Table 1.
Properties of SHARDS20018464 and of its two components.
| ID | RA | Dec | L | Lλ | EW (Lyα) | EW0(Lyα) | Fν |
|---|---|---|---|---|---|---|---|
| [erg s−1] | [erg s−1 Å−1] | Å | Å | [AB mag] | |||
| SExtractor global properties (galaxy+blob) | |||||||
| SHARDS20018464 | 189.28 | 62.23 | 3.5 × 1042 | – | – | – | 25.35 |
| First method: excess of light in the SB profile after removing a Sérsic profile | |||||||
| blob (Lyα) | – | – | 1.04 × 1043 | – | – | – | 24.35 |
| gal (continuum) | – | – | 2.87 × 1042 | 2.08 × 1040 | 500 | 111 | 25.75 |
| tot | – | – | 1.33 × 1043 | – | – | – | 24.09 |
| Second method: double Gaussian fit | |||||||
| blob (Lyα) | – | – | 2.34 × 1042 | – | – | – | 25.97 |
| gal (continuum) | – | – | 2.40 × 1042 | 1.74 × 1040 | 134 | 30 | 25.94 |
| tot | – | – | 3.34 × 1042 | – | – | – | 25.59 |
| Third method: excess of light in the SB profile | |||||||
| blob (Lyα) | – | – | 1.65 × 1042 | – | – | – | 26.35 |
| gal (continuum) | – | – | 6.26 × 1042 | 4.53 × 1040 | 36 | 8 | 24.90 |
| tot | – | – | 8.17 × 1042 | – | – | – | 24.61 |
| UV continuum estimated using the F606W HST/ACS filter | |||||||
| HST/ACS F606W | 189.28 | 62.23 | 1.08 × 1043 | 5.78 × 1039 | – | – | 26.99 |
| Combined SHARDS F551W17 and HST/ACS F606W filters | |||||||
| Lyα | – | – | 2.7 ×1042 | 5.78 × 1039 | 467 | 104 | – |
Notes. Top row: Properties of the SHARDS20018464 object (galaxy+blob) as obtained with SExtractor on the SHARDS F551W17 filter. The magnitude is calibrated using the zero point given by the SHARDS team. The values per wavelength units correspond to the effective centre wavelength of the filter. Rows 2–4: our main method, based on modelling the galaxy with a Sérsic profile and then computing the area of the blob as the difference between the total one and the area of the modelled galaxy. Rows 5–7: Values from the areas of the Gaussians. The total one is the area of the double Gaussian, the other are the individual ones. Rows 8-10: Values from the ellipse fitting method assuming that the galaxy is the dominant component. The total flux iso is the same as in the previous method, we computed those of the blob and the galaxy by applying the fraction of the area that corresponds to each of them (e.g. the blob is about 65% of the area, so 65% of the flux iso). The last two lines show the photometry with the broad band HST/ACS F606W filter and the values of L(Lyα) and EW(Lyα) derived combining the SHARDS narrow band filter and the HST/ACS broadband one. The L(Lyα) value is computed by subtracting the proportional continuum contribution of the HST/ACS F606W filter from the total luminosity in the SHARDS filter.
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