Table 2: Physical properties of the sample inferred from their SED.
Name $\log M_*$ (BC03) $\log M_*$ (M05) MB U-V SFR E(B-V)* Age
  $[M_{\odot}]$ $[M_{\odot}]$ [mag] [mag] $[M_{\odot}~\rm yr^{-1}]$ [mag] [Gyr]
CDFa-C9 10.18 $\rm ^{+0.40}_{-0.08}$ 10.13 $\rm ^{+0.30}_{-0.05}$ -22.36 -0.24 265 0.25 $\rm ^{+0.05}_{-0.10}$ 0.06 $\rm ^{+0.25}_{-0.01}$
CDFS-4414 10.57 $\rm ^{+0.19}_{-0.22}$ 10.48 $\rm ^{+0.06}_{-0.23}$ -22.47 -0.02 113 0.20 $\rm ^{+0.05}_{-0.10}$ 0.39 $\rm ^{+0.60}_{-0.29}$
CDFS-4417 10.29 $\rm ^{+0.37}_{-0.11}$ 10.32 $\rm ^{+0.29}_{-0.10}$ -22.79 -0.35 438 0.25 $\rm ^{+0.05}_{-0.10}$ 0.05 $\rm ^{+0.23}_{-9.99}$
CDFS-6664 9.49 $\rm ^{+0.10}_{-0.23}$ 9.30 $\rm ^{+0.22}_{-0.08}$ -20.93 -0.70 35 0.10 $\rm ^{+0.10}_{-0.04}$ 0.10 $\rm ^{+0.09}_{-0.05}$
CDFS-16767 10.05 $\rm ^{+0.10}_{-0.16}$ 9.90 $\rm ^{+0.13}_{-0.13}$ -21.90 -0.49 84 0.15 $\rm ^{+0.05}_{-0.05}$ 0.12 $\rm ^{+0.07}_{-0.07}$
CDFS-11991 9.69 $\rm ^{+0.12}_{-0.15}$ 9.64 $\rm ^{+0.18}_{-0.08}$ -21.64 -0.46 55 0.10 $\rm ^{+0.05}_{-0.04}$ 0.10 $\rm ^{+0.09}_{-0.05}$
CDFS-2528 9.76 $\rm ^{+0.09}_{-0.07}$ 9.71 $\rm ^{+0.16}_{-0.00}$ -21.57 -0.33 101 0.20 $\rm ^{+0.05}_{-0.05}$ 0.06 $\rm ^{+0.03}_{-0.01}$
SSA22a-M38 11.01 $\rm ^{+0.18}_{-0.41}$ 10.71 $\rm ^{+0.19}_{-0.40}$ -22.99 0.22 115 0.20 $\rm ^{+0.05}_{-0.20}$ 0.63 $\rm ^{+0.95}_{-0.45}$
SSA22a-aug16M16 10.29 $\rm ^{+0.20}_{-0.21}$ 10.15 $\rm ^{+0.11}_{-0.28}$ -22.32 -0.23 42 0.06 $\rm ^{+0.04}_{-0.06}$ 0.39 $\rm ^{+0.39}_{-0.23}$
The following quantities are reported in each column: Col. 1, object name; Col. 2, stellar mass inferred by using the galaxy templates of BC03; Col. 3, stellar mass inferred by using the galaxy templates of M05; Col. 4, absolute B magnitude; Col. 5, rest-frame U-V color; Col. 6, star formation rate (by using BC03); Col. 7, dust reddening affecting the stellar light, by using the attenuation curve of Calzetti et al. (2000); Col. 8, age of the stellar population.


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