[GRASS-SVN] r61258 - in grass-promo/grassposter/2014_EGU_M3_Landscape: . code images
svn_grass at osgeo.org
svn_grass at osgeo.org
Tue Jul 15 19:57:53 PDT 2014
Author: ychemin
Date: 2014-07-15 19:57:53 -0700 (Tue, 15 Jul 2014)
New Revision: 61258
Added:
grass-promo/grassposter/2014_EGU_M3_Landscape/images/MariaDepthm.png
grass-promo/grassposter/2014_EGU_M3_Landscape/images/mdi_high.png
grass-promo/grassposter/2014_EGU_M3_Landscape/images/mdi_low.png
Modified:
grass-promo/grassposter/2014_EGU_M3_Landscape/Makefile
grass-promo/grassposter/2014_EGU_M3_Landscape/code/code1.tex
grass-promo/grassposter/2014_EGU_M3_Landscape/poster.tex
grass-promo/grassposter/2014_EGU_M3_Landscape/tikzposter.sty
Log:
Updated poster
Modified: grass-promo/grassposter/2014_EGU_M3_Landscape/Makefile
===================================================================
--- grass-promo/grassposter/2014_EGU_M3_Landscape/Makefile 2014-07-16 02:44:20 UTC (rev 61257)
+++ grass-promo/grassposter/2014_EGU_M3_Landscape/Makefile 2014-07-16 02:57:53 UTC (rev 61258)
@@ -17,17 +17,20 @@
make pdf; \
done
-pdf: fig
+pdf: fig code
pdflatex $(FILE).tex
+ bibtex $(FILE)
fig: $(SVGPDF)
$(SVGPDF): %.pdf: %.svg
inkscape -z --export-pdf=$@ --export-area-drawing --export-dpi=300 $<
-#$(CODEPDF): %.pdf: %.tex
-# pdflatex -shell-escape -output-directory=$(CODEDIR) $<
+code: $(CODEPDF)
+$(CODEPDF): %.pdf: %.tex
+ pdflatex -shell-escape -output-directory=$(CODEDIR) $<
+
clean:
rm -f *~ *.aux *.log *.out *.toc *.bbl *.blg *-blx.bib *.ps
rm -f $(SVGPDF) $(CODEPDF)
Modified: grass-promo/grassposter/2014_EGU_M3_Landscape/code/code1.tex
===================================================================
--- grass-promo/grassposter/2014_EGU_M3_Landscape/code/code1.tex 2014-07-16 02:44:20 UTC (rev 61257)
+++ grass-promo/grassposter/2014_EGU_M3_Landscape/code/code1.tex 2014-07-16 02:57:53 UTC (rev 61258)
@@ -2,6 +2,7 @@
\usepackage{minted}
\begin{document}
\begin{minted}[frame=single,linenos,mathescape,fontsize=\small]{py}
+
#!/bin/env python
from math import *
@@ -19,15 +20,16 @@
return(17.83*(-atan(((uvvis4/uvvis2)-1.26)/0.01)) - 6.87)
print "@Surveyor"
-#dummy
-uvvis1=0.04
#M3 at Surveyor crater
+
uvvis2=0.05028829
uvvis4=0.0579434
print "@Bench"
#M3 at Bench (north outside)
+
uvvis2=0.05045871
uvvis4=0.05715561
+
\end{minted}
\end{document}
\ No newline at end of file
Added: grass-promo/grassposter/2014_EGU_M3_Landscape/images/MariaDepthm.png
===================================================================
(Binary files differ)
Property changes on: grass-promo/grassposter/2014_EGU_M3_Landscape/images/MariaDepthm.png
___________________________________________________________________
Added: svn:mime-type
+ application/octet-stream
Added: grass-promo/grassposter/2014_EGU_M3_Landscape/images/mdi_high.png
===================================================================
(Binary files differ)
Property changes on: grass-promo/grassposter/2014_EGU_M3_Landscape/images/mdi_high.png
___________________________________________________________________
Added: svn:mime-type
+ application/octet-stream
Added: grass-promo/grassposter/2014_EGU_M3_Landscape/images/mdi_low.png
===================================================================
(Binary files differ)
Property changes on: grass-promo/grassposter/2014_EGU_M3_Landscape/images/mdi_low.png
___________________________________________________________________
Added: svn:mime-type
+ application/octet-stream
Modified: grass-promo/grassposter/2014_EGU_M3_Landscape/poster.tex
===================================================================
--- grass-promo/grassposter/2014_EGU_M3_Landscape/poster.tex 2014-07-16 02:44:20 UTC (rev 61257)
