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Table 4

Best fit SED parameters, model A.

Candidate Quality Age (Gyr) Low High E(B−V) Low High Mass (109M⊙) Low High d.p. R-1
NB392_6-1 N/N/I 0.14 0.27 < 0.45 0.00 0.20 3.1 3.7 0.18 12 0.004
NB392_6-2 S/I/I 0.05 0.12 0.35 0.38 9.9 13.6 0.75 12 0.008
NB401_6-1 N/B/B 0.60 2.99 < 0.28 0.00 0.12 13.4 18.1 0.33 10 0.008
NB401_6-2 N/N/I 0.04 0.12 < 0.28 0.00 0.12 0.8 1.8 2.15 6 0.002
NB401_6-3 N/I/I 0.40 2.99 < 0.36 0.00 0.18 5.3 7.7 0.62 11 <0.001
NB401_6-4 N/I/I 0.05 0.13 < 0.33 0.00 0.16 2.7 4.2 2.03 10 0.048
NB401_6-5 N/B/B 0.58 2.99 < 0.35 0.00 0.15 8.1 10.3 1.16 12 0.002
NB401_6-6 S/I/I 0.72 2.99 0.21 0.26 10.7 15.0 1.39 12 0.002
NB401_6-7 N/N/I 0.00 2.99 < 0.23 0.00 0.11 0.19 1.05 0.76 6 0.006
NB401_6-8 N/B/B 0.17 0.48 < 0.20 0.00 0.11 1.1 1.8 0.22 8 0.005
NB401_6-9 N/I/I 0.16 0.29 < 0.33 0.00 0.14 2.7 3.2 0.66 11 0.128
NB401_6-10 N/B/I 0.22 0.33 0.21 0.24 14.3 16.4 0.37 12 0.003
NB401_6-11 N/N/I 0.05 0.15 0.19 0.21 7.6 15.6 1.96 6 0.018
NB401_6-12 N/N/B 0.04 0.13 0.24 0.27 4.1 9.1 1.18 6 0.009
NB401_6-13 N/B/B 0.02 0.07 0.19 0.22 0.6 1.2 0.32 8 0.086
NB401_6-14 N/I/I 0.07 0.10 0.38 0.40 20.1 23.9 6.21 12 0.002
NB401_6-15 S/I/I 0.50 2.99 < 0.33 0.00 0.14 6.4 8.7 1.13 9 0.002
NB401_6-16 N/N/B 0.07 0.17 < 0.26 0.00 0.11 0.9 1.5 1.52 8 0.004
NB401_6-17 N/B/B 0.55 2.99 < 0.26 0.00 0.12 4.0 5.7 0.54 10 0.002
NB401_6-18 N/N/I 0.04 2.99 0.29 0.34 5.7 20.6 1.46 6 0.007
NB401_6-19 S/B/B 0.16 0.22 0.33 0.37 39.2 43.3 0.54 12 0.003
NB401_6-20 N/B/B 0.04 0.10 0.33 0.36 3.0 4.7 0.82 11 <0.001
NB401_6-21 N/N/B 0.02 0.14 < 0.39 0.00 0.16 0.8 2.6 1.30 6 0.056
NB406_6-1 N/I/I 0.32 0.58 < 0.19 0.00 0.08 1.9 2.5 1.29 11 0.004
NB412_18-1 S/I/I 0.19 0.31 0.24 0.28 20.9 23.7 0.30 10 0.015

Notes. Derived SED properties for model A. For a detailed description on the setup of the SED fit, see the text. The Quality column lists: spectroscopically matching LAEs at the correct redshift according to the Barger et al. (2008) or Adams et al. (2011) spectroscopic catalogues (S or N for Spectrum or No spectrum)/Possible confusion from HST imaging (B or I or N for Blended or Isolated or No data)/Possible confusion from ground-based imaging (B or I for Blended or Isolated). Mass here corresponds to the total mass that has gone into stars (i.e. the integral of the star formation rate over the age of galaxy). The R-1 value shows the Gelman & Rubin (1992)R statistic. The best fit values and their upper and lower uncertainties correspond to the least-squares values with 68% confidence intervals. If only an upper or lower limit is listed, this corresponds to the 68% limit. The two columns following each parameter give the 68% lower and upper limits when marginalized over all parameters. represents the χ2 of the best fit model, divided by the degrees of freedom, which is the number of data points (d.p.) minus the number of parameters fitted.

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