Index: trunk/doc/release.2015/inputs/lib.bib =================================================================== --- trunk/doc/release.2015/inputs/lib.bib (revision 40615) +++ trunk/doc/release.2015/inputs/lib.bib (revision 40616) @@ -15875,5 +15875,5 @@ } -@ARTICLE{2000A&AS..144..363A, +@ARTICLE{2000AAS..144..363A, author = {{Alard}, C.}, title = "{Image subtraction using a space-varying kernel}", Index: trunk/doc/release.2015/ps1.detrend/Makefile =================================================================== --- trunk/doc/release.2015/ps1.detrend/Makefile (revision 40615) +++ trunk/doc/release.2015/ps1.detrend/Makefile (revision 40616) @@ -2,5 +2,5 @@ DO_PDFLATEX = 1 -DO_BIBTEX = 1 +DO_BIBTEX = 0 help: @@ -47,4 +47,5 @@ ../inputs/astro.sty \ ../inputs/apj.bst \ +../inputs/code.sty \ $(ALLPICS) \ detrend.tex Index: trunk/doc/release.2015/ps1.detrend/detrend.bbl =================================================================== --- trunk/doc/release.2015/ps1.detrend/detrend.bbl (revision 40615) +++ trunk/doc/release.2015/ps1.detrend/detrend.bbl (revision 40616) @@ -2,5 +2,5 @@ \expandafter\ifx\csname natexlab\endcsname\relax\def\natexlab#1{#1}\fi -\bibitem[{{Alard}(2000)}]{2000A&AS..144..363A} +\bibitem[{{Alard}(2000)}]{2000AAS..144..363A} {Alard}, C. 2000, \aaps, 144, 363 Index: trunk/doc/release.2015/ps1.detrend/detrend.tex =================================================================== --- trunk/doc/release.2015/ps1.detrend/detrend.tex (revision 40615) +++ trunk/doc/release.2015/ps1.detrend/detrend.tex (revision 40616) @@ -794,5 +794,5 @@ \end{figure} -\begin{deluxetable}{ccl} +\begin{deluxetable*}{ccl} \tablecolumns{3} \tablewidth{0pc} @@ -820,5 +820,5 @@ \enddata \label{tab:mask_values} -\end{deluxetable} +\end{deluxetable*} \subsubsection{Dynamic masks} @@ -884,4 +884,34 @@ pixels. +\paragraph{Optical ghosts} +\label{sec:optical_ghosts} + +The anti-reflective coating on the optical surfaces of GPC1 is less +effective at shorter wavelengths, which can allow bright sources to +reflect back onto the focal plane and generate large out-of-focus +objects. Due to the wavelength dependence, these objects are most +prominent in the \gps{} filter data. These objects are the result of +light reflecting back off the surface of the detector, reflecting +again off the lower surfaces of the optics (particularly the L1 +corrector lens), and then back down onto the focal plane. Due to the +extra travel distance, the resulting source is out of focus and +elongated along the radial direction of the camera focal +plane. Figure~\ref{fig:optical ghosts} shows an example exposure with +several prominent optical ghosts. + +These optical ghosts can be modeled in the focal plane coordinates +($L,M$) which has its origin at the center of the focal plane. In +this system, a bright object at location ($L,M$) on the focal plane +creates a reflection ghost on the opposite side of the optical axis +near ($-L,-M$). The exact location is fit as a third order polynomial +in the focal plane $L$ and $M$ directions (as listed in Table +\ref{tab:ghost_centers}). An elliptical annulus mask is constructed +at the expected ghost location, with the major and minor axes of the inner and outer elliptical annuli defined +by linear functions of the ghost distance from the optical axis, and +oriented with the ellipse major axis is along the radial direction +(Table \ref{tab:ghost_radii}). All stars brighter than a +filter-dependent threshold (listed in Table +\ref{tab:ghost_magnitudes}) have such masks constructed. + \begin{deluxetable}{lllc} \tablecolumns{4} @@ -904,34 +934,4 @@ \end{deluxetable} -\paragraph{Optical ghosts} -\label{sec:optical_ghosts} - -The anti-reflective coating on the optical surfaces of GPC1 is less -effective at shorter wavelengths, which can allow bright sources to -reflect back onto the focal plane and generate large out-of-focus -objects. Due to the wavelength dependence, these objects are most -prominent in the \gps{} filter data. These objects are the result of -light reflecting back off the surface of the detector, reflecting -again off the lower surfaces of the optics (particularly the L1 -corrector lens), and then back down onto the focal plane. Due to the -extra travel distance, the