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VISIR pipeline:
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Calibration data and recipes

Dark frames

TPL.IDVISIR_img_cal_Darks
VISIR_spec_cal_Darks
DPR.CATG CALIB
DPR.TECH IMAGE
SPECTRUM
DPR.TYPE DARK
TAGIM_CAL_DARK
SPEC_CAL_DARK
groupingINS.FILT1.NAME INS.PFOV
INS.FILT2.NAME, INS.GRAT1.NAME. INS.RESOL, INS.SLIT1.WID
recipe/callesorex visir_img_dark sof

[visir_dark_img.png  11K]
raw dark frame of the imaging detector
[visir_dark_spc.png  11K]
raw dark frame of the spectroscopic detector

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.

Products

PRO.CATGcontents
IMG_DARK_AVG, SPEC_DARK_AVGaverage of input raw frames
IMG_DARK_COLD, SPEC_DARK_COLDcold pixel map
IMG_DARK_HOT, SPEC_DARK_HOThot pixel map
IMG_DARK_DEV, SPEC_DARK_DEVdeviant pixel map

QC parameters

QC.RON Number of bad pixels
QC.RON1 Readout noise from 2 first raw frames
QC.RON2 Redaout noise from 2 last raw frames
QC.DARKMED Median value of the dark current
QC.NBCOLPIX Number of cold pixels
QC.NBHOTPIX Number of hot pixels
QC.NBDEVPIX Number of deviant pixels

 


Flat field frames

TPL.IDVISIR_img_cal_ExtrSrcFlats
VISIR_spec_cal_ExtrSrcFlats
DPR.CATG CALIB
DPR.TECH IMAGE,DIRECT
SPECTRUM,DIRECT
DPR.TYPE FLAT
TAGIM_CAL_FLAT
SPEC_CAL_FLAT
groupingINS.FILT1.NAME INS.PFOV
INS.FILT2.NAME, INS.GRAT1.NAME. INS.RESOL, INS.SLIT1.WID
recipe/callesorex visir_img_ff sof

[visir_flat_raw2_img.png 11K]
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.

Products

PRO.CATGcontents
IMG_FF, SPEC_FFaverage of seven raw frames
IMG_BPM, SPEC_BPMbad pixel map

QC parameters

QC.NBBADPIX Number of bad pixels

 


Imaging standard star frames

TPL.IDVISIR_img_cal_AutoChopNod
DPR.CATG CALIB
DPR.TECH IMAGE,CHOPNOD
DPR.TYPE STD
TAGIM_CAL_PHOT
IMG_STD_CATALOG (additional static calib.)
groupingINS.FILT1.NAME INS.PFOV
recipe/callesorex visir_img_phot sof

[visir_std_imgraw.png 11K]
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.

Products

PRO.CATGcontents
IMG_PHOT_COMBINEDcombined image
IMG_PHOT_CONTRIB_MAPimage contribution map

QC parameters

QC.BACKGD.MEANestimated mean of the background
QC.BACKGD.SIGMAestimated sigma of the background
QC.FLUXTOTtotal measured flux of the star
QC.FLUXSNR flux of the star for the best Signal/Noise ratio
QC.FLUXSNR.NOISEnoise for the best Signal/Noise ratio
QC.FWHMXFWHM in x
QC.FWHMY FWHM in y
QC.FWHMX.POS1FWHM in x of the first positive star
QC.FWHMY.POS1FWHM in y of the first positive star
QC.FWHMX.POS2FWHM in x of the second positive star
QC.FWHMY.POS2FWHM in y of the second positive star
QC.FWHMX.NEG1FWHM in x of the first negative star
QC.FWHMY.NEG1FWHM in y of the first negative star
QC.FWHMX.NEG2FWHM in x of the second negative star
QC.FWHMY.NEG2FWHM in y of the second negative star
QC.SENSITsensitivity (mJy/10sigma/1hr)
QC.CONVERconversion factor (ADU/Jy)
QC.STREHL strehl ratio
QC.STREHL.ERRORerror of the strehl ratio

 


LR/MR/HR-slit spectroscopic standard star frames

TPL.IDVISIR_spec_cal_LRAutoChopNod
DPR.CATG CALIB
DPR.TECH SPECTRUM,CHOPNOD
DPR.TYPE STD
TAGSPEC_CAL_PHOT
SPEC_STD_CATALOG (additional static calib.)
SPEC_CAL_LINES (additional static calib.)
SPEC_STD_QEFF (additional static calib.)
groupingINS.FILT2.NAME, INS.GRAT1.NAME. INS.RESOL, INS.SLIT1.WID
recipe/callesorex visir_spc_phot sof

[visir_std_spcraw.png 11K]
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.CATGcontents
SPC_PHOT_COMBINEDcombined spectrum
SPC_PHOT_TAB extracted spectrum as a table
SPC_PHOT_WEIGHTweight map

QC parameters

QC.BACKGD.MEANestimated mean of the background
QC.XCcross-correlation of the observed v. model sky spectr.
QC.XCSHIFTshift (pix) of model spectr.
QC.PHDEGREEdegree of the model dispersion polynomial
QC.PHDISPX1
QC.PHDISPX0
QC.XCWLENcalibrated central wavelength
QC.XCDEGREEdegree of the calibrated dispersion polynomial
QC.XCDISPX1
QC.XCDISPX0
QC.XFWHMFWHM at XCENTROI
QC.XCENTROIx-centroid of the spectr. brightest object
QC.SENS.MEAN mean of the spectroscopic sensitivities
QC.SENS.STDEVstandard deviation of spectroscopic sensitivities

 


Echelle spectroscopic standard star frames

TPL.IDVISIR_spec_cal_HRXAutoChopNod
DPR.CATG CALIB
DPR.TECH ECHELLE
DPR.TYPE STD
TAGSPEC_CAL_PHOT_HRG
SPEC_STD_CATALOG (additional static calib.)
SPEC_CAL_LINES (additional static calib.)
SPEC_STD_QEFF (additional static calib.)
groupingINS.FILT2.NAME, INS.GRAT1.NAME. INS.RESOL, INS.SLIT1.WID
recipe/callesorex visir_spc_phot_ech sof

[visir_std_echraw.png 11K]
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.CATGcontents
SPC_PHOT_HRG_COMBINEDcombined spectrum
SPC_PHOT_HRG_TAB extracted spectrum as a table
SPC_PHOT_HRG_WEIGHTweight map

QC parameters

QC.BACKGD.MEANestimated mean of the background
QC.XCcross-correlation of the observed v. model sky spectr.
QC.XCSHIFTshift (pix) of model spectr.
QC.PHDEGREEdegree of the model dispersion polynomial
QC.PHDISPX1
QC.PHDISPX0
QC.XCWLENcalibrated central wavelength
QC.XCDEGREEdegree of the calibrated dispersion polynomial
QC.XCDISPX1
QC.XCDISPX0
QC.XFWHMFWHM at XCENTROI
QC.XCENTROIx-centroid of the spectr. brightest object
QC.SENS.MEAN mean of the spectroscopic sensitivities
QC.SENS.STDEVstandard deviation of spectroscopic sensitivities

 
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