With ALMA or NOEMA, you may end up with an observational data set that contains several sources, each of them observed with a number of spectral windows of different spectral resolutions, covering many spectral lines.
The bookkeeping of such data sets can be intricate. To help the users to focus on the science, we have developped a pipeline (namely a suite of scripts named violetall-*.ima) that automates the whole imaging process in this case. This pipeline can be run through the magentaPIPELINE command, or through a control panel launched by the magentaPIPELINE /WIDGET command.
The pipeline control parameters are available in the blueALL% global structure, and can be checked using the magentaPIPELINE ? command.
The pipeline is intended to handle all spectral sub-bands for a single receiver tuning of the interferometer, with the data (possibly with several observing dates) for each sub-band and each source stored in a separate file (in UVFITS or GILDAS UV format).
The principle is to gather all UV tables in a sub-directory (named ./RAW/ by default), and to store the results of the various processing steps (Self Calibration, Spectral line extraction, Imaging) in different sub-directories (respectively named cyan./SELF/, ./TABLES/, ./MAPS/ by default).
The behaviour of the Imaging step depends on the pipeline mode, blueALL%MODE, that can be controlled by the magentaPIPELINE /MODE option. It also depends on whether a magentaCATALOG is used or not, and on the blueALL%RANGE[1:3] variable that controls the velocity span and resolution.
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Gildas manager
2023-06-01