- Timestamp:
- Jan 27, 2019, 11:41:45 AM (7 years ago)
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- trunk/doc/release.2015
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inputs/lib.bib (modified) (1 diff)
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ps1.detrend/Makefile (modified) (2 diffs)
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ps1.detrend/detrend.bbl (modified) (1 diff)
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ps1.detrend/detrend.tex (modified) (17 diffs)
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trunk/doc/release.2015/inputs/lib.bib
r40602 r40616 15875 15875 } 15876 15876 15877 @ARTICLE{2000A &AS..144..363A,15877 @ARTICLE{2000AAS..144..363A, 15878 15878 author = {{Alard}, C.}, 15879 15879 title = "{Image subtraction using a space-varying kernel}", -
trunk/doc/release.2015/ps1.detrend/Makefile
r40615 r40616 2 2 3 3 DO_PDFLATEX = 1 4 DO_BIBTEX = 14 DO_BIBTEX = 0 5 5 6 6 help: … … 47 47 ../inputs/astro.sty \ 48 48 ../inputs/apj.bst \ 49 ../inputs/code.sty \ 49 50 $(ALLPICS) \ 50 51 detrend.tex -
trunk/doc/release.2015/ps1.detrend/detrend.bbl
r40614 r40616 2 2 \expandafter\ifx\csname natexlab\endcsname\relax\def\natexlab#1{#1}\fi 3 3 4 \bibitem[{{Alard}(2000)}]{2000A &AS..144..363A}4 \bibitem[{{Alard}(2000)}]{2000AAS..144..363A} 5 5 {Alard}, C. 2000, \aaps, 144, 363 6 6 -
trunk/doc/release.2015/ps1.detrend/detrend.tex
r40615 r40616 794 794 \end{figure} 795 795 796 \begin{deluxetable }{ccl}796 \begin{deluxetable*}{ccl} 797 797 \tablecolumns{3} 798 798 \tablewidth{0pc} … … 820 820 \enddata 821 821 \label{tab:mask_values} 822 \end{deluxetable }822 \end{deluxetable*} 823 823 824 824 \subsubsection{Dynamic masks} … … 884 884 pixels. 885 885 886 \paragraph{Optical ghosts} 887 \label{sec:optical_ghosts} 888 889 The anti-reflective coating on the optical surfaces of GPC1 is less 890 effective at shorter wavelengths, which can allow bright sources to 891 reflect back onto the focal plane and generate large out-of-focus 892 objects. Due to the wavelength dependence, these objects are most 893 prominent in the \gps{} filter data. These objects are the result of 894 light reflecting back off the surface of the detector, reflecting 895 again off the lower surfaces of the optics (particularly the L1 896 corrector lens), and then back down onto the focal plane. Due to the 897 extra travel distance, the resulting source is out of focus and 898 elongated along the radial direction of the camera focal 899 plane. Figure~\ref{fig:optical ghosts} shows an example exposure with 900 several prominent optical ghosts. 901 902 These optical ghosts can be modeled in the focal plane coordinates 903 ($L,M$) which has its origin at the center of the focal plane. In 904 this system, a bright object at location ($L,M$) on the focal plane 905 creates a reflection ghost on the opposite side of the optical axis 906 near ($-L,-M$). The exact location is fit as a third order polynomial 907 in the focal plane $L$ and $M$ directions (as listed in Table 908 \ref{tab:ghost_centers}). An elliptical annulus mask is constructed 909 at the expected ghost location, with the major and minor axes of the inner and outer elliptical annuli defined 910 by linear functions of the ghost distance from the optical axis, and 911 oriented with the ellipse major axis is along the radial direction 912 (Table \ref{tab:ghost_radii}). All stars brighter than a 913 filter-dependent threshold (listed in Table 914 \ref{tab:ghost_magnitudes}) have such masks constructed. 915 886 916 \begin{deluxetable}{lllc} 887 917 \tablecolumns{4} … … 904 934 \end{deluxetable} 905 935 906 \paragraph{Optical ghosts}907 \label{sec:optical_ghosts}908 909 The anti-reflective coating on the optical surfaces of GPC1 is less910 effective at shorter wavelengths, which can allow bright sources to911 reflect back onto the focal plane and generate large out-of-focus912 objects. Due to the wavelength dependence, these objects are most913 prominent in the \gps{} filter data. These objects are the result of914 light reflecting back off the surface of the detector, reflecting915 again off the lower surfaces of the optics (particularly the L1916 corrector lens), and then back down onto the focal plane. Due to the917 extra travel distance, the resulting source is out of focus