resulting source is out of focus and -elongated along the radial direction of the camera focal -plane. Figure~\ref{fig:optical ghosts} shows an example exposure with -several prominent optical ghosts. - -These optical ghosts can be modeled in the focal plane coordinates -($L,M$) which has its origin at the center of the focal plane. In -this system, a bright object at location ($L,M$) on the focal plane -creates a reflection ghost on the opposite side of the optical axis -near ($-L,-M$). The exact location is fit as a third order polynomial -in the focal plane $L$ and $M$ directions (as listed in Table -\ref{tab:ghost_centers}). An elliptical annulus mask is constructed -at the expected ghost location, with the major and minor axes defined -by linear functions of the ghost distance from the optical axis, and -oriented with the ellipse major axis is along the radial direction -(Table \ref{tab:ghost_radii}). All stars brighter than a -filter-dependent threshold (listed in Table -\ref{tab:ghost_magnitudes}) have such masks constructed. - \begin{deluxetable}{lcc} \tablecolumns{3} @@ -954,9 +954,9 @@ \end{deluxetable} -\begin{deluxetable}{lcccc} +\begin{deluxetable*}{lcccc} \tablecolumns{5} \tablewidth{0pc} \tablecaption{Optical Ghost Annulus Axis Length} - \tablehead{\colhead{Radial Order}&\colhead{Inner Major Axis}&\colhead{Inner Minor Axis}& \colhead{Outer Major Axis}&\colhead{Outer Minor Axis}} + \tablehead{\colhead{Radial Order}&\colhead{Inner Major Axis}&\colhead{Inner Minor Axis}&\colhead{Outer Major Axis}&\colhead{Outer Minor Axis}} \startdata $r^0$ & 3.926693e+01 & 5.287548e+01 & 7.928722e+01 & 1.314265e+02 \\ @@ -964,5 +964,17 @@ \enddata \label{tab:ghost_radii} -\end{deluxetable} +\end{deluxetable*} + +%% \begin{deluxetable}{lcccc} +%% \tablecolumns{5} +%% \tablewidth{0pc} +%% \tablecaption{Optical Ghost Annulus Axis Length} +%% \tablehead{\colhead{Order}&\colhead{Maj$_{\rm in}$}&\colhead{Min$_{\rm in}$}& \colhead{Maj$_{\rm out}$}&\colhead{Min$_{\rm out}$}} +%% \startdata +%% $r^0$ & 3.926693e+01 & 5.287548e+01 & 7.928722e+01 & 1.314265e+02 \\ +%% $r^1$ & 5.325759e-03 &-2.191669e-03 & 1.722181e-02 & -2.627153e-03 \\ +%% \enddata +%% \label{tab:ghost_radii} +%% \end{deluxetable} \begin{deluxetable}{lrr} @@ -970,5 +982,6 @@ \tablewidth{0pc} \tablecaption{Optical Ghost Magnitude Limits} - \tablehead{\colhead{Filter} & \colhead{$m_{inst}$} & \colhead{Approx apparent mag ($3\pi$)}} +% \tablehead{\colhead{Filter} & \colhead{$m_{inst}$} & \colhead{\parbox{2cm}{Apparent mag ($3\pi$)}}} + \tablehead{\colhead{Filter} & \colhead{$m_{inst}$} & \colhead{Apparent mag ($3\pi$)}} \startdata \gps{} & -16.5 & 12.2 \\ @@ -981,12 +994,4 @@ \label{tab:ghost_magnitudes} \end{deluxetable} - -\begin{figure} - \centering -% \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts.jpg} - \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts_sm.png} - \caption{{\bf Ghosts:} Example of the full GPC1 field of view illustrating the sources and destinations of optical ghosts on exposure o5677g0123o (2011-04-26, 43s \gps{} filter). The bright stars on OTA33 and OTA44 result in nearly circular ghosts on the opposite OTA. In contrast, the trio of stars on OTA11 result in very elongated ghosts on OTA66.} - \label{fig:optical ghosts} -\end{figure} \paragraph{Optical glints} @@ -1013,12 +1018,4 @@ degree. -\begin{figure} - \centering -% \includegraphics[width=0.9\hsize,angle=0,clip]{images/glint_example_o5379g0103o.jpg} - \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_glints_sm.png} - \caption{{\bf Glints:} Example of a glint on exposure o5379g0103o (2010-07-02, 45s \ips{} filter). The source star out of the field of view creates a long reflection that extends through OTA73 and OTA63.