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The reduction of UVES data at QC Garching is done in a semi-automatic
manner: raw data are selected and inserted into a reduction
mechanism which produces
This mechanism is the UVES reduction pipeline.
The UVES pipeline Data Reduction Software
(DRS) has been implemented around the UVES context of MIDAS
(which is an evolved version of the ECHELLE context). It is
designed to automatically reduce point source object spectra
from raw frames to order extraction and final order merging.
The UVES pipeline is exportable. Find details
about ordering, downloads etc. here.
Find here a Users'
Manual. Find general information about ESO reduction pipelines
here.
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CALIBRATION,
REDUCTION |
UVES pipeline |
calibration
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science reduction
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recipes calib
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recipe
science |
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Find the description of calibration processing, science reduction
and recipes here.
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OPERATIONS |
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There are two instances of the UVES reduction pipeline:
- at the KUEYEN telescope on Paranal, running in automatic
mode,
- at HQ Garching run by the Quality Control Team in the
optimized mode.
The automatic mode is used for quick look purposes
and for on-site quality control. It processes all raw data
sequentially, i.e. as they arrive from the instrument. It
produces calibration products and reduced science data, but
will usually fail to obtain the best possible results.
It provides results for all standard and many non-standard
UVES settings.
The optimized mode is the mode, which becomes possible
when all data of a night have been collected, including the
daytime calibrations. Then the calibration data are sorted
and assessed independently of their timestamp. The best possible
master calibration data are created. Their quality is checked.
They are finally applied to the science data of a night. This
is the way all calibration data in supported modes are reduced
by QC Garching, as are all science data from Service Mode
programmes.
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SUPPORTED
MODES AND SETTINGS
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The UVES pipelines installed in Garching and on Paranal
support all four flavours of UVES SCIENCE data:
"ECHELLE", "ECHELLE,ABSORPTION-CELL", "ECHELLE,SLICER", and
"ECHELLE,ABSORPTION-CELL,SLICER". "ECHELLE" and
"ECHELLE,ABSORPTION-CELL" observations are reduced using
optimum extraction, "ECHELLE,SLICER" and
"ECHELLE,ABSORPTION-CELL,SLICER" with average extraction.
QC Garching processes the following UVES data:
- all calibration data taken in UVES standard settings,
no matter whether Service or Visitor Mode;
- all science data taken in UVES standard settings taken
in Service Mode. Since Period 70, this includes also
image slicer data.
The quick-look pipeline on Paranal processes any kind of
UVES data.
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FUNCTIONALITIES |
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The main functionalities of the UVES pipeline are:
- create master calibration data,
- reduce science frames,
- provide QC1 parameters.
QC Garching creates
- master
calibration data from raw calibration data taken in
standard settings, both for Visitor Mode and Service
Mode nights. The raw data are stored in the ESO Archive
and are public. They are assessed and selected in terms
of their quality and used for QC1 checks and trending;
- reduced
science data for Service Mode nights. For SM
programmes, QC Garching runs the pipeline on all science
raw data taken in UVES echelle standard settings, using
the best available, quality-checked master calibration data.
UVES SCIENCE data have been processed by the
pipeline
with the best available calibration data. Please note
that ESO is not assuming any responsibility in respect
to the usefulness of the reduced data.
The adopted reduction strategy may not be suitable
for the scientific purpose
of the observations.
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SERVICE
MODE PACKAGE |
SM
package |
Programmes performed in Service Mode receive a set of CD ROMs
(or DVDs) which contains
- all raw science data,
- reduced science data,
- suitable calibration data (both raw and master),
- listings and logs,
- QC1 reports.
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FILE
FORMAT |
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Raw UVES frames come in the following CCD formats :
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blue arm (1 CCD) |
red arm (2 CCDs) |
format (X,Y),
1x1 binning |
2148 x 3000 px
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4296x4096 px
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pre/overscan |
2x50 = 100 px
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4x50 = 200 px
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Apart from 1x1 binning, there is also 1x2, 2x2 and 2x3 binning
possible. Remember that pipeline processing is only done on
1x1 and 2x2 binnings.
CCD formats are described here.
Master calibration files (master BIAS, master FLAT) have
the prescan and overscan regions chopped off. Master files
for the red arm come in twins for either of the red CCD. Usually
the CCDs are called BLUE, REDU = red upper, and REDL = red
lower. All master files are rotated by 90 degrees. The red
masters are in addition flipped. Blue 1x1 binning master files
have the format 3000x2048 px, red master files 4096x2048 px.
For 2x2 binings, divide these numbers by 2.
Raw calibration files, raw science files, and master calibration
files, have the following approximate sizes in MB:
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raw BLUE |
raw RED
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1x1 |
12,6
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34,4
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2x2 |
3.2
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8.6
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master BLUE |
master REDU |
master REDL |
1x1 |
24.0
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32.8
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32.8
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2x2 |
6.0
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8.2
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8.2
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