and918 elongated along the radial direction of the camera focal919 plane. Figure~\ref{fig:optical ghosts} shows an example exposure with920 several prominent optical ghosts.921 922 These optical ghosts can be modeled in the focal plane coordinates923 ($L,M$) which has its origin at the center of the focal plane. In924 this system, a bright object at location ($L,M$) on the focal plane925 creates a reflection ghost on the opposite side of the optical axis926 near ($-L,-M$). The exact location is fit as a third order polynomial927 in the focal plane $L$ and $M$ directions (as listed in Table928 \ref{tab:ghost_centers}). An elliptical annulus mask is constructed929 at the expected ghost location, with the major and minor axes defined930 by linear functions of the ghost distance from the optical axis, and931 oriented with the ellipse major axis is along the radial direction932 (Table \ref{tab:ghost_radii}). All stars brighter than a933 filter-dependent threshold (listed in Table934 \ref{tab:ghost_magnitudes}) have such masks constructed.935 936 936 \begin{deluxetable}{lcc} 937 937 \tablecolumns{3} … … 954 954 \end{deluxetable} 955 955 956 \begin{deluxetable }{lcccc}956 \begin{deluxetable*}{lcccc} 957 957 \tablecolumns{5} 958 958 \tablewidth{0pc} 959 959 \tablecaption{Optical Ghost Annulus Axis Length} 960 \tablehead{\colhead{Radial Order}&\colhead{Inner Major Axis}&\colhead{Inner Minor Axis}& 960 \tablehead{\colhead{Radial Order}&\colhead{Inner Major Axis}&\colhead{Inner Minor Axis}&\colhead{Outer Major Axis}&\colhead{Outer Minor Axis}} 961 961 \startdata 962 962 $r^0$ & 3.926693e+01 & 5.287548e+01 & 7.928722e+01 & 1.314265e+02 \\ … … 964 964 \enddata 965 965 \label{tab:ghost_radii} 966 \end{deluxetable} 966 \end{deluxetable*} 967 968 %% \begin{deluxetable}{lcccc} 969 %% \tablecolumns{5} 970 %% \tablewidth{0pc} 971 %% \tablecaption{Optical Ghost Annulus Axis Length} 972 %% \tablehead{\colhead{Order}&\colhead{Maj$_{\rm in}$}&\colhead{Min$_{\rm in}$}& \colhead{Maj$_{\rm out}$}&\colhead{Min$_{\rm out}$}} 973 %% \startdata 974 %% $r^0$ & 3.926693e+01 & 5.287548e+01 & 7.928722e+01 & 1.314265e+02 \\ 975 %% $r^1$ & 5.325759e-03 &-2.191669e-03 & 1.722181e-02 & -2.627153e-03 \\ 976 %% \enddata 977 %% \label{tab:ghost_radii} 978 %% \end{deluxetable} 967 979 968 980 \begin{deluxetable}{lrr} … … 970 982 \tablewidth{0pc} 971 983 \tablecaption{Optical Ghost Magnitude Limits} 972 \tablehead{\colhead{Filter} & \colhead{$m_{inst}$} & \colhead{Approx apparent mag ($3\pi$)}} 984 % \tablehead{\colhead{Filter} & \colhead{$m_{inst}$} & \colhead{\parbox{2cm}{Apparent mag ($3\pi$)}}} 985 \tablehead{\colhead{Filter} & \colhead{$m_{inst}$} & \colhead{Apparent mag ($3\pi$)}} 973 986 \startdata 974 987 \gps{} & -16.5 & 12.2 \\ … … 981 994 \label{tab:ghost_magnitudes} 982 995 \end{deluxetable} 983 984 \begin{figure}985 \centering986 % \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts.jpg}987 \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts_sm.png}988 \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.}989 \label{fig:optical ghosts}990 \end{figure}991 996 992 997 \paragraph{Optical glints} … … 1013 1018 degree. 1014 1019 1015 \begin{figure}1016 \centering1017 % \includegraphics[width=0.9\hsize,angle=0,clip]{images/glint_example_o5379g0103o.jpg}1018 \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_glints_sm.png}1019 \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.}1020 \label{fig:optical glints}1021 \end{figure}1022 1023 1020 \paragraph{Diffraction Spikes and Saturated Stars} 1024 1021 \label{sec:diffraction_spikes} … … 1038 1035 diffraction spikes and core saturation highlighted, is shown in Figure 1039 1036 \ref{fig:saturated star}. 1037 1038 Saturation for the GPC1 detectors varies from chip to chip and cell to 1039 cell. Saturation levels have been measured in the lab for each cell 1040 and are recorded in the headers. The IPP analysis code reads the 1041 header value to determine the appropriate saturation point. Of the 1042 3840 cells in GPC1, the median saturation level is 60,400; 95\% have 1043 saturation levels $> 54,500$ DN; 99\% have saturation levels $> 1044 41,000$ DN. A small number of cells have recorded saturation values 1045 much lower than these values, but these also tend to be the cells for 1046 which other cosmetic effects (\eg, CTE \& dark current) are strong, 1047 likely affecting the measurement of the saturation value. 