+++ grass-promo/grassposter/2014_EGU_M3_Landscape/poster.tex 2014-07-16 02:57:53 UTC (rev 61258)
@@ -47,9 +47,8 @@
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\blocknode{Abstract}{
-\small \noindent The geology of the Apollo 12 landing site has been the subject of many studies, including recently by \cite{korotev2011apollo} and \cite{Snape2013basaltic}. This research attempts to bring additional understanding from a remote sensing perspective using the Moon Mineralogy Mapper ($M^3$) sensor data, onboard the Chandrayaan lunar orbiter. This has a higher spatial-spectral resolution sensor than the Clementine UV-Vis sensor and provides the opportunity to study the lunar surface with detailed spectral signatures.\newline
-
-Mapping of FeO (wt\%) and TiO 2 (wt\%) is done using the methods of \cite{lucey2000lunar} and \cite{wilcox2005mapping}. A FeO \& TiO 2 processing module (i.feotio2) is made specifically for this research within the Free \& Open Source Software GRASS GIS \cite{neteler2012grass}. Attempts will be made to estimate the lava flow thickness using the method of \cite{bugiolacchi2006stratigraphy} and individual lava layers thicknesses from \cite{weider2010individual}. Integration of this new information will be put in perspective and integrated with previous work. Analysis from the combined higher spatial and spectral resolutions will improve the accuracy of the geological mapping at the Apollo 12 landing site.\newline
+\small \noindent The geology of the Apollo 12 landing site has been the subject of many studies, including recently by \cite{korotev2011apollo} and \cite{Snape2013basaltic}. This research attempts to bring additional understanding from a remote sensing perspective using the Moon Mineralogy Mapper ($M^3$) sensor data, onboard the Chandrayaan lunar orbiter. This has a higher spatial-spectral resolution sensor than the Clementine UV-Vis sensor and provides the opportunity to study the lunar surface with detailed spectral signatures.\vspace{5mm}\newline
+Mapping of FeO (wt\%) and TiO 2 (wt\%) is done using the methods of \cite{lucey2000lunar} and \cite{wilcox2005mapping}. A FeO \& TiO 2 processing module (i.feotio2) is made specifically for this research within the Free \& Open Source Software GRASS GIS \cite{neteler2012grass}. Attempts will be made to estimate the lava flow thickness using the method of \cite{bugiolacchi2006stratigraphy} and individual lava layers thicknesses from \cite{weider2010individual}. Integration of this new information will be put in perspective and integrated with previous work. Analysis from the combined higher spatial and spectral resolutions will improve the accuracy of the geological mapping at the Apollo 12 landing site.
}
@@ -92,14 +91,14 @@
\bibliography{poster}
\endgroup
-\hrulefill
-\vspace{-5pt}
+%\hrulefill
+%\vspace{-5pt}
\begin{center}
\begin{tabular}{c}
\hspace{5mm}
\begin{minipage}{0.2\textwidth}
-\includegraphics[width=0.7in]{./images/grass_qr.pdf}
+\includegraphics[width=0.5in]{./images/grass_qr.pdf}
\end{minipage}
\begin{minipage}{0.25\textwidth}
@@ -115,37 +114,23 @@
\end{minipage}
\begin{minipage}{0.2\textwidth}
-\includegraphics[width=0.7in]{./images/grass_qr.pdf}
+\includegraphics[width=0.5in]{./images/grass_qr.pdf}
\end{minipage}
\end{tabular}
\end{center}
-\hrulefill
}
\startsecondcolumn
-%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
-\blocknode{Clementine data}{
-\smallskip
-\begin{center}
- \includegraphics[width=0.75\textwidth]{./images/Clementine}
- \newline
- Figure 3: Clementine RGB153 (top), segmentation (middle) and FeO (wt\%) per segmentation class (bottom).
