es.generateQA2Report
Return to directory of Todd's CASA extensions
The script was used during ALMA Cycle 0 (and at least part of Cycle 1) to create a QA2 report
to be delivered with the data to the PI. It was originally consolidated, tested, and maintained by Eric.
More recently, Todd is the maintainer.
Usage
es.generateQA2Report(ms1='', ms2='', phase_cal='', target='', target_source='',
tsys_field='', dospw='', refAnt='', qa2_output_dir='',
uvrange='0~30m', autoscale_yaxis=True, fdmSpwsToImage='',
ant_gain_check_caltable=None,
ant_amp_temporal_caltable=None,
ant_phase_temporal_caltable=None, wvrspw='', avgchannel=5,
flaggedFraction=0.75, phaseDiff='',useLocalAlmaHelper=True,
ampcalspw=[], phasecalspw=[], nSpwsFlagged=0,
wvrScanIntent='BANDPASS')
- ms1: the name of the parent ms (any trailing '/' will be removed)
- ms2: the name of the split ms (the default is to add ".split" to ms1)
- phase_cal: the source ID of the phase calibrator as a string (e.g. '3')
- target: the field ID of the science target as a string (e.g. '3')
- It is used by es.target_spectrum, and for cleaning and plotuv.
- The default is the ID of the target_source
- target_source: the source ID of the science target as a string (e.g. '3')
- It is used by es.sensitivity_calculator.
- The default is the first source with OBSERVE_TARGET intent.
- tsys_field: the field ID to use for Tsys stats as a astring (e.g. '3')
- dospw: a list of spws to use in target_spectrum (e.g. '0,1')
- refAnt: the reference antenna name to use in wvr_stat (e.g. 'DV05')
- wvrScanIntent: the scan intent to use in wvr_stat (e.g. 'FLUX')
- qa2_output_dir: the directory to write the output files
- uvrange: the uv range to use in target_spectrum (e.g. '0~30m')
- autoscale_yaxis: Boolean passed to wvr_stat
- fdmSpwsToImage: a list of spws to image in target_check (e.g. ['2','3'])
- ant_gain_check_caltable: the caltable to use in ant_gain_check
- ant_amp_check_caltable: the caltable to use in ant_amp_temporal
- ant_phase_check_caltable: the caltable to use in ant_phase_temporal
- wvrspw: the science spw to use in wvr_stat (e.g. '17')
- avgchannel: the number of channels to average in target_spectrum (integer)
- flaggedFraction: when computing clean cellsize, don't consider baselines for antennas whose data are flagged by more than this fraction
- ampcalspw: which spws to plot in ant_amp_temporal (default = all)
- phasecalspw: which spws to plot in ant_phase_temporal (default = all)
- nSpwsFlagged: number of spws that were fully flagged during calibration
INSTRUCTION
- Run Eric's reduction script generated by es.generateReducScript() in an appropriate directory.
- Run es.generateQA2report('msname')
SUMMARY OF CAL TABLES NEEDED:
1. tsys_stat() expects uid___Axxxxxx_xxxx.ms.tsys
2. ant_gain_check() expects uid___Axxxxxx_xxxx.ms.split.ap_pre_bandpass
but you can specify it via the optional ant_gain_check_caltable argument
3. bandpass_rms() expects uid___Axxxxxx_xxxx.ms.split.bandpass
4. bandpass_plot() expects original table uid___Axxxxxx_xxxx.ms.split.bandpass
and also looks for smoothed table uid___Axxxxxx_xxxx.ms.split.bandpass_smooth20ch
or uid___Axxxxxx_xxxx.ms.split.bandpass_bpoly
5. ant_amp_temporal() expects uid___Axxxxxx_xxxx.ms.split.flux_inf
if it doesn't find it, it looks for uid___Axxxxxx_xxxx.ms.split.cal_amp
but you can specify it via the optional ant_amp_temporal_caltable argument
6. ant_phase_temporal() expects uid___Axxxxxx_xxxx.ms.split.phase_inf
if it doesn't find it, it looks for uid___Axxxxxx_xxxx.ms.split.cal_phase
but you can specify it via the optional ant_phase_temporal_caltable argument
7. flux_values() expects uid___Axxxxxx_xxxx.ms.split.fluxscale
--
ToddHunter - 2013-03-27