1048 1049 \begin{figure} 1050 \centering 1051 % \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts.jpg} 1052 \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_ghosts_sm.png} 1053 \caption{{\bf Ghosts:} Example of the full GPC1 field of view 1054 illustrating the sources and destinations of optical ghosts on 1055 exposure o5677g0123o (2011-04-26, 43s \gps{} filter). The bright 1056 stars on OTA33 and OTA44 result in nearly circular ghosts on the 1057 opposite OTA. In contrast, the trio of stars on OTA11 result in 1058 very elongated ghosts on OTA66.} 1059 \label{fig:optical ghosts} 1060 \end{figure} 1061 1062 \begin{figure} 1063 \centering 1064 % \includegraphics[width=0.9\hsize,angle=0,clip]{images/glint_example_o5379g0103o.jpg} 1065 \includegraphics[width=0.9\hsize,angle=0,clip]{images/full_fpa_glints_sm.png} 1066 \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.} 1067 \label{fig:optical glints} 1068 \end{figure} 1040 1069 1041 1070 \begin{figure} … … 1222 1251 \label{sec:burntool} 1223 1252 1224 Pixels that approach the saturation point on GPC1, which varies by 1225 cell with common values around 60000 DN, introduce ``persistent 1226 charge'' on that and subsequent images. During the read out process 1227 of a cell with such a bright pixel, some of the charge remains in the 1228 undepleted region of the silicon and is not shifted down the detector 1229 column toward the amplifier. This charge remains in the starting 1230 pixel and slowly leaks out of the undepleted region, contaminating 1231 subsequent pixels during the read out process, resulting in a ``burn 1232 trail'' that extends from the center of the bright source away from 1233 the amplifier (vertically along the pixel columns toward the top of 1234 the cell). 1253 Pixels that approach the saturation point on GPC1 (see 1254 Section~\ref{sec:diffraction_spikes}) introduce ``persistent charge'' 1255 on that and subsequent images. During the read out process of a cell 1256 with such a bright pixel, some of the charge remains in the undepleted 1257 region of the silicon and is not shifted down the detector column 1258 toward the amplifier. This charge remains in the starting pixel and 1259 slowly leaks out of the undepleted region, contaminating subsequent 1260 pixels during the read out process, resulting in a ``burn trail'' that 1261 extends from the center of the bright source away from the amplifier 1262 (vertically along the pixel columns toward the top of the cell). 1235 1263 1236 1264 This incomplete charge shifting in nearly full wells continues as each … … 1565 1593 the PV3 processing. 1566 1594 1567 \begin{deluxetable }{lcccc}1595 \begin{deluxetable*}{lcccc} 1568 1596 \tablecolumns{5} 1569 1597 \tablewidth{0pc} … … 1585 1613 \enddata 1586 1614 \label{tab:detrend ppImage} 1587 \end{deluxetable }1588 1589 1590 \begin{deluxetable }{lcccc}1615 \end{deluxetable*} 1616 1617 1618 \begin{deluxetable*}{lcccc} 1591 1619 \tablecolumns{5} 1592 1620 \tablewidth{0pc} … … 1603 1631 \enddata 1604 1632 \label{tab:detrend ppMerge} 1605 \end{deluxetable }1606 1607 \begin{deluxetable }{lclll}1633 \end{deluxetable*} 1634 1635 \begin{deluxetable*}{lclll} 1608 1636 \tablecolumns{5} 1609 1637 \tablewidth{0pc} … … 1649 1677 \tablenotetext{a}{These dates mark the beginning and ending of the two-mode dark models, between which multiple dates use the B-mode dark.} 1650 1678 \label{tab:detrend list} 1651 \end{deluxetable }1679 \end{deluxetable*} 1652 1680 1653 1681 \section{Warping} … … 1877 1905 convolution kernels can be calculated for each image. To calculate 1878 1906 the convolution kernels, we use the algorithm described by 1879 \cite{1998ApJ...503..325A} and extended by \cite{2000A &AS..144..363A}1907 \cite{1998ApJ...503..325A} and extended by \cite{2000AAS..144..363A} 1880 1908 to perform optimal image subtraction. These `ISIS' kernels 1881 1909 \citep[named after the software package described … … 2330 2358 University (ELTE), and the Los Alamos National Laboratory. 2331 2359 2332 \bibliography{lib}{}2333 2360 \bibliographystyle{apj} 2334 2361 % \bibliography{lib}{} 2362 \input{detrend.bbl} 2335 2363 2336 2364 \end{document}
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