-\end{center}
-}
-
-
-
-\startthirdcolumn
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\blocknode{M$^3$ derived FeO from standard equations}{
\bigskip
\begin{center}
\begin{tabular}{ c p{0.45\textwidth}}
- \raisebox{-1.1\totalheight}{\includegraphics[width=0.5\textwidth]{./code/code1}}
+ \raisebox{-1.1\totalheight}{\includegraphics[width=0.5\textwidth]{./code/code1.pdf}}
%\caption{Testing FeO algorithms.}
\label{fig:FeOtesting}
&
@@ -159,6 +144,7 @@
\cite{lawrence2002iron} & 4.72 & 6.38 \\
\cite{wilcox2005mapping} & 22.28 & 21.82 \\
\cite{zhang2013mapping} & 19.74 & 19.49 \\
+\cite{zhang2013mapping} (corrected) & 15.65 & 14.76 \\
\hline
\end{tabular}
\end{center}
@@ -166,9 +152,9 @@
\noindent It is known that the local range of FeO is below 10wt\% from UVVIS data (see Figure on the lower left), only the \cite{lawrence2002iron} equation is giving an appropriate range. \cite{lucey2000lunar} equation fails because of the offset of uvvis4/uvvis2(=1.15 vs offset = 1.19) and the one for uvvis2(=0.05 vs offset = 0.08), as both of the parts are negative thus giving a positive division output, their interplay should bring a negative number for the arctangent negative sign to compensate. This clearly does not happen with $M^3$ data in the Bench and Surveyor craters, the results from the arctangent being positive, and the sign change brings the main part of the equation to a negative, further reduced by the negative final offset.\newline
\end{tabular}
\end{center}
-\noindent Upon using the equation from \cite{lawrence2002iron}, it turned out that though the wt\%FeO range was satisfactory for few crater points, the rate of change was actually reverse to the expected one, reducing to null towards the South of the landing site and increasing towards the North.\newline
-\noindent The equation from \cite{zhang2013mapping} is giving an appropriate rate of change, however, the local values are too large compared to the Clementine derived FeO values. Comparing the zonal contrast between Clementine FeO map from \cite{lucey2000lunar} the $M^3$ from \cite{zhang2013mapping} leads to an interesting prospect as even the shapes are not consistent (see Figures ~\ref{fig:subfeoclem} \& ~\ref{fig:subfeoM3}). This indicates that the inner work of the angle equation is not sensitive to the same type of distance between R950 and R750 as they are in Clementine and in $M^3$. In an ideal condition, the calibration of both sensor bands would be identical, and the sensor response for each band would also be the same. This is not a reality, from the design and manufacture inheritance of multi-spectral sensors and hyperspectral sensors, to the data collection flight and its environment. Finally, some accident or issues can damage the operation.\newline
-\noindent After Contacting W. Zhang of \cite{zhang2013mapping} about the issue in its algorithm, he promptly answered that the article had a typo in the equation. After correction, the output were in a better range (about 15 for the two craters in the table above).\newline
+\noindent Upon using the equation from \cite{lawrence2002iron}, it turned out that though the wt\%FeO range was satisfactory for few crater points, the rate of change was actually reverse to the expected one, reducing to null towards the South of the landing site and increasing towards the North.\vspace{5mm}\newline
+\noindent The equation from \cite{zhang2013mapping} is giving an appropriate rate of change, however, the local values are too large compared to the Clementine derived FeO values. Comparing the zonal contrast between Clementine FeO map from \cite{lucey2000lunar} the $M^3$ from \cite{zhang2013mapping} leads to an interesting prospect as even the shapes are not consistent (see Figures ~\ref{fig:subfeoclem} \& ~\ref{fig:subfeoM3}). This indicates that the inner work of the angle equation is not sensitive to the same type of distance between R950 and R750 as they are in Clementine and in $M^3$. In an ideal condition, the calibration of both sensor bands would be identical, and the sensor response for each band would also be the same. This is not a reality, from the design and manufacture inheritance of multi-spectral sensors and hyperspectral sensors, to the data collection flight and its environment. Finally, some accident or issues can damage the operation.\vspace{5mm}\newline
