SINFONI: SINFONI calibration files and recipes
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SINFONI calibration files and recipes

On this page we inform how SINFONI calibration data are processed.

Contents:

Day-time calibration

• DARK
• DISTORTION
• FLAT
• WAVE
• LINEARITY
  
  Night-time calibration
  Source on the sky required
  
  
• STD
• PSF
  
  Static calibration
  Source on the sky required
  
  
• first column
• static bad pixel map
• arc reference tables
• drs-setup-wave

More information is given in the following pages

• SINFONI calibration
• SINFONI User Manual
• SINFONI reference frames
• SINFONI QC1 parameter database (not yet)

This page describes the individual recipe calls, the required raw input data and products as they are used by the pipeline in Garching. The example products are mostly generated with pipeline version 1.0.5 (2005-05-24).

Purpose. Dark frames are measured to monitor the technical performance of the detector. They are also used to correct the pixel-to-pixel dark current variations,in particular those pixels with a very high dark current. They come in stacks of 3 raw frames. They are routinely measured every night when SINFONI is operational. They are all processed into master Dark frames and quality-checked on the mountain and by QC Garching. They are not stable, hence all master dark frames are stored in the calibration archive and individually delivered.

Input

Products.

QC parameters

Purpose. Distortion frames are measured to monitor the optical distortion and the distnaces between the slitlets. They come in stacks of 88 raw frames of different DPR.TYPE. They are routinely measured after every interventionl. They are all processed into DISTORTION and SLITLETS_DISTANCES product tables. They are quality-checked on the mountain and by QC Garching. All master master distortion and slitlet tables are stored in the calibration archive and individually delivered.

Input

Products.

QC parameters

Purpose. Linearity frames are to monitor the response properties of the detector. They come in stacks of several pairs of lamp-on and lamp-off frames. They are routinely measured after every intervention. They are all processed into a several coeffient frames. They are quality-checked on the mountain and by QC Garching. All master master linearity cubes are stored in the calibration archive and individually delivered.

Input

Products.

QC parameters

Purpose. Flat frames are to monitor the pixel-topixel response properties of the detector. They come in stacks of several pairs of lamp-on and lamp-off frames. They are routinely measured. They are all processed into a master bad pixel map and a master flat. They are quality-checked on the mountain and by QC Garching. All master master linearity cubes are stored in the calibration archive and individually delivered.

Input

Products

QC parameters

Purpose. Arc frames are to monitor the wavelength solution and calibrate the observations. They come in stacks of several pairs of lamp-on and lamp-off frames. They are routinely measured every morning. They are all processed into a several product frames. They are quality-checked on the mountain and by QC Garching. All master wavelength calibration products are stored in the calibration archive and individually delivered.

Input

Products.

QC parameters

Purpose. Telluric Standard stars are taken to provide a telluric absorption template on top of a bright spectrum of a star with negligible stellar features. Science spectra are not corrected for telluric absorption features

Input

Products.

The columns of the PRO.CATG=STD_STAR_SPECTRA products are:
wavelength : in micron

• counts_tot: the sum of all counts in a given area of each plane of the COADD_STD cube. The area over which all counts are summed is given by the central position of the source plus minus a factor times the FWHM of the Gaussian fit. The default factor is 5, but can be modified in the sinfo_rec_jitter.rc file (generated via esorex --create-config sinfo_rec_jitter). The corresponding command line paramter is --std_star-fwhm_fct). The resulting number of counts are per DIT (not per sec).
• bkg_tot: the background in counts as derived by a 2D-Gaussian fit to the expected single object in the FOV in the given plane. When the FWHM of the standard star is very large and becomes comparable with the small size of the FOV (dependent on the used camera 0.025, 0.1 or 0.250) the sky estimation might become false. The pipeline checks this case and returns extra information in the recipe log (see pipeline manual for details).
• counts_bkg: = counts_tot minus bkg_tot, hence this column gives the total counts per DIT of the source. No assumptions on the PSF of the objects are applied. No special extraction algorithm is applied.
• bb_flux_norm: Using the filter (lambda_c) and the MK type (Teff) of the standard star, get the ratio flux ratio between a black body at lambda and Teff and a reference black body at lambda_c and 10000K.
• efficiency: a) convert the flux on the detector in erg/s/cm/cm/A units; b) scale the bb_flux_norm to the flux of a 0th magnitude star in the given band; c) devide result of a) by result of b).
  

The PRO.CATG=CONVFACTOR is contains only the Mag per counts/sec

the function determines an intensity conversion factor for the instrument
by fitting a 2D-Gaussian to an collapsed image of a standard star
with known brightness (only for non-AO observations).
Then the resulting Gaussian is integrated and the counts
are divided by the exposure time (Fits header information)

factor = mag / (float)sum * exptime ;

QC parameters

PSF

Purpose. Arc frames are to monitor the wavelength solution and calibrate the observations. They come in stacks of several pairs of lamp-on and lamp-off frames. They are routinely measured every morning. They are all processed into a several product frames. They are quality-checked on the mountain and by QC Garching. All master wavelength calibration products are stored in the calibration archive and individually delivered.

Input

Products.

QC parameters

Send comments to <Mark.Neeser@eso.org>  Last update: June 1, 2006