Changeset 41238 for trunk

Timestamp:

Jan 28, 2020, 12:00:34 PM (6 years ago)

Author:

eugene

Message:

mark modified text for journal

Location:

trunk/doc/release.2015/ps1.detrend

Files:

• Makefile (modified) (2 diffs)
• detrend.tex (modified) (10 diffs)

trunk/doc/release.2015/ps1.detrend/Makefile

@@ -44 +44 @@
 images/stack_3956997_num.png \
 images/stack_3956997_exp.png \
-images/stack_3956997_expwt.png
+images/stack_3956997_expwt.png \
+images/warp.and.stack.demo.pdf
 
 APICS = \
@@ -73 +74 @@
 images/stack_3956997_num_sm.png \
 images/stack_3956997_exp_sm.png \
-images/stack_3956997_expwt_sm.png
+images/stack_3956997_expwt_sm.png \
+images/warp.and.stack.demo.pdf
 
 FILES = \

trunk/doc/release.2015/ps1.detrend/detrend.tex

@@ -30 +30 @@
 % \def\plotopt{_mt}
 
+%% set to '.' for the journal and arxiv versions:
 % use this to make the figure picture path flexible:
-\def\picdir{images}
-% \def\picdir{.}
+% \def\picdir{images}
+\def\picdir{.}
 
 % CZW commands from my previous draft.
@@ -254 +255 @@
 will be made available in a future data release.
 
-In this article, we use the following type-faces to distinguish
-different concepts:
+\textadd{In this article, we use the following type-faces to distinguish
+different concepts:}
 \begin{itemize}
 \item \ippstage{Small caps} for the analysis stages.
@@ -385 +386 @@
 \hline
   Burntool repair          & registration & \ref{sec:burntool} \\
-  Non-linearity correction & cell         & \ref{sec:nonlinearity} \\
-  Overscan Subtraction     & cell         & \ref{sec:overscan} \\
-  Dark \& Bias Subtraction & cell         & \ref{sec:dark} \\
-  Pattern Row correction   & cell         & \ref{sec:pattern.row} \\
-  Noisemap                 & cell         & \ref{sec:noisemap} \\
+  Non-linearity correction & chip         & \ref{sec:nonlinearity} \\
+  Overscan Subtraction     & chip         & \ref{sec:overscan} \\
+  Dark \& Bias Subtraction & chip         & \ref{sec:dark} \\
+  Pattern Row correction   & chip         & \ref{sec:pattern.row} \\
+  Noisemap                 & chip         & \ref{sec:noisemap} \\
   Flat-field Correction    & chip         & \ref{sec:flat} \\
   Fringe Correction$^1$    & chip         & \ref{sec:fringe} \\
@@ -1759 +1760 @@
 \subsection{Astrophysical vs Other Backgrounds}
 
-The model of the background light is subtracted from each chip image
+\textadd{The model of the background light is subtracted from each chip image
 during the \IPPstage{chip}-stage processing before source detection
 begins.  The decision to subtract a background model is somewhat
 tricky as the trade-offs are not clear in all possible cases.  It is
 helpful to consider the types of sources which contribute to the
-background light in astronomical images.
+background light in astronomical images.}
 
 \begin{table*}[tpb]
@@ -1787 +1788 @@
 \end{table*}
 
-First, there is ``scattered'' light\footnote{We put the term ``scattered'' in quotes because this
+\textadd{First, there is ``scattered'' light\footnote{We put the term ``scattered'' in quotes because this
   background may include light which reaches the detector directly
   from the sky or other light source rather than scattering off
@@ -1804 +1805 @@
 ``scattered'' background light source would be the large out-of-focus
 pupil image observed in \eg, the NOAO and CTIO wide-field imagers
-\citep{2007ASPC..376..269S}.
-
-Second, there are direct terrestrial contributions to the background
+\citep{2007ASPC..376..269S}.}
+
+\textadd{Second, there are direct terrestrial contributions to the background
 light.  This source of light follows the same path as the light from
 the stars to the detector, but has an origin much closer to the
@@ -1816 +1817 @@
 are not expected to be repeatable for a given location on the sky,
 though the pupil ghost image may well be the same for a fixed
-telescope pointing and night sky brighness.
-
-Finally, there are astrophysical contributions to the background
+telescope pointing and night sky brighness.}
+
+\textadd{Finally, there are astrophysical contributions to the background
 light.  These range from the (relatively) nearby zodiacal light to the
 extragalactic background.  Depending on the context and the source
@@ -1827 +1828 @@
 object, e.g., a well-resolved galaxy, it is necessary to 
 decide what portion of the large-scale flux is a background and what
-is part of the flux of the object being measured.
-
-When one measures the flux of an object in an image, two approaches to
+is part of the flux of the object being measured.}
+
+\textadd{When one measures the flux of an object in an image, two approaches to
 the background light are possible.  On the one hand, one could attempt
 to include the background as part of the model-fitting parameters at
@@ -1841 +1842 @@
 Second, by subtracting a background model, we remove varying
 backgrounds from the image so that the resulting pixels can later be
-combined to make a deep stack.  
-
-The IPP background subtraction works well to remove the large-scale
+combined to make a deep stack.  }
+
+\textadd{The IPP background subtraction works well to remove the large-scale
 background structures from the terrestrial and scattered-light
 sources, and to subtract the background light of large-scale
@@ -1859 +1860 @@
 M31, which covers an entire pointing of GPC1, the measured background
 was added back to the \IPPstage{chip} stage images.  This special
-processing was not used for the large scale $3\pi$ PV3 reduction.
+processing was not used for the large scale $3\pi$ PV3 reduction.}
 
 \section{GPC1 Detrend Construction}