+\noindent After Contacting W. Zhang of \citep{zhang2013mapping} about the issue in its algorithm, he promptly answered that the article had a typo in the equation. After correction, the output were in a better range (about 15 for the two craters in the table above).\newline
\begin{center}
\begin{tabular}{ c c }
@@ -196,17 +182,61 @@
\end{tabular}
\end{tabular}
\end{center}
+\vspace{2mm}
+}
+\startthirdcolumn
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\blocknode{Lava Flow Depth}{
+\smallskip
+\noindent Isolating the 95\% top and 5\% bottom of the destriped FeO image brought the possibility to suggest the Fresh Crater Ejecta (FCE) values. The FCE was found near Lansberg P in the surroundings of (-22.8215621403E,-2.09875487116N) with 11 samples averaging to 17.87 FeO wt\%.\newline
+\begin{center}
+ \begin{tabular}{cc}
+ \includegraphics[width=0.42\textwidth]{./images/mdi_high}\hspace{20mm}
+ &
+ \includegraphics[width=0.47\textwidth]{./images/mdi_low}
+ \end{tabular}\newline
+Figure 3 (left): Locating FCE above Lansberg P, with the upper 95\% FeO wt\%\\
+Figure4 (right): Locating lowest E Westward Copernicus, with the lower 5\% FeO wt\%.
+\end{center}
+
+\noindent The H value is the lower boundary of the FeO wt\% in the region, typically found in the nearest highland region. There are two solid constraints to it value. H should be strictly less than E and strictly more than zero ($0<H<E$). The E value was found in Copernicus ejecta ring and actually taken from the FeO wt\% map. The minimum value found in the FeO\_M3G20090111T013904.destripe map is 3.88 wt\%, belonging to the ejecta ring of Copernicus. Thus it can be inferred that $0<H<3.88$, strictly, in this Copernican work. Looking at over M$^3$ FeO tiles, there is no lower value to the crater ejecta of Copernicus. Some Alpes Formation and Dark Mantling Material in the vicinity of Gay Lussac do not go lower than this.\newline
+
+\noindent This is obviously shows the limit of this statistical search method. Another attempt was undertaken using the original tile FeO\_M320090610T113334 a visual search for H in the vicinity of Montes Carpatus (Northwestern of Copernicus with -23.6070634574E, 14.571534275N) was done and from 14 samples found $\overline{H}=5.88$. Another visual search in the ejecta blanket of Copernicus for a FCE value, 22 samples were collected, giving an average FCE value of 7.16. Thus, it is found that $0 < \overline H < \overline{FCE}$, which is a logical outcome. It is thus proposed to carry forward this parametrisation for mapping the depth of the Copernican lava flow with the following equation ~\ref{eq:NewMareDepthVal}.\newline
+\begin{equation}\label{eq:NewMareDepthVal}
+Mh = \frac {D_*} {8} \times \frac {E-\overline{H}} {\overline{FCE}-\overline{H}} = \frac {117000}{8} \times \frac {E-5.88}{17.87-5.88} [m]
+\end{equation}
+\noindent Which realizes as the following equation.\newline
+\begin{equation}\label{eq:NewMareDepthValCoef}
+Mh = (E-5.88) \times 1219.77 [m]
+\end{equation}
}
+
+
+
+
+\blocknode{Conclusions}{
+\smallskip
+Conclusions
+}
+
\startfourthcolumn
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\blocknode{Clementine data}{
+\smallskip
-
+\begin{center}
+ \includegraphics[width=0.45\textwidth]{./images/Clementine}
+ \newline
+ Figure 3: Clementine RGB153 (top), segmentation (middle) and FeO (wt\%) per segmentation class (bottom).
