Table 1.
Imaging dataset.
| Filter | λcentral(nm) | Exp. time (s) | FWHM (arcsec) | AB Mag. limit (S/N = 10) | Instrument | Pixel scale  |
|---|---|---|---|---|---|---|
 |
355 | 28 700 | 0.94 | 26.6 (26.8) | LBC (LBT) | 0.225 |
 |
475 | 12 200 | 1.12 | 27.1 | LBC (LBT) | 0.225 |
 |
622 | 12 000 | 0.97 | 26.4 | LBC (LBT) | 0.225 |
 |
764 | 27 000 | 0.97 | 25.8 (26.2) | Suprime-Cam (Subaru) | 0.150 |
 |
903 | 38 880 | 1.15 | 24.9 | Suprime-Cam (Subaru) | 0.150 |
| Y (c) | 1020 | 42 360 | 0.85 | 25.1 (26.0) | Vir-Cam (VISTA) | 0.300 |
| J (c) | 1250 | 49 720 | 0.81 | 24.9 (25.5) | Vir-Cam (VISTA) | 0.300 |
| H (c) | 1650 | 42 520 | 0.80 | 24.6 (25.0) | Vir-Cam (VISTA) | 0.300 |
| K (c) | 2150 | 39 400 | 0.80 | 24.1 (25.1) | Vir-Cam (VISTA) | 0.300 |
Notes. The FWHM of the PSF has been measured on a stacking of a selected sample of bright non-saturated stars. Limiting magnitudes have been measured in diameter apertures of 2 arcsec. Because some images have variable depth across the field, we report in parentheses the limiting magnitude of the deepest portions in each band.
References. (a)Boutsia et al. (2014), (b)Taniguchi et al. (2007), and (c)McCracken et al. (2012).
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