Quality Control and
Data Processing

Scoring&thresholds Efficiency

The value of the thresholds have been defined together with the Instrument scientist.

History

The evolution of the transmission on the AT is shown here

Algorithm Efficiency

The pipeline calculates the visibilities on the 6 baselines, the 3 closure phases as well as the transmission of each beam when the photometry of the object observed is known. ~

ESO provides to the observer a tool to retrieve the calibrator best suitable for their observations. This tool is available under

QC1_parameters

FITS key	QC1 database: table, name	definition	class*	HC_plot**	more docu
QC.PHI123.AVG	pionier_fringe..phi123_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
QC.PHI124.AVG	pionier_fringe..phi124_avg	average phase closure	CAL		[docuSys coming]
QC.PHI134.AVG	pionier_fringe..phi134_avg	average phase closure	CAL		[docuSys coming]
QC.PHI234.AVG	pionier_fringe..phi234_avg	average phase closure	CAL		[docuSys coming]
QC.SNR12.AVG	pionier_fringe..snr12_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
QC.SNR13.AVG	pionier_fringe..snr13_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
QC.SNR14.AVG	pionier_fringe..snr14_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
QC.SNR23.AVG	pionier_fringe..snr23_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
QC.SNR24.AVG	pionier_fringe..snr24_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
QC.SNR34.AVG	pionier_fringe..snr34_avg	average SNR per baseline SNR=SNRU/SNRL	CAL		[docuSys coming]
*Class: KPI - instrument performance; HC - instrument health; CAL - calibration quality; ENG - engineering parameter **There might be more than one.

fringes (reconstructed as seen during the observation)

Trending

When fringes are obtained on a target (Science or astronomical calibrator), its uncalibrated Visibility and closure phase is calculated by the pipeline.
The HC plots Visibility and Visibility (night) shows the Visibilities on the last 3 months of data and the ones measured during the observing night.

The closure phases are also trended here

Scoring&thresholds Visibility and Closure Phase on Astromical Calibrators

These data are not scored as they depend on a lot of "external" factors : baselines of observations, atmospheric conditions, tracking of the delay lines

History

The evolution of the Visibilities is shown here

Algorithm Visibility and Closure Phase on Astromical Calibrators

The pipeline uses the fringe data contained in the raw files to reduce them into uncalibrated measurements of the visibilities and the closure phases. It is done file by file (typically a PIONIER observation contains 5 files).
The pipeline averages the data over the 100 scans (standard exposure).

ESO provides to the observer a tool to retrieve the calibrator best suitable for their observations. This tool is available under . This catalog includes diameters of more than 440000 objects.

QC1_parameters

FITS key	QC1 database: table, name	definition	class*	HC_plot**	more docu
QC.TFVIS12.AVG	pionier_fringe..tfvis12_avg	average TF per baseline	CAL		[docuSys coming]
QC.TFVIS13.AVG	pionier_fringe..tfvis13_avg	average TF per baseline	CAL		[docuSys coming]
QC.TFVIS14.AVG	pionier_fringe..tfvis14_avg	average TF per baseline	CAL		[docuSys coming]
QC.TFVIS23.AVG	pionier_fringe..tfvis23_avg	average TF per baseline	CAL		[docuSys coming]
QC.TFVIS24.AVG	pionier_fringe..tfvis24_avg	average TF per baseline	CAL		[docuSys coming]
QC.TFVIS34.AVG	pionier_fringe..tfvis34_avg	average TF per baseline	CAL		[docuSys coming]
*Class: KPI - instrument performance; HC - instrument health; CAL - calibration quality; ENG - engineering parameter **There might be more than one.

Trending

When fringes are obtained on an astronomical calibrator its uncalibrated Visibility and closure phase are calculated by the pipeline. If the calibrator has a known diameter (and associated error), the pipeline calculates its Transfer Function.
The HC plots Transfer Function and Transfer Function (night) shows the Transfer Function on the last 3 months of data and the ones measured during the observing night.

Scoring&thresholds Transfer Function on Calibrators

These data are not scored in the HC plots but are used to assess the quality of the night.
A calibrator should be an object as small as possible for the observing baselines, so its TF should be close to 1. The TF measured on the same object, on the same baselines and not too far in time (to have the same atmospheric conditions) should not show a high scatter,

History

The evolution of the TF is shown here

Algorithm Transfer Function on Calibrators

The pipeline uses the uncalibrated measurements of the visibilities and the closure phases calculated previously as well as the diametre of the calibrator (if found) to calculate the Transfer Function.
.