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Table 1

Comparison of stellar masses and specific star formation rates of SMGs calculated using various methods, stellar population models and star formation histories.

Fita SSPb SFHc Mean M∗ Median M∗ Mean SSFR Median SSFR AgeYd AgeOe FracOf
(log M⊙) (log M⊙) (Gyr-1) (Gyr-1) (Gyr) (Gyr)
M10 Padova cont+burst 11.32 ± 0.05 2.86 ± 0.43 0.050 1.856 0.84
H11 BC03 1burst/const 10.87 ± 0.06 9.71 ± 1.99 0.820 ···  ··· 
H11 M05 1burst/const 10.71 ± 0.06 12.96 ± 2.17 0.860 ···  ··· 
C10 BC03 double 11.44 ± 0.08 10.87 ± 8.68 0.191 1.332 0.87
C10 BC03 tau 11.16 ± 0.10 17.36 ± 11.98 1.178 ···  ··· 
C10 BC03 1burst 11.06 ± 0.10 14.88 ± 8.69 0.246 ···  ··· 
C10 M05 double 11.73 ± 0.06 1.25 ± 0.19 0.075 1.777 0.66
C10 M05 tau 10.46 ± 0.13 167.34 ± 47.42 0.767 ···  ··· 
C10 M05 1burst 11.24 ± 0.07 8.43 ± 4.57 0.198 ···  ··· 

Notes. The Chabrier (2003) IMF is assumed. Errors are standard deviations for the means and bootstrap 68% ranges for medians.

(a)

SED fitting method presented in M10 (Michałowski et al. 2010a), H11 (Hainline et al. 2011), or C10 (Cirasuolo et al. 2010).

(b)

Single stellar population models being either Padova tracks, BC03 (Bruzual & Charlot 2003) or M05 (Maraston 2005).

(c)

Assumed star formation history being either a continous SFH with a burst (cont+burst), an average of the single burst and constant (1 burst/const), double burst (double), single burst (1 burst), or exponentially declining (tau).

(d)

Mean age of the younger stellar component.

(e)

Mean age of the older stellar component.

(f)

Mean fractional contribution to the total stellar mass of the older component.

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