The astrometric accuracy is derived in the same way as for the Wide survey. We refer to the beginning of Section 4.5 for a description of the method. The Deep analysis is however simpler than the Wide because there is only one single position per field. The astrometric calibration of the Deep fields is detailed in Section 3.5, so we only focus on the accuracy in this section.
The results of the internal and external error analysis are given in Tables 17 and 18. The internal errors have been measured by SCAMP, from the astrometric solutions of each Deep field, for each filter separately. In contrast, the external errors quoted in Tables 17 and 18 are not the values derived from the astrometric solutions. They are computed separately as well, but after the production of the Deep images, in order to get the true astrometric errors of sources in each stack. The reference external catalogue is 2MASS, and the external errors found are very similar to the Wide survey.
On average, the mean internal astrometric rms errors in the Deep fields are
|
| (17) |
and the mean external errors
 | (18) |
where, the dispersions are the rms errors. Since the four fields are calibrated independently, the values quoted above are only rough estimates; the errors for D1, D2, D3 and D4 are given in Tables 17 and 18. The rather large scatter in the internal errors is due to the different ways each Deep field has been calibrated (either using an internal catalogue based on the i band data, or using the external 2MASS catalogue, see Section 3.5). The external astrometric errors are similar to the Wide survey and correspond to the expectations, considering the astrometric errors in the 2MASS reference catalogue.