Table 3
Redshifts, star formation rates and results of the FIR SED fitting of the 870 μm LABOCA sources in the field around MRC1138−256.
| Alias | Member | z opt/NIR | z FIR | SFR Hα | SFR FIR | L FIR | T | β | Template |
| (M⊙ yr-1) | (M⊙ yr-1) | (1012L⊙) | (K) | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
|
|
|||||||||
| DKB01a | YES | 2.84 |
2.3 ± 0.7 | 30 | 1320 | 7.6 | 35 | 1.5 | #13 (DKB13) |
| DKB01b | YES | 2.165 | 2.3 ± 0.7 | 230 | 1090 | 6.3 | 37 | 1.3 | #13 (DKB13) |
| DKB02 | P | 2.12 |
2.7 ± 0.8 | 3080 | 17.9 | 35 | 1.5 | #6 (I22491) | |
| DKB03 | YES | 2.163 | 2.1 ± 0.6 | 290 | 650 | 3.8 | 31 | 1.5 | #10 (DKB03) |
| DKB04 | U | ... | 3.6 ± 1.1 | 1010 | 5.9 | 35 | 1.5 | #14 (DKB14) | |
| DKB05 | U | ... | 2.4 ± 0.7 | 490 | 2.8 | 35 | 1.5 | #10 (DKB03) | |
| DKB06 | NO | 0.028 | 0.8 ± 0.2 | 1 | 0.009 | 22 | 1.9 | #7 (Mrk231) | |
| DKB07 | YES | 2.160 | 2.2 ± 0.6 | 1750 | 10.1 | 56 | 1.0 | #11 (DKB07) | |
| DKB08a | U | 2.2 | 5.6 ± 1.7 | >20⋆ | 1460 | 8.4 | 35 | 1.5 | #8 (QSO1) |
| DKB08b | U | .. | 5.6 ± 1.7 | 1460 | 8.4 | 35 | 1.5 | #8 (QSO1) | |
| DKB09 | U | ... | 3.6 ± 1.1 | † | † | † | † | #11 (DKB07) | |
| DKB10 | U | ... | 3.0 ± 0.9 | 810 | 4.7 | 35 | 1.5 | #12 (DKB12c) | |
| DKB11 | U | ... | 2.6 ± 0.8 | 620 | 3.6 | 35 | 1.5 | #12 (DKB12c) | |
| DKB12a | YES | 2.171 | 2.1 ± 0.6 | 240 | 860 | 5.0 | 35 | 1.8 | #12 (DKB12c) |
| DKB12b | YES | 2.170 | 2.1 ± 0.6 | 160 | 860 | 5.0 | 35 | 1.8 | #12 (DKB12c) |
| DKB12c | YES | 2.164 | 2.1 ± 0.6 | 30 | 850 | 4.9 | 35 | 1.8 | #12 (DKB12c) |
| DKB12d | YES | 2.166 | 2.9 ± 0.9 | 100 | 850 | 4.9 | 35 | 1.8 | #6 (I22491) |
| DKB13 | NO | 1.34 |
1.3 ± 0.4 | 280 | 1.6 | 38 | 1.0 | #13 (DKB13) | |
| DKB14 | NO | 1.37 |
1.3 ± 0.4 | 2020 | 11.7 | 45 | 1.6 | #14 (DKB14) | |
| DKB15 | P | 2.2 | 3.4 ± 1.0 | 90 | 460 | 2.7 | 35 | 1.5 | #11 (DKB07) |
| DKB16 | YES | 2.154 | 1.9 ± 0.6 | 1140 | 830 | 4.8 | 48 | 1.3 | #7 (Mrk231) |
Notes. Column (1): short name of LABOCA source. Column (2): classification on membership of the z ≈ 2.2 protocluster structure. YES = secure member; P = possible member; U = no reliable statement on membership could be made; NO = membership securely excluded. Column (3): spectrosopcic (three digits after the decimal), photometric redshift (two digits after the decimal) and Hα imaging (one digit after the decimal) of the LABOCA counterpart. Column (4): redshift estimate from the FIR SED. Column (5): the star formation rate derived from narrow-band Hα imaging (Koyama et al. 2013a) is based on the NB flux and includes corrections for [NII] contamination and dust extinction following Koyama et al. (2013a). Column (7): FIR luminosity. Column (8): dust temperature. Column (9): spectral index. In order to overcome the well-known T − z degeneracy (e.g., Blain et al. 2002), we fixed the temperature T to 35 K and the spectral index β to 1.5 where no spectroscopic information is available. The same we also do for sources with only 3 detections in the FIR bands. Column (10): template used.
Due to its faintness in the Ks-band no corrections could be applied. Column (6): star formation rate derived from our infrared luminosities estimates and using the conversion from Kennicutt (1998).
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