} - \label{fig:optical glints} -\end{figure} - \paragraph{Diffraction Spikes and Saturated Stars} \label{sec:diffraction_spikes} @@ -1038,4 +1035,36 @@ diffraction spikes and core saturation highlighted, is shown in Figure \ref{fig:saturated star}. + +Saturation for the GPC1 detectors varies from chip to chip and cell to +cell. Saturation levels have been measured in the lab for each cell +and are recorded in the headers. The IPP analysis code reads the +header value to determine the appropriate saturation point. Of the +3840 cells in GPC1, the median saturation level is 60,400; 95\% have +saturation levels $> 54,500$ DN; 99\% have saturation levels $> +41,000$ DN. A small number of cells have recorded saturation values +much lower than these values, but these also tend to be the cells for +which other cosmetic effects (\eg, CTE \& dark current) are strong, +likely affecting the measurement of the saturation value. + +\begin{figure} + \centering +% \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts.jpg} + \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts_sm.png} + \caption{{\bf Ghosts:} Example of the full GPC1 field of view + illustrating the sources and destinations of optical ghosts on + exposure o5677g0123o (2011-04-26, 43s \gps{} filter). The bright + stars on OTA33 and OTA44 result in nearly circular ghosts on the + opposite OTA. In contrast, the trio of stars on OTA11 result in + very elongated ghosts on OTA66.} + \label{fig:optical ghosts} +\end{figure} + +\begin{figure} + \centering +% \includegraphics[width=0.9\hsize,angle=0,clip]{images/glint_example_o5379g0103o.jpg} + \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_glints_sm.png} + \caption{{\bf Glints:} Example of a glint on exposure o5379g0103o (2010-07-02, 45s \ips{} filter). The source star out of the field of view creates a long reflection that extends through OTA73 and OTA63.} + \label{fig:optical glints} +\end{figure} \begin{figure} @@ -1222,15 +1251,14 @@ \label{sec:burntool} -Pixels that approach the saturation point on GPC1, which varies by -cell with common values around 60000 DN, introduce ``persistent -charge'' on that and subsequent images. During the read out process -of a cell with such a bright pixel, some of the charge remains in the -undepleted region of the silicon and is not shifted down the detector -column toward the amplifier. This charge remains in the starting -pixel and slowly leaks out of the undepleted region, contaminating -subsequent pixels during the read out process, resulting in a ``burn -trail'' that extends from the center of the bright source away from -the amplifier (vertically along the pixel columns toward the top of -the cell). +Pixels that approach the saturation point on GPC1 (see +Section~\ref{sec:diffraction_spikes}) introduce ``persistent charge'' +on that and subsequent images. During the read out process of a cell +with such a bright pixel, some of the charge remains in the undepleted +region of the silicon and is not shifted down the detector column +toward the amplifier. This charge remains in the starting pixel and +slowly leaks out of the undepleted region, contaminating subsequent +pixels during the read out process, resulting in a ``burn trail'' that +extends from the center of the bright source away from the amplifier +(vertically along the pixel columns toward the top of the cell). This incomplete charge shifting in nearly full wells continues as each @@ -1565,5 +1593,5 @@ the PV3 processing. -\begin{deluxetable}{lcccc} +\begin{deluxetable*}{lcccc} \tablecolumns{5} \tablewidth{0pc} @@ -1585,8 +1613,8 @@ \enddata \label{tab:detrend ppImage} -\end{deluxetable} - - -\begin{deluxetable}{lcccc} +\end{deluxetable*} + + +\begin{deluxetable*}{lcccc} \tablecolumns{5} \tablewidth{0pc} @@ -1603,7 +1631,7 @@ \enddata \label{tab:detrend ppMerge} -\end{deluxetable} - -\begin{deluxetable}{lclll} +\end{deluxetable*} + +\begin{deluxetable*}{lclll} \tablecolumns{5} \tablewidth{0pc} @@ -1649,5 +1677,5 @@ \tablenotetext{a}{These dates mark the beginning and ending of the two-mode dark models, between which multiple dates use the B-mode dark.} \label{tab:detrend list} -\end{deluxetable} +\end{deluxetable*} \section{Warping} @@ -1877,5 +1905,5 @@ convolution kernels can be calculated for each image. To calculate the convolution kernels, we use the algorithm described by -\cite{1998ApJ...503..325A} and extended by \cite{2000A&AS..144..363A} +\cite{1998ApJ...503..325A} and extended by \cite{2000AAS..144..363A} to perform optimal image subtraction. These `ISIS' kernels \citep[named after the software package described @@ -2330,7 +2358,7 @@ University (ELTE), and the Los Alamos National Laboratory. -\bibliography{lib}{} \bibliographystyle{apj} - +% \bibliography{lib}{} +\input{detrend.bbl} \end{document}