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README
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1 Installation
Requirements:
• Python 3.0 or higher.
• Compiled shared libraries of the FORTRAN version of the Starlink as-
tronomical libraries (SLALIB) available from http://starlink.eao.hawaii.edu/starlink/2018ADownload.
• A copy of parallel ready H5Py. Installation instructions can be found
here http://docs.h5py.org/en/stable/mpi.html.
N.B.: If you are using an Anaconda packaged version of Python installation you may
need to remove the existing conda install of HDF5.
• The latest version of HealPy and mpi4py (either openMPI or MPICH
work as backends).
To install the Manchester COMAP reduction pipeline:
• Clone/download the github repository found here: https://github.com/SharperJBCA/COMAPreduce
• Enter the directory:
> cd COMAPreduce
> run python setup.py install
If your SLALIB libaries are not in standard location you must define
the environment variable: SLALIB_LIBS
• To run the COMAP pipeline make a new directory above COMAPreduce
> cd ../ && mkdir runcomapreduce
and copy the run.py, COMAP_FEEDS.dat and .ini files to this directory.
• The pipeline can then be run using the command:
> mpirun -n X python run.py -F FILELIST.list -P PARAMETERS.ini. FILELIST.list
should contain a list of files with either just the filenames to be processed or
the full path to files to be processed. PARAMETERS.ini will con-
trol the processing to be performed, details of which are described in
Sections 2 and 3.
• N.B.: You will also need to copy COMAP_FEEDS.dat from COMAPreduce to your working directory.
2 Usage
2.1 Parameter Files
There are several example parameter files already included:
• AmbLoad.ini - This will calculate the T sys and gain (e.g. volts per
Kelvin) from ambient load stare observations.
• Downsample.ini - This will downsample a data file in frequency by
factor times and also check to see if any pointing needs to be added.
• FitJupiter.ini - This will fix the pointing, downsample, and cali-
brate a Jupiter observation to the ambient load. Then it will fit a
Gaussian to the time ordered data to derive amplitude, pointing and
beam width measurements. It will also produce a calibration scale in
units of Janskys/Kelvin for every horn and frequency channel.