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RadioAstron Closed Loop for DiFX

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    Comparing version 14:21, 16 May 2019 by jwagner with version 13:40, 17 May 2019 by jwagner.

    ...

    ---Iterative improvement of the ASC poly coefficients might be necessary. Currently, we know ASC has a method to do this, but at Bonn we do not have details yet. With PIMA fringe fitting one could determine delay, rate, acceleration residuals. However how higher-order terms could be refined is yet unclear. Once we settle at a good approach, a mechanism to feed back fringe-fit results into raPatchClosedloop.py will be implemented.

    TODO:

    1) run PIMA, make fringe fit on scan(s)

    2) parse PIMA .fri files, patch rate&accel into ASC coeffs producing a new file (2nd gen): need some new script perform the parse and patch

    3) re-run raPatchClosedloop with the 2nd gen poly file, re-run DiFX

    4) run PIMA on the 2nd gen visibility data to check whether residual rate and accel are reduced

    Version from 14:21, 16 May 2019

    This revision modified by jwagner (Ban)

    ...

    Version as of 13:40, 17 May 2019

    This revision modified by jwagner (Ban)

    ...

    ---Iterative improvement of the ASC poly coefficients might be necessary. Currently, we know ASC has a method to do this, but at Bonn we do not have details yet. With PIMA fringe fitting one could determine delay, rate, acceleration residuals. However how higher-order terms could be refined is yet unclear. Once we settle at a good approach, a mechanism to feed back fringe-fit results into raPatchClosedloop.py will be implemented.

    TODO:

    1) run PIMA, make fringe fit on scan(s)

    2) parse PIMA .fri files, patch rate&accel into ASC coeffs producing a new file (2nd gen): need some new script perform the parse and patch

    3) re-run raPatchClosedloop with the 2nd gen poly file, re-run DiFX

    4) run PIMA on the 2nd gen visibility data to check whether residual rate and accel are reduced