+\end{center}
+}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\blocknode{M$^3$ Signal at Apollo 12 landing site}{
\smallskip
@@ -225,7 +255,7 @@
\end{tabular}
}%End of tabular
&
- \noindent Chandrayaan $M^3$ data was downloaded from PDS \url{http://pds-imaging.jpl.nasa.gov/}{pds-imaging.jpl.nasa.gov}. The tile \textit{M3G20090111T013904\_V01\_RFL.IMG} was imported in GRASS GIS, resulting in 85 bands. The spectrum for four craters where extracted in the Figure \ref{fig:specsignature4craters}. Bench and Surveyor are both together in the lower reflectance curves. On the higher side, Sharp and Middle Crescent are consistently above the two others. This higher broadband Albedo is increasing towards the West, where one of the ray is clearly drawn (Oblique white strip in the middle of The Clementine upper map. Compared to the spectral data from Figure ~\ref{fig:specsignatureASTERlib} the reflectance is overall lower and the obvious shape differences are there. Additional spectrum signature data from \cite{clark2007usgs} is in the process of being extracted for analysis.\newline\linebreak
+ \noindent Chandrayaan $M^3$ data was downloaded from PDS \url{http://pds-imaging.jpl.nasa.gov/}. The tile \textit{M3G20090111T013904\_V01\_RFL.IMG} was imported in GRASS GIS, resulting in 85 bands. The spectrum for four craters where extracted in the Figure \ref{fig:specsignature4craters}. Bench and Surveyor are both together in the lower reflectance curves. On the higher side, Sharp and Middle Crescent are consistently above the two others. This higher broadband Albedo is increasing towards the West, where one of the ray is clearly drawn (Oblique white strip in the middle of The Clementine upper map. Compared to the spectral data from Figure ~\ref{fig:specsignatureASTERlib} the reflectance is overall lower and the obvious shape differences are there. Additional spectrum signature data from \cite{clark2007usgs} is in the process of being extracted for analysis.\newline\linebreak
\noindent Figure 8: \newline Spectral signature of $M^3$ from four craters.
\newline\linebreak
\noindent Figure 9: \newline Spectral signature from Apollo 12 (Speclib v2.0).
@@ -237,10 +267,6 @@
}%End of Block
-\blocknode{Conclusions}{
-\smallskip
-Conclusions
-}
\end{tikzpicture}
Modified: grass-promo/grassposter/2014_EGU_M3_Landscape/tikzposter.sty
===================================================================
--- grass-promo/grassposter/2014_EGU_M3_Landscape/tikzposter.sty 2014-07-16 02:44:20 UTC (rev 61257)
+++ grass-promo/grassposter/2014_EGU_M3_Landscape/tikzposter.sty 2014-07-16 02:57:53 UTC (rev 61258)
@@ -504,9 +504,9 @@
(0,0) -- ($(\paperwidth+5,0) + tan(\a)*(0,\paperwidth)$); }
\foreach \i in {1,2,...,35}{
- \begin{scope}[shift={($(rand*60,rand*70)$)}]
+ \begin{scope}[shift={($(rand*120,rand*70)$)}]%Yann: double rand shift 60->120: all page circles
\draw[backgroundlightcolor!80!, line width=0.1cm]
- ($0.5*(topright)$) circle (4);
+ ($0.5*(topright)$) circle (rand*2+4);%Yann: added rand*2 to circle config
\end{scope}
}
% }{}
More information about the grass-commit
mailing list