PIPELINES AT ESO
Pipelines are used at ESO to process both calibration data and science data
and to retrieve quality information.
There is a dedicated
pipeline for each VLT and VLTI instrument.
Find general information about ESO reduction pipelines here.
The main functionalities of the pipelines are:
QC Garching creates master calibration data from all raw calibration data. The
raw data are stored in the ESO Archive and are public. They are
quality-checked and used for data reduction and for trending.
- create master calibration data,
- reduce science frames,
- extract QC information from the data.
For selected instrument modes, we offer science-grade data products processed
with the pipelines.
There are two instances of the data reduction pipelines:
The automatic mode is used for quick look and for on-site quality
control. It processes all raw data sequentially, as they arrive from the
instrument. If calibration products ("master calibrations") are required for
processing science data, these are taken from a database with standard,
pre-manufactured calibration products. The automatic mode is not tuned to
obtain the best possible results.
- at the instrument workstation on Paranal, running in automatic mode,
- at HQ Garching, run by the Quality Control Group in the optimized mode.
The optimized mode is the mode, which uses all data of a night, including the
daytime calibrations. The calibration data are sorted and grouped according to
their dependencies. Master calibration data are created. Their quality is
The ESPRESSO detector consists of two e2v CCDs, each with 9216x9232 optically
| file type || binning || size of raw file|
| calibration or science frame || 1x1 || 352 MB|
| calibration or science frame || 2x1 || 176 MB|
| calibration or science frame || 4x2 || 44 MB|
| calibration or science frame || 8x4 || 11 MB|
Raw calibration and science data come as FITS files with one primary header unit (HDU) and at least two extensions,
one for each chip.
The primary HDU has all keywords necessary to identify the observation and the state of the telescope and the instrument;
the data part is empty. Pixel data are stored in the extensions.
Observations of standard stars and of science targets have additional
extensions which contain data from the exposure meter (as binary table) and
integrated images of the fibre heads. The size of these extensions is
negligible compared to the first two extensions.