ESO
SINFONI Pipeline User Manual
Doc:
VLT-MAN-ESO-19500-3600
Issue:
Issue 1.0
Date:
Date 2005-10-19
Page:
83 of 88
If a wavelength map is available (wavecal.wave_map_ind==TRUE) and a dispersion relation does not
need to be found (wavecal.calib_ind==0) one may want to correct what is already available to match the
actual arc lamp frame, by creating a shifted dispersion relation. Then the overall line shift between the
solution found from the fit and the position of the lines in the frame is computed.
Finally if wavecal.calib_indicator==TRUE and wavecal.estimate_indicator==TRUE the slitlet posi-
tions are fit using a parameter list input FITS table. The slitlet position determination may follow either
the Boltzmann or the estimate methods as described in 10.1.12.
10.2.6
Science observations: si_rec_objnod
The input frames are selected defining obj-sky pairs. In case a sky frame is missing in the set of frames a
sky frame is estimated as described in 10.1.16. Each pair is stacked.
Each stacked frame is resampled using the information from the input calibration image (WAVE_MAP)
doing a polynomial interpolation with objnod.n_coeffs parameters to generate an output 3D frame as
described in 10.1.14. This operation determines the dispersion, the minimum, the maximum and the
central wavelength as well as the central pixel of the output calibrated image.
If objnod.north_south_ind == FALSE, a 3D frame is reconstructed from each stacked frame by using
the information contained in the slitlet position table SLIT_POS.
The 3D frame is refined using different methods (objnod.fine_tuning_method). Possible values are P
(polynomial of order objnod.order), S (Spline). The 3D frame is stretched in Y to make it appear as a
parallepipedus with a square cross-section. We usually call this a “3D cube”.
If objnod.jitter_index==TRUE, finally all the cubes corresponding to the different object jittered po-
sitions are merged into a big data cube by averaging the overlap regions weighted by integration times
and using a given kernel type objnod.kernel_type as described in 10.1.15 possibly scaling the sky back-
ground (if objnod.scale_sky == TRUE) and doing a kappa sigma clipping (if objnod.kappa_sigma ==
TRUE) of intensity outliers.
10.2.7
STD star data reduction: si_rec_stdstar
The initial data reduction is the same as the one of a normal science frame (si_rec_objnod). Then:
The position of the source maximum, its centroid and FWHM, are determined from the average im-
age of the coadded cube. Those parameters are used to automatically set the optimal extraction pa-
rameters in a square region whose size depends on the average of the FWHM in the X and Y direc-
tions and a user definable scale parameter std_star.factor, eventually reduced in case the star position
falls outside the actual z-cross section plane. The output is in the form of an image and a table. If
std_star.conversion_index==TRUE a conversion magnitude to counts/seconds is performed.
The instrument efficiency is determined as described in 10.1.17.
The extracted star spectrum and the efficiency are saved in a table.
