This documentation is intended both for QC scientists and SciOps astronomers (who may want to ignore the technical information displayed in grey).
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NAME |
pionier_kappaQC.py
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VERSION |
1.0 -- 2015-06-06
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SYNTAX |
PYTHON
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CALL |
measureQuality from $DFS_PRODUCT/KAPPA_MATRIX/$DATE:
pionier_kappaQC.py -a $AB
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INSTRUMENT |
PIONIER
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RAWTYPE |
RAW_KAPPA_MATRIX
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PURPOSE |
a) generates QC reports
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PROCINPUT |
No special input is required:
a) $DATE is read from the input AB
c) frames are implicitly read from the AB.
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QC1TABLE |
trending | table(s) in QC1 database:
pionier_dark
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TRENDPLOT |
trending | HealthCheck plot(s) associated to this procedure:
trend_report_KAPPA_HC.html
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QC1PAGE |
trending | associated documentation:
kappamatrix_qc1.html
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QC1PLOTS
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r.PIONI.2015-11-28T09:05:00.033_tpl_0000.png
r.PIONI.2015-11-28T09:05:00.033_tpl_0001.png
r.PIONI.2015-11-28T09:05:00.033_tpl_0002.png
r.PIONI.2015-11-28T09:05:00.033_tpl_0002.png
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QC1PARAM |
QC1 parameters written into QC1 table :
SOURCE(header/script) DBNAME value description
QC.KAPPA1.RMS kappa_rms1 0.27 error_on_kappa_optical_train1
QC.KAPPA2.RMS kappa_rms2 0.24 error_on_kappa_optical_train2
QC.KAPPA3.RMS kappa_rms3 0.35 error_on_kappa_optical_train3
QC.KAPPA4.RMS kappa_rms4 0.31 error_on_kappa_optical_train4
QC.KAPPARAW1.AVG kappa_avg1 754.06 flux_optical_train1_in_adu
QC.KAPPARAW2.AVG kappa_avg2 921.48 flux_optical_train2_in_adu
QC.KAPPARAW3.AVG kappa_avg3 646.6 flux_optical_train3_in_adu
QC.KAPPARAW4.AVG kappa_avg4 1040.7 flux_optical_train4_in_adu
QC.KAPPA12.AVG kappa_avg12 0.99 kappa_baseline12_(interferometric_transmission)
QC.KAPPA13.AVG kappa_avg13 0.99 kappa_baseline13_(interferometric_transmission)
QC.KAPPA14.AVG kappa_avg14 0.98 kappa_baseline14_(interferometric_transmission)
QC.KAPPA23.AVG kappa_avg23 0.97 kappa_baseline23_(interferometric_transmission)
QC.KAPPA24.AVG kappa_avg24 0.98 kappa_baseline24_(interferometric_transmission)
QC.KAPPA34.AVG kappa_avg34 0.99 kappa_baseline34_(interferometric_transmission)
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ALGORITHM |
Description of algorithms:
This measures the internal flux ratio (interferometric transmission
for the pixels on the detector (science outputs).
Data can be taken on sky (used to calibrate sky data).
or on the internal lamp (HC).
Four files are recorded, each of them has the shutter of one telescope opened (T),
the other 3 beeing closed (F) : TFFF,FTFF, FFTF, FFFT
Compute the photometric transmission matrix.
The first 40 elements of the scans are discarded
and all values of the rest of the scans are averaged
The normalization is done by averaging the flux of each telescope
and per spectral channel
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CERTIF |
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COMMENTS |
None
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[2016-11-02T07:22:50] created by qcDocu v1.1.2, a tqs tool
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