|This documentation is intended both for QC scientists and SciOps astronomers (who may want to ignore the technical information displayed in grey).
QCsinfo_sci.py and QCsinfo_persist.py (for the persistence check)
2.0 -- 2009-07-02 completely re-written in Python with added QC functions and images
from $DFS_PRODUCT/OBSNOD/$DATE/ or $DFS_PRODUCT/OBSJIT/$DATE/
QCsinfo_sci.py -a $AB -i 1
OBSNOD and OBSJIT
a) generates QC reports |
No input is required: |
a) $DATE is now read from AB
b) primary file is set in QCsinfo_sci.py and is the PRO.CATG=COADD_OBJ product with the _0000.fits extension.
c) raw frames are implicitly read from the AB.
d) other products such as MED_COADD_OBJ, and OBJECT_NODDING_STACKED are used and implicitly read.
trending | table(s) in QC1 database: |
trending | HealthCheck plot(s) associated to this procedure: |
trending | associated documentation: |
display the OBJECT_NODDING_STACKED full detector intermediate product on the Real Time Display
display MED_COADD_OBJ product on the Real Time Display
display 3-d sciece cube product COADD_OBJ on the QFitsView display
QC Report 1:
UL: the OBJECT_NODDING_STACKED full detector intermediate science image with the number of saturated pixels listed.
UR: the MED_COADD_OBJ median cube collapsed science image. A number of paramters are listed:
the Program ID, the Obs ID, the target name, the time and AM difference between the science OB and its
associated telluric STD, and for the brightest source detected:
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
MED_COADD_OBJ median cube collapsed science image. The respective averages through this center are shown as dotted lines.
QC Report 2:
UL: three single column traces of the current product (OBJECT_NODDING_STACKED) through:
x = 500 (dark grey)
x = 1000 (middle grey)
x = 1500 (light grey)
and an averaged sum of all columns (blue).
UR: three single row traces of the current product (OBJECT_NODDING_STACKED) through:
x = 500 (dark grey)
x = 1000 (middle grey)
x = 1500 (light grey)
and an averaged sum of all rows (blue).
LL: the background-subtracted spectrum of the brightest science source. This spectrum is computed by the post-pipeline
script QCsinfo_sci.py. The green line is the peak flux extracted from each cube plane at the position of the brightest source,
whereas the blue line is the average flux over the FWHM measured for the brightest source. The red line is an estimate of the
LR: a logarithmic histogram of the OBJECT_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.
Only if an over-flux is detected is another report created: QC Report 3:
top: a logarithmic histogram of the OBJECT_NODDING_STACKED full detector science image with the
persistence critical region shown as a red dotted line.
LL: the STD_NODDING_STACKED full detector intermediate product image.
LR: an estimate of the location of possible persistence critical pixels.
QC1 parameters written into QC1 table (sinfoni_sci):|
SOURCE(header/script) DBNAME value description
QC.FRMON.MEANFLUX qc_frmon_meanflux 327.1 mean flux ON-lamp frame
QC.FRMOFF.MEANFLUX qc_frmoff_meanflux 307.6 mean flux OFF-lamp frame
QC.FRMDIF.MEANFLUX qc_frmdif_meanflux 55.14 mean flux ON-OFF lamp
QC.FRMON.MAXFLUX qc_frmon_maxflux 4.841e+04 max flux in ON-lamp frame
QC.FRMOFF.MAXFLUX qc_frmoff_maxflux 4.843e+04 max flux in OFF-lamp frame
QC.FRMDIF.MAXFLUX qc_frmdif_maxflux 1.698e+04 max flux in ON-OFF lamp
QC.FRMON.NPIXSAT qc_frmon_npixsat 10.98 number of ON-lamp saturated pixels
RTC.OBS.ENC.MEAN rtc_obs_enc_mean 0.36 rtd encircled energy mean
RTC.OBS.ENC.STD rtc_obs_enc_std 0.01 rtd encircled energy std
RTC.OBS.FWHM.MEAN rtc_obs_fwhm_mean 61.27 rtd fwhm mean
