Table 4
Summary and comparison of physical properties of SMM J0658 and other highly magnified SMGs.
| Source | SMM J0658 | SMM J16359+6612 | SMM J2135 − 0102 |
| (1) | (2) | (3) | |
|
|
|||
| Redshift | 2.7793 | 2.5174 | 2.3259 |
| Magnification | 80–115 | 45 ± 3.5 | 32.5 ± 4.5 |
| Submm flux density (mJy) | ~0.5 | ~0.8a | ~3 |
| LCO(1 − 0)(108 K km s-1 pc2) | 22.6 ± 3.6 | – | 173 ± 9 |
| LCO(3 − 2)(108 K km s-1 pc2) | 12.7 ± 2.0 | 37 ± 2 | 117.6 ± 0.9 |
| Mgas(109 M⊙) | 1.8 ± 0.3 | 4.5 ± 1.0 | 14 ± 1 |
| Mdyn(109 M⊙) | (13 ± 4)(L/1kpc)b | 15 ± 3 | 40 − 80 |
| LFIR(1012L⊙)c | 0.3 ± 0.03 | 1.6 ± 0.4 | 2.3 ± 0.1 |
| SFR(M⊙ yr-1) | 100–150 | ~500 | 400 ± 20 |
d
|
170 | ~320 | 165 ± 7 |
| Mdust(107 M⊙) |
|
1.9 ± 0.3 | ~15 |
| Tdust(K) | 33 ± 5 | 51 ± 3 | (30;57 ± 3)e |
Notes. All values have been corrected for the individual gravitational magnification factors. (1) This work; (2) Kneib et al. (2004, 2005); (3) Danielson et al. (2010).
Flux density measured at 850 μm; the other two flux densities were measured at 870 μm. For a submm spectral index of ~3 the flux difference between the two wavelengths is less than 3%.
Dust temperatures for the extended and clumpy dust component reported by Danielson et al. (2010) for a two-phase model.
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