Purpose. Dark frames are
measured to monitor the performance of the detectors - the dark
current and the read-out-noise. In general they come in stacks of 3
raw frames for each detector and are taken daily in defined
instrumental setups: imaging - INS.FILT1.NAME=CLOSE, INS.PFOV=0,127,
spectroscopy - INS.FILT2.NAME=N_SW, INS.GRAT1.NAME=GUMRSW,
INS.RESOL=MR, INS.SLIT1.WID=1.
Recipe. The dark frames are processed into master
dark product using visir_img_dark pipeline recipe and quality-checked by QC Garching.
QC checks. The QC parameters monitored are the dark
current and the read-out-noise. Also, detectors' temperatures
are read from the headers of the dark frames. The values of
the qc1 parameters are accessible
via trending page.
raw frame of the flat field for the imaging detector
Purpose. Flatfield frames
are measured to monitor the technical performance of the imaging
and spectroscopic detectors of VISIR. So far, they have not been
meant to calibrate science data. The flatfield calibrations are
used to monitor the gain, number of bad pixels, the bad pixel
map, and to derive the Fixed Pattern Noise. They come in stacks
of 7 raw frames (or less), where each frame corresponds to
exposure with different temperature of the Warm Calibration Unit
in the Extended Source mode. The temperature changes from -40 C
to 20 C with 10 C step. The imaging detector flat field is taken daily during
day-time calibrations in defined instrumental setup -
INS.FILT1.NAME=PAH1, INS.PFOV=0,127.
Recipe. The flat field frames are processed into master
flat product using visir_img_ff pipeline recipe and quality-checked by QC Garching.
QC checks. The QC parameter monitored is the namber of bad pixels.
The values of
the qc1 parameters are accessible
via trending page.
raw frame of the imaging standard star; It is completely dominated by the thermal background radiation; You can only see the target by subtracting chopped/nodded raw frames from each other
Purpose. Imaging standard
star frames are measured to obtain flux calibration and to
monitor instrument response, ambient conditions, background,
etc. They are quality-checked by QC Garching. All master
calibrations are stored in the calibration database.
Recipe. The imaging standard star frames are processed
using visir_img_phot pipeline recipe and quality-checked by QC Garching.
QC checks. The QC parameters monitored are
sensitivity, conversion factor and mean of the sky
background. The values of the qc1 parameters are accessible
via trending
page.
raw frame of the LR spectroscopic standard star; It is completely dominated by the thermal background radiation; You can only see the spectrum by subtracting chopped/nodded raw frames from each other
Purpose. Spectroscopic
standard star frames are measured to obtain constraints on the
flux/wavelength calibration and to monitor instrument response,
ambient conditions, background, etc. They are quality-checked by QC Garching. All master calibrations are stored in the calibration database.
Recipe. The spectroscopic standard star frames are processed
using visir_spc_phot pipeline recipe and quality-checked by QC Garching.
QC checks. Currently, none of the QC parameters inferred from
the spectroscopic star observations are monitored.
Products
PRO.CATG
contents
SPC_PHOT_COMBINED
combined spectrum
SPC_PHOT_TAB
extracted spectrum as a table
SPC_PHOT_WEIGHT
weight map
QC parameters
QC.BACKGD.MEAN
estimated mean of the background
QC.XC
cross-correlation of the observed v. model sky spectr.
raw frame of the echelle spectroscopy standard star
Purpose. Echelle standard
star frames are measured to obtain constraints on the flux/wavelength
calibration. They are quality-checked by QC Garching. All master
calibrations are stored in the calibration database.
Recipe. The echelle standard star frames are processed
using visir_spc_phot_ech pipeline recipe and quality-checked by QC Garching.
QC checks. Currently, none of the QC parameters inferred from
the echelle star observations are monitored.
Products
PRO.CATG
contents
SPC_PHOT_HRG_COMBINED
combined spectrum
SPC_PHOT_HRG_TAB
extracted spectrum as a table
SPC_PHOT_HRG_WEIGHT
weight map
QC parameters
QC.BACKGD.MEAN
estimated mean of the background
QC.XC
cross-correlation of the observed v. model sky spectr.