Table 2
Submillimeter and infrared properties of the lensed ultra-luminous galaxies.
| Source ID | F250 | F350 | F500 | μ LIR | μ | LIR |
| (mJy) | (mJy) | (mJy) | (1013 L⊙) | (1012 L⊙) | ||
|
|
||||||
| SDP.81 | 129 ± 20 | 182 ± 28 | 166 ± 27 | 5.8 | 9.5 ± 0.8 | 6.1 |
| NA.v1.144 | 295 ± 45 | 294 ± 45 | 191 ± 31 | 5.7 | 5.3 ± 2.9 | 11 |
| SDP.9 | 485 ± 73 | 323 ± 49 | 175 ± 28 | 4.4 | 8.5 ± 1.8 | 5.2 |
| NB.v1.78 | 273 ± 42 | 282 ± 43 | 214 ± 33 | 11 | 10.5 ± 1.4 | 10 |
| G12.v2.30 | 323 ± 49 | 378 ± 57 | 298 ± 45 | 15.7 | 9.6 ± 0.9 | 16 |
| G15.v2.779 | 115 ± 19 | 192 ± 30 | 204 ± 32 | 8.5 | 4.1 ± 0.2 | 21 |
| SDP.17b | 328 ± 50 | 308 ± 47 | 220 ± 34 | 6.9 | 4.3 ± 1.2 | 16 |
Notes.F250, F350, and F500 are the SPIRE flux densities at 250, 350, and 500 μm; μLIR is the apparent total infrared luminosity (8−1000 μm); μ is the adopted lensing magnification factor derived from lensing modeling of 880 μm continuum, mostly from Bussmann et al. (in prep.; see text Sect. 3 for details); LIR is the intrinsic infrared luminosity, derived from the literature (Harris et al. 2012; Lupu et al. 2012; Fu et al. 2012; Bussmann et al. 2012) except for NB.v1.78, for which an approximate value is inferred from scaling the value of G12.v2.30 with the ratio of the 350 μm flux densities.
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