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.
Input:
TPL.ID
SINFONI_ifs_cal_Darks
DPR.TYPE
DARK
TAG
DARK RAW
grouping
DET.DIT
recipe/call
esorex sinfo_rec_mdark sof
Products:
PRO.CATG
contents
MASTER_DARK
average of three raw frames (used in cascade)
BP_MAP_HP
hot (high dark current) pixel map
QC parameters derived by the pipeline:
QC.DARKMED.AVE
average of the median dark current measured in each of 3 raw darks
QC.DARKMED.STDEV
standard deviation of dark current in 3 raw dark frame medians
QC.DARK.FPN
windowed and non-robust scatter in a area on the chip
QC.RON.RMS
scatter in Fixed-Pattern-Noise
QC.RON1
RON of first consecutive pair of raw frames (raw2-raw1)
QC.RON2
RON of second consecutive pair of raw frames (raw3-raw2)
QC.BP_MAP.BADPIX
number of bad (hot) pixel
QC.DARK.FPN
windowed and non-robust scatter in a area on the chip
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.
Input:
TPL.ID
SINFONI_ifs_tec_NorthSouth
DPR.TYPE (75 frames)
DISTORTION,FIBRE,NS
DPR.TYPE (2 frames)
DISTORTION,FLAT,LAMP
DPR.TYPE (2 frames)
DISTORTION,FLAT,WAVE
TAG
DISTORTION_FIBRE_NS
TAG
DISTORTION_FLAT_LAMP
TAG
DISTORTION_FLAT_WAVE
grouping
INS.SETUP.ID : S1_J, S2_H, S3_K, S4_H+K
recipe/call
esorex sinfo_rec_distortion sof
Products:
PRO.CATG
contents
used further in cascade
DISTORTION
table with polynomial distortion coefficients
YES
SLITLETS_DISTANCE
table with slitlet positions
YES
WAVE_LAMP_STACKED
arc lamp used to located edges of slitlets
NO
MASTER_FLAT_LAMP
master flat (only used to flat-field distortions)
NO
BP_MAP_DIST
bad pixel map from raw flats
YES
FIBRE_NS_STACKED
stacked fibre lamp-on minus stacked fibre lamp-off frames
NO
FIBRE_NS_STACKED_ON
stacked fibre lamp-on frames
NO
FIBRE_NS_STACKED_OFF
stacked fibre lamp-off frames
NO
FIBRE_NS_STACKED_DIST
undistorted stack of fibre lamp-on minus fibre lamp-off frames
NO
QC parameters
QC.COEFF00 .. QC.COEFF12
Polynomial distortion coefficients
QC.XSHIFT.UL
x-shift of the upper left quadrant center (512,1536)
QC.XSHIFT.UR
x-shift of the upper right quadrant center (1536,1536)
QC.XSHIFT.LL
x-shift of the lower left quadrant center (512,512)
QC.XSHIFT.LR
x-shift of the lower right quadrant center (1536,512)
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.
Input:
TPL.ID
SINFONI_ifs_tec_LinDet
DPR.TYPE (24 frames)
LINEARITY,LAMP
TAG
LINEARITY_LAMP RAW
grouping
INS.SETUP.ID : S1_J, S2_H, S3_K, S4_H+K
recipe/call
esorex sinfo_rec_detlin sof
Products:
PRO.CATG
contents
BP_COEFFS
a cube with each plane a different linearity coefficient: plane[0], plane[1], plane[2]
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.
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.
Input:
TPL.ID
SINFONI_ifs_cal_Arcs
DPR.TYPE (3 on/off pairs)
FLAT,WAVE
TAG
WAVE_LAMP RAW
grouping
INS.SETUP.ID : S1_J, S2_H, S3_K, S4_H+K
grouping
INS.OPTI1.NAME : 0.025, 0.1, 0.25
required master calibrations
SLITLETS_DISTANCE (from distortion)
required master calibrations
DISTORTION (from distortion)
required master calibrations
REF_TABLE (static calibration)
required master calibrations
MASTER_FLAT_LAMP (from mflats)
required master calibrations
MASTER_BP_MAP (from mflats)
required master calibrations
SLIT_POS (will maybe disappear)
recipe/call
esorex sinfo_rec_wavecal sof
Products:
PRO.CATG
contents
WAVE_MAP
wavelength solution per column (used for cascade)
SLIT_POS
table with 32 slit-begin slit-end numbers (used for cascade)
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:
TPL.ID
SINFONI_ifs_cal_StandardStar
DPR.TYPE (usually 1)
STD and SKY,STD
TAG
STD
TAG
SKY_STD
grouping
INS.SETUP.ID : S1_J, S2_H, S3_K, S4_H+K
grouping
INS.OPTI1.NAME : 0.025, 0.1, 0.25
required master calibrations
SLITLETS_DISTANCE (from distortion)
required master calibrations
DISTORTION (from distortion)
required master calibrations
MASTER_FLAT_LAMP (from mflats)
required master calibrations
MASTER_BP_MAP (from mflats)
required master calibrations
SLIT_POS (from wavecal)
required master calibrations
FIRST_COL (static calibration)
required master calibrations
WAVE_MAP (from wavecal)
required master calibrations
ATM_REF_CORR (static calibration)
recipe/call
esorex sinfo_rec_jitter sof
Products:
PRO.CATG
contents
COADD_STD
cube, coadded from jittered cubes, plane50, plane512, plane1024, plane1536, plane2120
MASK_COADD_STD
cube with weight factors
OBS_STD
N object cubes before being co-added
STD_NODDING_STACKED
N stacked object frames before being 'cubed'
MED_COADD_STD
median collapsed COADD_STD
STD_STAR_SPECTRA
table with extracted spectrum and response function
STD_STAR_SPECTRUM
extracted spectrum in fits format
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)
mirror sites:
PL (internal link)
HQ
[?]
Distortion recipe
