The astrometric and photometric pre-processing produces the direct
observational results for the SM and AF CCDs, thus feeding the astrometric core
process (AGIS) and the band photometry processing (PhotPipe). More specifically, it
converts the raw telemetry (see Section 2.2.2) to image
parameters (see Section 2.4.8), i.e., transit time,
flux, and position on the CCD, for each CCD transit of each detected object.
This necessarily includes the calibration of the CCD bias (see
Section 2.3.5), and cosmetics (see
Section 2.3.4), as well as the background (see
Section 2.3.3, Section 2.4.6), and
the PSF/LSF (see Section 2.3.2). For an overview of the
pre-processing, see Fabricius et al. (2016).
Another functionality of the photometric pre-processing is the reconstruction
of the raw photometric measurements from the BP and RP CCDs to feed the
and bands photometry (PhotPipe), see Section 2.4.3.
In the process, it also produces preliminary spectro-photometric results
(see Section 2.4.7),
mainly used to monitor the correct operation of those instruments (see Section 2.5.2).
The pre-processing also takes care of the identification of objects (see
Section 2.4.9) in a source list
and of determining a first on-ground attitude
(see Section 2.4.5) of the spacecraft, using a star
catalogue (see Section 2.2.3).
The pre-processing runs on a daily basis, to allow a close
monitoring of the status and performance of the instruments (see
Section 2.5.1), and to issue alerts on interesting
sources. However, the CCDs and instrument cannot be calibrated
optimally in almost real time, as the models need refinement, and as they
depend on information on the source astrometry and photometry, not yet
available. Calibrations, image parameter determination, and object
identification are therefore elements of a grand iteration loop, completed
once in every data reduction cycle (see Section 2.4.2).
The feedback from the astrometric and photometric core processes is
particularly important for the PSF calibration, which must properly take
chromatic effects into account for the image shape as well as for the PSF