RTC.OBS.FWHM.STD rtc_obs_fwhm_std 0.67 rtd fwhm std
RTC.OBS.L0MEAN rtc_obs_l0mean 39.68 rtc mean outer scale [m]
RTC.OBS.LOSTD rtc_obs_l0std 5.90 rtc std dev of outer scale [m]
RTC.OBS.R0MEAN rtc_obs_r0mean 0.12 rtc mean Fried parameter [m]
RTC.OBS.R0STD rtc_obs_r0std 0.01 rtc std dev of Fried parameter [m]
RTC.OBS.STR.MEAN rtc_obs_str_mean 10.75 rtd mean strehl ratio
RTC.OBS.STR.STD rtc_obs_str_std 0.88 rtd strehl ratio standard deviation
RTC.OBS.T0MEAN rtc_obs_t0mean 13.13 rtc mean correlation time [s]
RTC.OBS.T0STD rtc_obs_t0std 4.05 rtc std dev of correlation time [m]
RTC.OBS.WFEMEAN rtc_obs_wfemean 1.58 rtc mean wavefront error
RTC.OBS.WFESTD rtc_obs_wfestd 0.17 rtc std dev of wavefront error
QCsinfo_sci.py qc_nreal_det 1.64 number of sources detected (greater than 3sigma)
QCsinfo_sci.py qc_xpos 37.25 flux-weighted X-axis centroid
QCsinfo_sci.py qc_ypos 37.44 flux-weighted Y-axis centroid
QCsinfo_sci.py qc_flux 1.748e+04 total flux (in ADU) within 3 sigma aperture
QCsinfo_sci.py qc_iso_area 207.7 total aperture area over which flux is summed (pixels^2)
QCsinfo_sci.py qc_net_flux 64.76 net flux (in ADU): qc_flux/qc_iso_area
QCsinfo_sci.py qc_spectra_peak 329.8 mean flux of extracted spectrum at peak flux pixel
QCsinfo_sci.py qc_spectra_mean 200.3 average flux of extracted spectrum (mean in fwhm)
QCsinfo_sci.py qc_spectra_std 201.3 std dev of extracted spectrum mean flux level
QCsinfo_sci.py qc_posang -1.30 brightest source position angle (CCW along X-axis)
QCsinfo_sci.py qc_elong 1.10 brightest source elongation (A_image/B_image)
QCsinfo_sci.py qc_ellip 0.15 brightestsource ellipticity (1 - B_image/A_image)
QCsinfo_sci.py qc_fwhm_dimm 0.90 DIMM seeing corrected to observed airmass and IR bandpass (arcsec)
QCsinfo_sci.py qc_fwhm_sinfo 1.31 brightest source FWHM assuming a Gaussian core (arcsec)
QCsinfo_sci.py qc_delta_fwhm 0.41 difference (qc_fwhm_sinfo - qc_fwhm_dimm) (arcsec)
QCsinfo_sci.py qc_persist_danger 0 a test if source flux levels are too high (danger of persistence = 1; no danger = 0)
QCsinfo_sci.py qc_Npersist 0 total number of persistence critical pixels
QCsinfo_sci.py qc_temp_det -192 detector temperature (C)
QCsinfo_sci.py qc_temp_grat -195.4 grating housing temperature (C)
QCsinfo_sci.py qc_temp_ambi 10.43 ambient temperature (C)
QCsinfo_sci.py qc_delta_temp_det 0.002 difference between science data and wave detector temperature
QCsinfo_sci.py qc_delta_temp_grat -0.37 difference between science data and wave grating temperature
QCsinfo_sci.py qc_delta_time -0.24 delta days between science data and telluric STD observation
QCsinfo_sci.py qc_delta_am 0.00 delta airmass between science data (mid-OB value!) and the telluric STD observation
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_sci.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 STD exposure. The average of these two values is computed and converted to the
same airmass and wavelength as the respective telluric 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_sci.py).
Persistence test : the post-pipeline script (QCsinfo_persist.py) tests the OBJECT_NODDING_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.
- stars in sky frame
- strong skew of spectrum
Science OB down-graded:
- if observed source has saturated flux levels
- if strong persistence from previous science, PSF, or telluric STD star observations exists in current science frame
- if the difference in time between the science observation and its associated telluric standard star is greater than 1 day
- if the difference in airmass between the science observation and its associated telluric standard is greater than 1
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