QC documentation system: QC procedure QCsinfo_psf.py for SINFONI

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QCsinfo_dark.py QCsinfo_flat.py QCsinfo_wave.py
QCsinfo_dist.py QCsinfo_line.py QCsinfo_pupil.py
QCsinfo_hcao.py QCsinfo_std.py QCsinfo_psf.py
QCsinfo_sci.py
 
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NAME QCsinfo_psf.py and QCsinfo_persist.py (for the persistence check)
VERSION 1.0 -- 2006-06-22 fill template by handbook
1.1 -- 2006-07-07 revised and certified
2.0 -- 2009-04-20 completely re-written in Python with added QC functions and images
SYNTAX Python
CALL measureQuality
from $DFS_PRODUCT/PSF/$DATE:
 QCsinfo_psf.py -a $AB -i 1
INSTRUMENT SINFONI
RAWTYPE PSF
PURPOSE a) generates QC reports
PROCINPUT No input is required:
a) $DATE is now read from AB
b) primary file is set in QCsinfo_psf.py and is the PRO.CATG=COADD_PSF product with the _0000.fits extension.
c) raw frames are implicitly read from the AB.
d) other products such as MASTER_PSF, PSF_CALIBRATOR_STACKED, PSF_STAR_SPECTRA, AO_PERFORMANCE, and ENC_ENERGY are used and implicitly read.
QC1TABLE trending | table(s) in QC1 database:
sinfoni_psf
TRENDPLOT trending | HealthCheck plot(s) associated to this procedure:
trend_report_PSF_flux_HC.html
QC1PAGE trending | associated documentation:
psf_QC1.html
QC1PLOTS
top

