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- | You may want to reprocess your spectroscopic data. This can be done on the **observer5** computer. The necessary software is installed in /opt/EffelsbergSpecPipeline. There is a bash script to set all the necessary paths. tcsh shell users should change to bash by typing bash. The teleskop, obs2 account are already bash accounts. Launch the following command:\\ | ||
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- | **source /opt/EffelsbergSpecPipeline/init_classwriter.sh**\\ | ||
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- | Now you should be ready to run the Offline Calibration pipeline. Type\\ | ||
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- | **OfflinePipeline**\\ | ||
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- | Now you are in an ipython interface to reduce the data. There are the following commands to reduce the data:\\ | ||
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- | **setFitsDir('/daten/Raw')**\\ | ||
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- | Set the source directory for the rawdata. The program looks in the directory for the raw mbfits files.\\ | ||
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- | **setClassName('Filename','Directory')**\\ | ||
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- | this sets the output gildas, class file. if only:\\ | ||
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- | **setClassName('Filename')**\\ | ||
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- | is given, the named file is created in the current dictionary. Without this command | ||
- | a file name e.g. like class_2010_10_20.100m is created in the current directory. | ||
- | To write the files one has to know the scan number and must give the subscan number. | ||
- | Subscan numbers are 1 based. If the subscan is not in the file an error is plotted.\\ | ||
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- | **reduceSubscan(scannumber,subscannumber)**\\ | ||
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- | If you reduce the same scan twice, it is written twice to the class file with the same scan number. You can investigate the result with [[information_for_astronomers:using_class_on_observer3_computer_in_effelsberg|]]\\ | ||
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- | **fixFFTSRefChannel(shiftFFTSRefChannel=True)**\\ | ||
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- | Before February 2011 the reference channel of the FFTS has to be shifted by +0.5 channels if the spectrum was not if flipped, otherwise -0.5 channels.\\ | ||
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- | **flipArrayOrientation(reverseArrayOrientation=True)**\\ | ||
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- | This function flips the dataArrays for the following reduce operations. | ||
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