Table 1
Summary of interferometrically observed COSMOS SMGs besides our work.
| Source | Reference | LABOCA | Redshift | ||||
| source | separation | F 870 μm | spectroscopic | photometric+ | mm-to-radio | ||
| [′′] | [mJy] | ||||||
|
|
|||||||
| AzTEC-1 | (1), (2), (3) | COSLA-60 | 12.6 ± 3.6 | 4.64 |
|
– | |
| AzTEC-2 | (1), (4) | COSLA-4 | 14.4 ± 3.0 | 1.125 | – | – | |
| AzTEC-3 | (1), (5) | – | – | – | 5.299 |
|
– |
| AzTEC-4 | (1) | – | – | – | – |
|
– |
| AzTEC-5 | (1), (6) | – | – | – | 3.971 |
|
– |
| AzTEC-6 | (1) | – | – | – | 0.802 |
|
– |
| AzTEC-7 | (1) | – | – | – | – |
|
– |
| AzTEC-8 | (7), (8) | COSLA-73 | – | 12.3 ± 3.6 | 3.179 |
|
– |
| AzTEC-9 | (7) | COSLA-3 | – | 16.4 ± 3.3 | 1.357 |
|
– |
| AzTEC-10 | (7) | – | – | – | – |
|
– |
| AzTEC-11 | (7) | – | – | – | 1.599 |
|
– |
| AzTEC-11-N | (7) | – | – | – | – |
|
– |
| AzTEC-11-S | (7) | – | – | – | – | – | >2.58 |
| AzTEC-12 | (7) | – | – | – | – |
|
– |
| AzTEC-13 | (7) | COSLA-158 | – | 11.8 ± 3.9 | – | – | >3.59 |
| AzTEC-14-E | (7) | – | – | – | – | – | >3.03 |
| AzTEC-14-W | (7) | – | – | – | – |
|
– |
| AzTEC-15 | (7) | – | – | – | – |
|
– |
| AzTEC-16 | (9) | – | – | – | 1.505 |
|
– |
| J1000+0234 | (10) | – | – | – | 4.542 |
|
– |
| AzTEC/C1 | (11) | COSLA-89 | – | 12.4 ± 3.7 | – | 5.6 ± 1.2 | |
| Cosbo-1* | (12) | COSLA-1 | – | 13.8 ± 1.5 | – | – |
|
| Cosbo-3 | (8), (11) | COSLA-2 | – | 13.1 ± 2.6 | 2.490 |
|
– |
| Cosbo-8 | (11) | – | – | – | – | 3.1 ± 0.5 | – |
| Cosbo-14 | (12) | – | – | – | – | – | – |
Notes.
Photometric redshifts drawn from the total χ2 distribution as described in Sect. 6 and not corrected for any systematic offsets.
Formally this source is not detected in optical, near- and mid-IR maps/catalogs, therefore we here use the mm-to-radio flux based redshift here, which is consistent with the photometric redshift given by Aravena et al. (2010).
References. (1) Younger et al. (2007); (2) Younger et al. (2009); (3) Smolčić et al. (2011); (4) Baloković et al. (in prep.); (5) Capak et al. (2010); Riechers et al. (2010); (6) Karim et al. (in prep.); (7) Younger et al. (2009); (8) Riechers et al. (in prep.); (9) Sheth et al. (in prep.); (10) Capak et al. (2009), Schinnerer et al. (2009); (11) Smolčić et al. (2012); (12) Aravena et al. (2010).
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