Table 1
Typical uncertainties in the determination of redshifts, extinctions, luminosity-weighted ages, luminosity-weighted metallicities, and stellar masses, expected from running our code on ALHAMBRA red sequence galaxies at different redshift bins and for different S/N (10, 20, and 50).
| Parameters | 0.0 ≤ z ≤ 0.2 | 0.2 ≤ z ≤ 0.4 | 0.4 ≤ z ≤ 0.6 | 0.6 ≤ z ≤ 0.8 | 0.8 ≤ z ≤ 1.0 |
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| S/N = 10 | |||||
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| z phot | 0.01 ± 0.03 | 0.00 ± 0.04 | 0.00 ± 0.03 | 0.00 ± 0.02 | 0.00 ± 0.02 |
| A V | 0.10 ± 0.22 | 0.08 ± 0.20 | 0.04 ± 0.17 | 0.04 ± 0.15 | 0.02 ± 0.14 |
| log 10 AgeL [yr] | −0.01 ± 0.19 | −0.03 ± 0.17 | −0.03 ± 0.14 | 0.00 ± 0.11 | 0.03 ± 0.10 |
| [Fe/H] L | −0.09 ± 0.29 | 0.01 ± 0.30 | 0.03 ± 0.26 | 0.00 ± 0.23 | 0.03 ± 0.22 |
| log 10M⋆ [M⊙] | 0.10 ± 0.28 | 0.02 ± 0.12 | 0.01 ± 0.10 | 0.01 ± 0.08 | −0.01 ± 0.06 |
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| S/N = 20 | |||||
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| z phot | 0.00 ± 0.01 | 0.00 ± 0.01 | 0.00 ± 0.01 | 0.00 ± 0.01 | 0.00 ± 0.01 |
| A V | 0.06 ± 0.15 | 0.04 ± 0.13 | 0.01 ± 0.10 | 0.02 ± 0.09 | 0.00 ± 0.08 |
| log 10 AgeL [yr] | −0.03 ± 0.14 | −0.03 ± 0.13 | −0.01 ± 0.11 | 0.00 ± 0.09 | 0.01 ± 0.07 |
| [Fe/H] L | −0.06 ± 0.20 | −0.03 ± 0.19 | −0.01 ± 0.16 | −0.01 ± 0.14 | 0.00 ± 0.12 |
| log 10M⋆ [M⊙] | 0.02 ± 0.15 | 0.01 ± 0.09 | 0.00 ± 0.07 | 0.00 ± 0.06 | −0.01 ± 0.05 |
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| S/N = 50 | |||||
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| z phot | 0.00 ± 0.00 | 0.00 ± 0.00 | 0.00 ± 0.00 | 0.00 ± 0.00 | 0.00 ± 0.00 |
| A V | 0.01 ± 0.08 | 0.00 ± 0.06 | 0.00 ± 0.05 | 0.00 ± 0.03 | 0.00 ± 0.02 |
| log 10 AgeL [yr] | −0.02 ± 0.11 | −0.02 ± 0.09 | 0.00 ± 0.08 | 0.00 ± 0.06 | 0.00 ± 0.05 |
| [Fe/H] L | −0.03 ± 0.08 | −0.02 ± 0.08 | −0.02 ± 0.07 | −0.02 ± 0.06 | −0.01 ± 0.05 |
| log 10M⋆ [M⊙] | 0.00 ± 0.08 | 0.01 ± 0.06 | 0.00 ± 0.05 | 0.00 ± 0.04 | 0.00 ± 0.03 |
Notes. The random errors in the parameters are given as the mean and rms of the best Gaussian function that reproduces the distribution of the differences between the input and output parameter values, as illustrated in the right panels of Fig. 8.
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