psf1.png
display the PSF_CALIBRATOR_STACKED full detector intermediate product on the Real Time Display
psf2.png
display MASTER_PSF product on the Real Time Display
psf3.png
QC Report 1:
UL: the PSF_CALIBRATOR_STACKED full detector intermediate product image with the number of saturated pixels listed.
UR: the MASTER_PSF median cube collapsed image. A number of paramters are listed for the brightest source detected:
the source center (pixels), the integrated flux (within 3 sigma), the isophotal area (3 sigma), the net flux per pixel,
the image FWHM (arcsec), the DIMM seeing corrected for the same airmass and filter used by this standard star,
the status of the AO loop (OPEN or CLOSED),
the position angle of the brightest source (degrees CCW from the x-axis), and its elongation and ellipticity.
The source center, its position angle, and its FWHM are marked on the image. NOTE: The conversion from pixels to arcsec
in the FWHM takes into account the fact that the reconstructed SINFONI cube has RECTANGULAR pixels such that on-sky
Delta_X = 0.5*Delta_Y.
The correct conversion, in terms of the source position angle (PA), is: FWHM(arcsec) = FWHM(pixels) * pixel_scale * sqrt[(0.5*cos(PA))**2 + (sin(PA))**2].
LL: the (scaled) difference between two cube planes. Plane 100 - Plane 2072. The wavelengths of these planes
are listed to the right of this image.
LR: a horizontal (blue line) and vertical (red line) cut through the center of the brightest detected source of the
MASTER_PSF median cube collapsed image. The respective averages through this center are shown as dotted lines.
psf4.png
QC Report 2:
UL: three single column traces of the current product (PSF_CALIBRATOR_STACKED) through:
x = 500 (dark grey)
x = 1000 (middle grey)
x = 1500 (light grey)
and an averaged sum of all columns (blue).
UC: three single row traces of the current product (PSF_CALIBRATOR_STACKED) through:
x = 500 (dark grey)
x = 1000 (middle grey)
x = 1500 (light grey)
and an averaged sum of all rows (blue).
UR: the background-subtracted PSF star spectrum (PSF_STAR_SPECTRA) extracted by the pipeline.
LL: the relative encircled normalized energy as a function of radius from the source center (arcsec).
LC: the strehl ratio as a function of wavelength (microns). The median strehl ratio (dotted green line)
and the area denoting the 1 sigma strehl ratio (shaded green area) are shown.
LR: a logarithmic histogram of the STD_NODDING_STACKED full detector image is shown as a dark blue line, while
the reflection of the non-positive flux histogram is shown in light blue.
persist.png
Only if an over-flux is detected is another report created: QC Report 3:
top: a logarithmic histogram of the PSF_CALIBRATOR_STACKED full detector image with the
persistence critical region shown as a red dotted line.
LL: the PSF_CALIBRATOR_STACKED full detector intermediate product image.
LR: an estimate of the location of possible persistence critical pixels.
QC1PARAM QC1 parameters written into QC1 table (sinfoni_psf):
SOURCE(header/script)       DBNAME                value         description
if PR.find('tpx') > 0:
  QC.FRMON.MEANFLUX      qc_frmon_meanflux         0.00        mean flux ON-lamp frame
  QC.FRMOFF.MEANFLUX     qc_frmoff_meanflux        0.00        mean flux OFF-lamp frame
  QC.FRMDIF.MEANFLUX     qc_frmdif_meanflux        33.82       mean flux ON-OFF lamp
  QC.FRMON.MAXFLUX       qc_frmon_maxflux          0.00        max flux in ON-lamp frame
  QC.FRMOFF.MAXFLUX      qc_frmoff_maxflux         0.00        max flux in OFF-lamp frame
  QC.FRMDIF.MAXFLUX      qc_frmdif_maxflux         5.313e+04   max flux in ON-OFF lamp
  QC.FRMON.NPIXSAT       qc_frmon_npixsat          0.89        number of ON-lamp saturated pixels
  QC.FWHM.MAJ            qc_fwhm_maj               4.92        STD star fwhm along major axis
  QC.FWHM.MIN            qc_fwhm_min 	           3.96        STD star fwhm along minor axis
  QC.FWHM.X              qc_fwhm_x 	           4.57        STD star fwhm along X axis
  QC.FWHM.Y              qc_fwhm_y 	           3.60        STD star fwhm along Y axis
  QC.FWHM.LLX            qc_fwhm_llx 	           8           STD star fwhm LLX
  QC.FWHM.LLY            qc_fwhm_lly 	           8           STD star fwhm LLY
  QC.FWHM.HBX            qc_fwhm_hbx 	           16          STD star fwhm HBX
  QC.THETA               qc_theta 	           -1.92       STD star ellipsis angle theta
  QC.SHIFT.X             qc_shiftx 	           2.79        X centroid - image center
  QC.SHIFT.Y             qc_shifty 	           0.07        Y centroid - image center
  QC.STREHL              qc_strehl 	           0.13        strehl ratio from image
  QCsinfo_psf.py         qc_strehl_med 	           0.13        median strehl ratio
  QCsinfo_psf.py         qc_strehl_std 	           0.05        std deviation from all strehl ratios 
  QCsinfo_psf.py         qc_xpos 	           35.87       flux-weighted X-axis centroid
  QCsinfo_psf.py         qc_ypos 	           32.77       flux-weighted Y-axis centroid
  QCsinfo_psf.py         qc_center_offset 	   11.77       source offset (in pixels) from nominal field center
  QCsinfo_psf.py         qc_flux 	           2.146e+04   total flux (in ADU) within 3 sigma aperture
  QCsinfo_psf.py         qc_iso_area 	           396.4       total aperture area over which flux is summed (pixels^2)
  QCsinfo_psf.py         qc_net_flux 	           34.65       net flux (in ADU): qc_flux/qc_iso_area
  QCsinfo_psf.py         qc_posang 	           -8.33       STD star position angle (CCW along X-axis)
  QCsinfo_psf.py         qc_elong 	           1.46        STD star elongation (A_image/B_image)
  QCsinfo_psf.py         qc_ellip 	           0.16        STD star ellipticity (1 - B_image/A_image)
  QCsinfo_psf.py         qc_fwhm_dimm 	           0.90        DIMM seeing corrected to observed airmass and IR bandpass (arcsec)
  QCsinfo_psf.py         qc_fwhm_sinfo 	           0.73        STD star FWHM assuming a Gaussian core (arcsec)
  QCsinfo_psf.py         qc_delta_fwhm 	           0.17        difference (qc_fwhm_sinfo - qc_fwhm_dimm) (arcsec)
  QCsinfo_psf.py         qc_persist_danger 	   0           a test if source flux levels are too high (danger of persistence = 1; no danger = 0)
  QCsinfo_psf.py         qc_Npersist 	           0           total number of persistence critical pixels
  RTC.OBS.FWHM.MEAN      rtc_obs_fwhm_mean 	   56.03       rtd fwhm mean
  RTC.OBS.FWHM.STD       rtc_obs_fwhm_std 	   4.318       rtd fwhm std
  RTC.OBS.ENC.MEAN       rtc_obs_enc_mean 	   0.23        rtd encircled energy mean
  RTC.OBS.ENC.STD        rtc_obs_enc_std 	   0.02        rtd encircled energy std
  RTC.OBS.STR.MEAN       rtc_obs_str_mean 	   13.89       rtd mean strehl ratio
  RTC.OBS.STR.STD        rtc_obs_str_std 	   0.53        rtd strehl ratio standard deviation
ALGORITHM Description of algorithms: (status 2009-07-30)
RTC QC parameters: special AO software
QC.FRM parameters : simple statistics on the final product cube
QC.FWHM parameters : Gauss fit integrated into the pipeline; QC1 parameter inventory TBD
X,Y position, flux, and FWHM parameters : the post-pipeline script (QCsinfo_psf.py) runs SExtractor (Bertin and Arnouts 1996 A&A 117,393)
and writes these parameters for the brightest source detected. The strehl median and sigma values are first filtered for erroneous values
produced by the pipeline.
DIMM and sinfoni FWHM parameters : The header keywords TEL.AMBI.FWHM.START and TEL.AMBI.FWHM.END store the DIMM seeing measurements
(at 0.5 microns and at the zenith) at the beginning and end of the PSF exposure. The average of these two values is computed and converted to the
same airmass and wavelength as the respective PSF standard, and also include a correction for an 8m aperture using the relation given in
(Sarazin, M. 2000, Astronomical Site Monitor, VLT.SPE.ESO.17410.1174) (QCsinfo_psf.py).
Persistence test : the post-pipeline script (QCsinfo_persist.py) tests the PSF_CALIBRATOR_STACKED full detector image for instances of
6 or more pixels (to select against cosmic ray events) having flux levels greater than 10,000 ADU. If 10 or more such events are discovered
an over-flux alarm is given (qc_persist_danger = 1). The number of affected pixels satisfying the above criteria are given by qc_Npersist.
CERTIF Tolerated:
- multiple sources
- stars in sky frame
- strong skew of spectrum
Rejected:
- very low flux levels
- extremely high flux (saturated)
- strong persistence in SKY frame
COMMENTS None
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