Table 1.
Basic information about the synthetic imaging datasets and some assumptions for simulating the different sources of noise.
| Survey | Instrument | Filter | Wavelength | PSF FWHM | Pixel size | mlim | SBbkg | texp |
|---|---|---|---|---|---|---|---|---|
| (Å) | (arcsec) | (arcsec) | (mag) | (mag) | (s) | |||
| GALEX | … | FUV | 1340–1810 | 4.48 | 1.5 | … | … | 1500 |
| GALEX | … | NUV | 1693–3008 | 5.05 | 1.5 | … | … | 1500 |
| LSST | … | u | 3206–4082 | 1.17 | 0.2 | 23.6 | 22.70 | 150 |
| LSST | … | g | 3876–5665 | 1.13 | 0.2 | 24.5 | 22.00 | 150 |
| LSST | … | r | 5377–7055 | 1.00 | 0.2 | 23.9 | 20.80 | 150 |
| LSST | … | i | 6766–8325 | 1.00 | 0.2 | 23.6 | 20.30 | 150 |
| LSST | … | z | 8035–9375 | 1.00 | 0.2 | 23.4 | 19.40 | 150 |
| Euclid wide | VIS | IE | 4971–9318 | 0.17 | 0.1 | 24.6 | 22.33 | 4 × 590 |
| Euclid wide | NISP | YE | 9382–12435 | 0.40 | 0.3 | 23.0 | 22.10 | 4 × 88 |
| Euclid wide | NISP | JE | 11523–15952 | 0.45 | 0.3 | 23.0 | 22.11 | 4 × 90 |
| Euclid wide | NISP | HE | 14972–20568 | 0.50 | 0.3 | 23.0 | 22.28 | 4 × 54 |
Notes. mlim, SBbkg, and texp are 10σ (S/N = 10) limiting magnitude within 2″ aperture, the background surface brightness, and total exposure time of the final mosaic, respectively. The values for Euclid are not updated to the latest estimates of the actual in-flight values because that information was not available at the time of our analysis. For the LSST images, we adopt the depths from a single visit (i.e. exposure), which will be available for a wide area soon after the survey is started, not the final depths after 10 years of the survey.
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