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Overview_IMG_LM_N.tex
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\subsection{Imaging in LM and N}
\label{ssec:overview_lm_imaging}
% HB 20230731: This note is not really necessary I think.
%\textbf{Note: The pipeline layout has been modified compared to the
% PDR design in order to achieve better modularity. Basic reduction
% and background subtraction have been split into two recipes that now
% are applied to both standard calibration and science data. ADI recipes have been added since PDR however integration of \ac{HCI}
% into this workflow requires more work: \ac{HCI} images will be treated
% the same way at least through basic reduction, possibly through
% background subtraction. \ac{ADI} combination may require a separate
% recipe, at least for some \ac{HCI} configurations.}
The purpose of the pipeline is to correct or remove contributions from
the instrument, telescope, and atmosphere and produce science-grade
data products. In the case of the METIS imaging modes the main
contributions to correct or remove are dark current, flatfield, bad
pixels, and, most importantly, thermal background emission from the
sky and the telescope. Further effects include persistence,
cross-talk, geometric distortions, etc. The final product of the
imaging pipeline is one or more image(s) that are flux-calibrated in units of
photons/s/pixel against a standard star.
Several images can be stacked into a single possibly mosaiced image.
Due to the differences in characteristics between the HAWAII2RG
detector used for imaging in the L and M bands and the GeoSnap
detector used for the N band, the operational concept for the two
imager subsystems are quite different. This induces differences in the
way the data have to be reduced.
The GeoSnap detector has more stable gain than AQUARIUS detector,
which was still in the baseline at PDR\@. Chopping is still necessary, albeit
at a lower frequency of a few Hz, and a chop/nod technique, which meets the
specific ELT requirements (Section~\ref{sssec:nbandsbackgroundsubtracion}),
will be employed for background subtraction. As the dark
signal is automatically removed when the exposures from the different
chop and nod positions are combined no master dark is required for the
reduction of science data. The GeoSnap data is also flat fielded.
Observations and reduction of LM band data with the HAWAII2RG detector
can proceed as in the near infrared. After dark subtraction and
flat-fielding, the background is estimated from a series of dithered
science exposures or from exposures on a nearby blank patch of sky.
The association maps for the current designs of the imaging pipelines
in~LM and~N are shown in Figs.~\ref{fig:IMG_LM_Assomap}
and~\ref{fig:IMG_N_Assomap}, respectively.
%\TODO{For \ac{HCI} data, \ac{ADI} may need to be part of reduction recipe if
% individual background subtracted images are the goal?} We provide ADI recipes since PDR.
\newgeometry{bottom=0.1cm, top=0.1cm}
\begin{landscape}
\begin{figure}
\centering
\resizebox{\linewidth}{!}{\input{tikz/IMG_LM_assomap_tikz.tex}}
\caption[Reduction cascade and association map for imaging in L and
M]{Association map for imaging in the LM band. The figure shows only
the primary product created from each recipe; for a full list of
products refer to the recipe descriptions in
Sect.~\ref{ssec:recipes_img_lm}. The dashed line separates
calibration tasks that are done at AIT or infrequently during
operations (left) from daily tasks (right).}
\label{fig:IMG_LM_Assomap}
\end{figure}
\end{landscape}
\begin{landscape}
\begin{figure}
\centering
\resizebox{\linewidth}{!}{\input{tikz/IMG_N_assomap_tikz.tex}}
\caption[Reduction cascade and association map for imaging in N]{%
Association map for imaging in the N band. The figure shows
only the primary product created from each recipe; for a full
list of products refer to the recipe descriptions in
Sect.~\ref{ssec:recipes_img_n}. The dashed line separates
calibration tasks that are done at AIT or infrequently during
operations (left) from daily tasks (right).}
\label{fig:IMG_N_Assomap}
\end{figure}
\end{landscape}
\restoregeometry
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