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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).

(a)

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%.

(b)

L is the size of the CO-emitting region.

(c)

Rest-frame infrared luminosity between wavelengths λ = 8–1000 μm.

(d)

Star formation efficiency, defined as LFIR/Mgas.

(e)

Dust temperatures for the extended and clumpy dust component reported by Danielson et al. (2010) for a two-phase model.

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