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VISIR:
VISIR calibration files and recipes |
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VISIR calibration files and
recipes
This page describes processing techniques of the
VISIR calibration data.
More information is given in the following sites:
FLAT
Purpose. These flatfield frames are measured to monitor
the technical performance of the imaging and spectroscopic detectors of VISIR.
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, 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.
They are routinely measured every morning when
VISIR is operational. They are all processed into master Flat frames and quality-checked
on the mountain and by QC Garching. They are not stable, hence all master Flat
frames are stored in the calibration archive and individually delivered.
Input
| TPL.ID | VISIR_img_cal_ExtSrcFlats, VISIR_spec_cal_ExtSrcFlats | | DPR.TYPE
| FLAT | | TAG | IM_CAL_FLAT, SPEC_CAL_FLAT | | grouping | | | recipe/call | esorex
visir_img_ff sof, esorex visir_spc_ff sof |
|
Products
| PRO.CATG | contents |
| IMG_FF, SPEC_FF | average
of seven raw frames |
| IMG_BPM, SPEC_BPM | bad pixel map | |
QC parameters
| QC.NBBADPIX | Number of bad pixels |
|
Imaging STD
Purpose. Imaging standard star
frames are measured to obtain flux calibration and to monitor instrument response, ambient conditions, background , etc.
They are quality-checked on the mountain and
by QC Garching. All master calibrations are stored in
the calibration archive and individually delivered.
Input
| TPL.ID | VISIR_img_cal_AutoChopNod | | DPR.TYPE | STD |
| TAG | IM_CAL_PHOT |
| TAG | IMG_STD_CATALOG |
| grouping | |
| recipe/call | esorex
visir_img_phot sof |
|
Products
| PRO.CATG | contents |
| IMG_PHOT_COMBINED | combined image |
| IMG_PHOT_CONTRIB_MAP | image contribution map |
|
QC parameters
| QC.BACKGD.MEAN | |
| QC.BACKGD.SIGMA | |
| QC.FLUXTOT | |
| QC.FLUXSNR | |
| QC.FLUXSNR.NOISE | |
| QC.FWHMX | |
| QC.FWHMY | |
| QC.FWHMX.POS1 | |
| QC.FWHMY.POS1 | |
| QC.FWHMX.POS2 | |
| QC.FWHMY.POS2 | |
| QC.FWHMX.NEG1 | |
| QC.FWHMY.NEG1 | |
| QC.FWHMX.NEG2 | |
| QC.FWHMY.NEG2 | |
| QC.SENSIT | |
| QC.CONVER | |
| QC.STREHL | |
| QC.STREHL.ERROR | |
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Telluric STD
Purpose. Telluric
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 on the
mountain and by QC Garching. All master calibrations are stored in the
calibration archive and individually delivered.
Input
| TPL.ID | VISIR_spec_cal_LRAutoChopNod | | DPR.TYPE | STD |
| TAG | SPEC_CAL_PHOT |
| TAG | SPEC_STD_CATALOG |
| TAG | SPEC_CAL_LINES |
| TAG | SPEC_STD_QEFF |
| grouping | |
| recipe/call | esorex
visir_spc_phot sof |
|
Products
| PRO.CATG | contents |
| SPC_PHOT_COMBINED | combined spectrum |
| SPC_PHOT_TAB | table |
| SPC_PHOT_WEIGHT | weight map |
|
QC parameters
| QC.BACKGD.MEAN | |
| QC.XC | |
| QC.XCWLEN | |
| QC.XCSHIFT | |
| QC.PHDEGREE | |
| QC.PHDISPX1 | |
| QC.PHDISPX0 | |
| QC.XCDEGREE | |
| QC.XCDISPX1 | |
| QC.XCDISPX0 | |
| QC.XFWHM | |
| QC.XCENTROI | |
| QC.SENS.MEAN | |
| QC.SENS.STDEV | |
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Static
calibrations
| PRO.CATG | description | downloads | | | tables
with the arc line positions and scaled arc line intensity | |
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Last update: March 21, 2005
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