Table 1
Photometric observations of the GRB 130603B afterglow (host subtracted).
| t − t0 (days) | Telescope/instrument | Band | Exposure (s) | AB magnitude | |
|
|
|||||
| 0.244 | NOT/MOSCA | r | 5 × 360 | 21.15 ± 0.02 | |
| 0.254 | WHT/ACAM | z | 3 × 300 | 20.39 ± 0.06 | |
| 0.274 | WHT/ACAM | i | 3 × 300 | 20.86 ± 0.06 | |
| 0.281 | 1.23m CAHA | V | 6 × 300 | 21.60 ± 0.10 | |
| 0.290 | GTC/OSIRIS | r | 30 | 21.30 ± 0.02 | |
| 0.294 | WHT/ACAM | g | 3 × 300 | 21.90 ± 0.06 | |
| 0.329 | VLT/FORS2 | V | 60 | 21.47 ± 0.02 | |
| 0.599 | Gemini-N/GMOS-N | z | 5 × 100 | 21.94 ± 0.03 | |
| 0.603 | UKIRT | K | 70 × 10 | 21.06 ± 0.11 | |
| 0.607 | Gemini-N/GMOS-N | i | 5 × 100 | 22.34 ± 0.03 | |
| 0.614 | UKIRT | J | 70 × 10 | 21.48 ± 0.14 | |
| 0.615 | Gemini-N/GMOS-N | r | 5 × 100 | 22.83 ± 0.03 | |
| 0.623 | Gemini-N/GMOS-N | g | 5 × 100 | 23.47 ± 0.04 | |
| 1.59 | Gemini-N/GMOS-N | g | 5 × 120 | >25.7 | |
| 1.60 | Gemini-N/GMOS-N | r | 5 × 120 | 25.6 ± 0.3 | |
| 1.61 | UKIRT | J | 140 × 10 | >22.5 | |
| 1.61 | Gemini-N/GMOS-N | i | 5 × 120 | >24.7 | |
| 1.62 | Gemini-N/GMOS-N | z | 5 × 120 | >23.9 | |
| 2.32 | VLT/HAWK-I | J | 22 × 60 | >24.3 | |
| 3.26 | GTC/OSIRIS | r | 3 × 200 | >25.1 | |
| 4.26 | GTC/OSIRIS | r | 3 × 200 | >25.5 | |
| 7.30 | VLT/HAWK-I | J | 22 ×60 | >23.6 | |
| 8.23 | TNG/DOLoRes | r | 4 × 300 | >23.75 | |
| 8.25 | TNG/DOLoRes | i | 4 × 300 | >24.61 | |
| 21.26 | TNG/DOLoRes | r | 8 × 300 | >23.47 | |
| 21.29 | TNG/DOLoRes | i | 8 × 300 | >23.98 | |
Notes. The VLT/FORS2 V-band photometry is measured in a small (0.7′′) aperture, but is not host subtracted. The errors given are statistical only and do not account for systematics between slightly different filter systems. The details of the subtraction also introduces small differences to the recovered flux, especially for sources sitting on moderately bright extended regions of their host galaxies. To account for this we estimate the additional variance on artificial stars inserted into the images to be ~ 0.05 mag.
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