SINFONI pipeline:
Calibration files and recipes

This page is a description of how SINFONI calibration data is processed.

Contents (click on the links to jump to the specific calibrations):

Day-time calibration

• DARK
• DISTORTION
• FLAT
• WAVE
• LINEARITY
  
  Night-time calibration
  
  
• STD
• PSF
  
  Static calibration
  
  
• 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

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 have been generated with pipeline version 2.0.8 (2009-09-15).

Purpose. Dark frames are obtained to monitor the technical performance of the detector, and to correct subsequent data for pixel-to-pixel dark current variations and pixels with very high dark currents (i.e. hot pixels). Darks generally come in stacks of 3 raw frames and are routinely measured during each night when SINFONI is operational. All raw darks of a given DIT are processed into master dark frames and hot pixel maps and are quality-checked on the mountain and by QC Garching. Since SINFONI darks are generally not stable, all master dark frames are stored in the calibration archive and individually delivered in the service mode packages recieved by the PI.

Input

Products.

QC parameters derived by the pipeline

Purpose. Distortion frames are obtained to monitor the optical distortion and the distances between the slitlets. They come in stacks of 79 raw frames consisting of:
75 north/south fibre images
2 flat lamp images (one each of lamp-on, lamp-off)
2 wavelength lamp calibrations (one each of lamp-on, lamp-off)

Distortions are made for all wavebands (J, H, K, and H+K) at the 25 mas pixel scale. They are routinely measured once per month and after each instrument intervention. They are all processed into DISTORTION and SLITLETS_DISTANCES product tables that 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 in the service mode packages recieved by the PI.

Input

Products.

QC parameters

Purpose. Linearity frames are created in order to monitor the response properties of the detector. They come in stacks of several pairs of lamp-on and lamp-off frames, spanning a range of detector DITs (usually 1 to 45 seconds). Linearities are made for all wavebands (J, H, K, and H+K) at the 25 mas pixel scale and are routinely measured approximately every 20 days and after every intervention. They are all processed into several coeffient frames and are quality-checked on the mountain and by QC Garching. All master master linearity cubes are stored in the calibration archive and individually delivered in the service mode packages recieved by the PI.

Input

Products.

QC parameters

Purpose. Flat frames are created to correct and monitor the pixel-to-pixel response properties of the detector. They come in stacks of several pairs of lamp-on and lamp-off frames. They are routinely measured and are 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 in the service mode packages recieved by the PI.

Input

Products

QC parameters

Purpose. Arc frames are created to derive 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 in the service mode packages recieved by the PI.

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