Table 2
Results from the SED fitting.
| ID | EWH α | χ2 | Agey | Zy | AV.y | My | Mo | log(NO⋆) | R | σO⋆ |
|---|---|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| 20002280 | 61 | 1.09 |  |
 |
 |
 |
 |
3.9 | 2.29 | 450 |
| 10000098 | 23 | 0.85 |  |
 |
 |
 |
 |
2.4 | 0.95 | 95 |
| 10000145 | 42 | 0.61 |  |
 |
 |
 |
 |
3.5 | 1.44 | 453 |
| 10000515 | 38 | 2.49 |  |
 |
 |
 |
 |
3.7 | 2.59 | 222 |
| 10000777 | 34 | 1.09 |  |
 |
 |
 |
 |
4.5 | 1.85 | 2809 |
| ...... |
Notes. Fixed values for the old population: age (2 Gyr), metallicity (Z = 0.004) and extinction (E(B-V) = 0.08). The complete table is available at the CDS; only the first rows are shown here as guidance. Columns: (1) SHARDS ID. (2) Photometrically derived Hα EW, in Ångstroms. (3) Reducedchi-squared of the best-fit. (4) Age of the young stellar population, in Myr. (5) Metallicity of the young stellar population. (6) Extinction (AV) of the young stellar population, in magnitudes. (7) Mass of the young stellar population, in log(M⊙). (8) Mass of the old stellar population, in log(M⊙) (9) Number of O stars per galaxy (logarithm). (10) Physical effective radius of the galaxy in kpc, based on F160W data (Skelton et al. 2014). (11) Surface density of O stars, in N⋆ kpc−2.
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