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Quality Control and
Data Processing


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QUALITY CONTROL
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CRIRES: Dark
DARK level | DARK RON | DARK NBAD

 
HC PLOTS
Dark median YJHK bands
Dark median LM bands
Read-Out Noise
Dark median
Dark nbad
QC1 database (advanced users): browse | plot

Dark frames are taken daily as part of the calibration plan in sets of 3 frames for each DET.SEQ1.DIT value. Darks in specific setups: INS.WLEN.ID=Y1029, J1232, H1559, K2217, L3377, M4266, with short and long DIT are taken every day as health checks. Darks in other setups are only measured when they are triggered by settings of science data observed during the night.


Example of the DET.WLEN.ID=J1232, DET.SEQ1.DIT=10.0 sec dark frames for all 3 detectors.

Information about the Quality Control performed utilizing dark frames of the instrument BEFORE the upgrade (before 2021-09) can be found here.


DARK level
DARK level | DARK RON | DARK NBAD

QC1_parameters

FITS key QC1 database: table, name definition class* HC_plot** more docu
QC.DARK.MEDIAN criresp_dark..dark_median median dark level of input frames HC [docuSys coming]
*Class: KPI - instrument performance; HC - instrument health; CAL - calibration quality; ENG - engineering parameter
**There might be more than one.

Trending

The median dark level is trended for each detector, as well as for YJHK and LM bands, separately.

Scoring&thresholds DARK level

The dark_median of the J1228 wavelength setup master darks is tightly scored, with dynamic thresholds following the median average of the current period. The only requirement on the dark current is stability on the calibration timescale.

History

Date event
2021-10-01 beginning of operations of the upgraded CRIRES

Algorithm DARK level

Group the input frames by different values of DET.SEQ1.DIT and WLEN.ID; Load the images and create the associate error for each of them; Collapse the images; Compute BPM from the collapsed master dark; The median level of master dark is calculated for each detector.


DARK RON
DARK level | DARK RON | DARK NBAD

QC1_parameters

FITS key QC1 database: table, name definition class* HC_plot** more docu
QC.DARK.RON1 criresp_dark..dark_ron1 RON whole frame raw2-raw1HC [docuSys coming]
*Class: KPI - instrument performance; HC - instrument health; CAL - calibration quality; ENG - engineering parameter
**There might be more than one.

Trending

The read-out noise (RON) is trended for each detector, selected setups.

Scoring&thresholds DARK RON

The ron1 is scored, with dynamic thresholds following the median average of the current period. The only requirement on the dark RON is stability on the calibration timescale.

History

Date event
2021-10-01 beginning of operations of the upgraded CRIRES

Algorithm DARK RON

Group the input frames by different values of DET.SEQ1.DIT and WLEN.ID; Load the images and create the associate error for each of them; Collapse the images; Compute BPM from the collapsed master dark; The RON is derived from difference between 2nd and 1st input frame, ron1, and between 3rd and 2nd, ron2) of the master dark; It is calculated for each detector.


DARK NBAD
DARK level | DARK RON | DARK NBAD

QC1_parameters

FITS key QC1 database: table, name definition class* HC_plot** more docu
QC.DARK.NBAD criresp_dark..dark_nbad number of bad pixels in master dark [docuSys coming]
*Class: KPI - instrument performance; HC - instrument health; CAL - calibration quality; ENG - engineering parameter
**There might be more than one.

Trending

The number of bad pixels (nbad) is trended for each detector, selected setup.

Scoring&thresholds DARK NBAD

The dark_nbad is scored, with dynamic thresholds following the median average of the current period. The only requirement on the dark number of bad pixels is stability on the calibration timescale.

History

Date event
2021-10-01 beginning of operations of the upgraded CRIRES

Algorithm DARK NBAD

Group the input frames by different values of DET.SEQ1.DIT and WLEN.ID; Load the images and create the associate error for each of them; Collapse the images; Compute BPM from the collapsed master dark; The number of bad pixels is calculated where the bad pixels are those that deviate from average signal; It is calculated for each detector.


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