Table 1.
IDs, SExtractor segmentation numbers, photometric and spectroscopic redshifts, stellar masses and SFRs of group member galaxies.
CANDELS ID | 3DHST | Seg. | zphot | zspec | log10(M⋆/M⊙, FAST) | SFRIR (M⊙ yr−1) | SFRFAST (M⊙ yr−1) |
---|---|---|---|---|---|---|---|
29816 | 38191 | 92 | 1.64±0.24 | 1.84±0.02 | 10.03![]() |
< 247 | < 17.08 |
30304 | 38274 | 78 | 1.72±0.18 | – | 10.50![]() |
108±32 | < 8.58 |
30147 | 38263 | 90 | 1.68±0.05 | 1.85±0.01 | 10.44![]() |
< 169 | < 0.67 |
29630 | 38497 | 88 | 1.95±0.27 | 1.86±0.01 | 8.80![]() |
< 146 | < 0.44 |
30186 | 38187 | 89 | 1.92±0.10 | 1.850±0.005 | 11.32![]() |
1810±219 | < 168.53 |
30186 | – | 99 | – | – | 10.14![]() |
– | < 2.85 |
30186 | – | 100 | – | – | 9.64![]() |
– | < 0.64 |
30336 | – | 85 | 1.78±0.21 | – | 10.45![]() |
< 262 | < 27.03 |
30144 | 38174 | 94 | 1.52±0.16 | 1.89±0.03 | 10.29![]() |
313±108 | < 7.25 |
29702 | 38356 | 87 | 1.64±0.11 | – | 9.83![]() |
< 276 | < 4.50 |
30329 | 38290 | 79 | 1.95±0.12 | – | 10.76![]() |
68±18 | < 1.15 |
28224 | 38527 | 83 | 1.53±0.23 | – | 8.88![]() |
< 120 | < 1.45 |
– | 38212 | 95 | – | – | 9.25![]() |
– | < 0.24 |
– | – | 96 | – | – | 8.94![]() |
– | < 0.25 |
– | – | 180 | – | – | 9.72![]() |
– | < 1.80 |
– | 38531 | 181 | – | 1.85±0.05 | 8.53![]() |
– | < 0.12 |
Notes. zphot are taken from the Stefanon et al. (2017) catalogue, with errors derived from SED fitting in the FIR catalogue. SFRs derived in the FIR catalogue (SFRIR) and using SED fitting (SFRFAST, this work) are labelled accordingly. Stellar masses are taken from our FAST++ fitting, with the 68% errors shown. Some CANDELS IDs appear several times, associated with different segmentation IDs, derived from the higher-resolution imaging (see also Fig. 2). SFRIR shown in bold indicate that the galaxies are detected at S/N > 5 in the FIR regime, and SFRIR are only shown for those galaxies with S/NFIR > 2.5. 3σ upper limits are shown on SFR values (using the errors on the derived SFR, from the FIR catalogue SED fitting or FAST SED fitting, respectively).
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