Table 4.
Error budget of the J-PLUS photometric calibration.
| Passband | σSLR | σISL | σISL + P | σWD | σISL + P + WD | σcal |
|---|---|---|---|---|---|---|
| 0pt2ex | [mmag] (a) | [mmag] (b) | [mmag] (c) | [mmag] (d) | [mmag] (e) | [mmag] (f) |
| u | 37 | 23 | 17 | 5 | 18 | 18 |
| J0378 | 38 | 23 | 19 | 5 | 20 | 20 |
| J0395 | 37 | 22 | 17 | 5 | 18 | 18 |
| J0410 | 28 | 16 | 9 | 4 | 10 | 11 |
| J0430 | 27 | 18 | 9 | 4 | 10 | 11 |
| g | 21 | 13 | 4 | 2 | 4 | 7 |
| J0515 | 18 | 11 | 6 | 3 | 7 | 8 |
| r | 14 | 12 | 4 | 0 | 4 | 6 |
| J0660 | 19 | 17 | 4 | 3 | 5 | 7 |
| i | 12 | 12 | 4 | 2 | 4 | 7 |
| J0861 | 14 | 12 | 5 | 4 | 6 | 8 |
| z | 15 | 12 | 5 | 4 | 6 | 8 |
Notes.
Stellar locus regression (SLR) was used as calibration method. Uncertainty from duplicated MS stars in overlapping pointings.
Instrumental stellar locus (ISL) or PS1 was used to homogenize the photometry. Uncertainty from duplicated MS stars in overlapping pointings.
ISL (or PS1) and the plane correction were used to homogenize the photometry. Uncertainty from duplicated MS stars in overlapping pointings.
Final uncertainty in the J-PLUS flux calibration, 
, where σr = 5 mmag (Sect. 5.4).
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