ± 6.5 | 0.40 | 2.08 ± 0.77 | 0.61 ± 0.16 | 40 ± 1 | 11.3 ± 1.7 | 12.8 ± 4.3 |
| NAv1.195 | 2.951 | 179 ± 7 | 279 ± 8 | 265 ± 9 | 65.2 ± 2.3 | 1.57 | 0.21 ± 0.04 | ± 0.14 | 36 ± 1 | 4.1 ± 0.3 | 7.4 ± 2.0 |
| NAv1.177 | 2.778 | 264 ± 9 | 310 ± 10 | 261 ± 10 | 50.1 ± 2.1 | – | – | ± 0.15 | – | – | (5.5 ± 1.1) |
| NBv1.78 | 3.111 | 273 ± 7 | 282 ± 8 | 214 ± 9 | 59.2 ± 4.3 | 0.55 | 1.09 ± 1.41 | 0.67 ± 0.20 | 43 ± 1 | 13.0 ± 1.5 | 10.7 ± 3.9 |
|
|
|||||||||||
| G09v1.124-Wa | 2.410 | 242 ± 7 | 293 ± 8 | 231 ± 9 | 50.0 ± 3.5 | – | – | ± 0.15 | 40 ± 1 | 1 | 3.3 ± 0.3 |
| G09v1.124-Ta | – | – | ± 0.15 | 36 ± 1 | 1.5 ± 0.2 | 2.7 ± 0.8 | |||||
| G09v1.40 | 2.089b | 389 ± 7 | 381 ± 8 | 241 ± 9 | 61.4 ± 2.9 | 0.41 | 0.77 ± 0.30 | 0.75 ± 0.15 | 36 ± 1 | 15.3 ± 3.5 | 6.5 ± 2.5 |
| SDP11 | 1.786 | 417 ± 6 | 378 ± 7 | 232 ± 8 | 30.6 ± 2.4 | 0.89 | 0.22 ± 0.08 | 0.66 ± 0.14 | 41 ± 1 | 10.9 ± 1.3 | 6.2 ± 1.9 |
| NCv1.268 | 3.675 | 145 ± 7 | 201 ± 8 | 212 ± 9 | 78.9 ± 4.4 | 0.93 | 0.31 ± 0.14 | 1.10 ± 0.14 | 39 ± 1 | 11.0 ± 1.0 | 9.5 ± 2.7 |
| NAv1.56 | 2.301 | 481 ± 9 | 484 ± 13 | 344 ± 11 | 73.1 ± 2.4 | 1.50 | 0.14 ± 0.08 | 1.12 ± 0.27 | 38 ± 1 | 11.7 ± 0.9 | 11.3 ± 3.1 |
Notes. z is the redshift inferred from previous CO detection quoted by B13 (see the references therein); F250, F350 and F500 are the SPIRE flux densities at 250, 350 and 500 μm, respectively (Pascale et al. 2011); F880 is the SMA flux density at 880 μm; rhalf and ΣSFR are the intrinsic half-light radius at 880 μm and the lensing-corrected surface SFR (star formation rate) density (Sect. 4.2); f1.4 GHz is the 1.4 GHz band flux densities from the VLA FIRST survey; Td is the cold-dust temperature taken from B13 (note that the errors quoted for Td are significantly underestimated since the uncertainties from differential lensing and single-temperature dust SED assumption are not fully considered); μ is the lensing magnification factor from B13, except for G09v1.124 which is adopted from Ivison et al. (2013); μLIR is the apparent total infrared luminosity mostly inferred from B13. The μLIR in brackets are not listed in B13, thus we infer them from single modified black body dust SED fitting using the submm photometry data listed in this table.
The cluster source G09v1.124 includes two main components: G09v1.124-W to the east and G09v1.124-T to the west (Fig. A.3) and the values of these two rows are quoted from Ivison et al. (2013);
our H2O observation gives z = 2.093 for G09v1.40. This value is slightly different from the value of 2.089 quoted by B13 from Lupu et al. (in prep.) obtained by CSO/Z-Spec, but consistent with CO(3–2)observation by Riechers et al. (in prep.).
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