From 39ef28af054ec4d06f25aa9c94bcfeaaadc27f41 Mon Sep 17 00:00:00 2001 From: hanemile Date: Wed, 7 Mar 2018 21:04:23 +0100 Subject: presentation (posters) --- pres/plakate_test/a0header.ps | 6 + pres/plakate_test/test.aux | 1 + pres/plakate_test/test.fdb_latexmk | 63 ++++++ pres/plakate_test/test.fls | 107 +++++++++ pres/plakate_test/test.log | 213 ++++++++++++++++++ pres/plakate_test/test.pdf | Bin 0 -> 21209 bytes pres/plakate_test/test.synctex.gz | Bin 0 -> 1321 bytes pres/plakate_test/test.tex | 440 +++++++++++++++++++++++++++++++++++++ 8 files changed, 830 insertions(+) create mode 100644 pres/plakate_test/a0header.ps create mode 100644 pres/plakate_test/test.aux create mode 100644 pres/plakate_test/test.fdb_latexmk create mode 100644 pres/plakate_test/test.fls create mode 100644 pres/plakate_test/test.log create mode 100644 pres/plakate_test/test.pdf create mode 100644 pres/plakate_test/test.synctex.gz create mode 100644 pres/plakate_test/test.tex (limited to 'pres/plakate_test') 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10000000) + diff --git a/pres/plakate_test/test.pdf b/pres/plakate_test/test.pdf new file mode 100644 index 0000000..25e6f95 Binary files /dev/null and b/pres/plakate_test/test.pdf differ diff --git a/pres/plakate_test/test.synctex.gz b/pres/plakate_test/test.synctex.gz new file mode 100644 index 0000000..b91bd78 Binary files /dev/null and b/pres/plakate_test/test.synctex.gz differ diff --git a/pres/plakate_test/test.tex b/pres/plakate_test/test.tex new file mode 100644 index 0000000..1d78615 --- /dev/null +++ b/pres/plakate_test/test.tex @@ -0,0 +1,440 @@ +\documentclass[portrait]{sciposter} + +\usepackage[utf8x]{inputenc} +\usepackage[ngerman, english]{babel} +\usepackage{amsmath} +\usepackage{amsfonts} +\usepackage{amssymb} +\usepackage{graphicx} +\usepackage{multicol} +\usepackage{sectionbox} + +\author{Emile Hansmaennel} +\title{Development of components for\\ a ChiralSTEM -- Mode} +\institute{Universität Regensburg\\} +\email{andreas.hasenkopf@physik.uni-regensburg.de} +\leftlogo[1]{UniLogo2} +\rightlogo[1]{TEM-Logo} +\conference{14. European Microscopy Congress, Aachen, September 1--5, 2008} +\begin{document} + +\maketitle +\rule{\textwidth}{2mm} + +\begin{multicols}{3} + +\begin{abstract} +The effect of \textbf{E}nergy-loss \textbf{M}agnetic \textbf{C}hiral \textbf{D}ichroism (EMCD) was proposed by Schattschneider et al. \cite{emcd_proposal} in analogy to XMCD due to similar scattering cross section expressions (wave vector transfer $\vec{q}$ in inelastic electron scattering $\leftrightarrow$ polarization vector $\vec{\epsilon}$ in X-ray absorption). The effect was measured for the first time by Rubino \cite{emcd_nature}. + +The state of the art method for recording EMCD-spectra is the ''intrinsic method'' requiring the specimen to fulfill three strict properties (mono crystal, thickness, orientation) due to its use as a beam splitter. In order to avoid these requirements an alternative setup with a twin aperture and Boersch phase plate for generating 2 coherent electron waves with a phase difference of $\pi/2$ is suggested. Chiral contrast in energy-loss spectra is achieved due to a magnetic sample. + +To determine whether a twin aperture is suitable for EMCD-measurements -- in particular in STEM-mode -- the wave function and intensity distribution in the sample plane are calculated numerically and the optimum dimensions for the aperture and phase plate are determined. Finally a STEM operation with a twin aperture is realized. +\end{abstract} + +\section{Intrinsic method} +\textbf{\scshape Analogon to Circular Polarization}: two scattered coherent electron waves (wave vector transfers: $q_1$, $q_2$, $q_1\perp q_2$ or $q\,'_1$, $q\,'_2$, $q\,'_1\perp q\,'_2$) with a phase difference of $\pi/2$. + +\begin{figure}[h] +\begin{center} +\label{fig_intrinsic} +\includegraphics[width=\textwidth]{poster_aperture_einzel.png} +\caption{setup -- intrinsic method} +\end{center} +\end{figure} + +\textbf{\scshape Setup}: see fig. \ref{fig_intrinsic}. +\begin{itemize} +\item proposed by Nelhiebel \cite{emcd_intrinsic} and used in prior EMCD-measurements\cite{emcd_nature,pd_rubino,pd_hurm}, +\item mono crystalline sample as beam splitter, +\item two Bragg reflexes with phase difference $\pi/2$ in the diffraction plane according to dynamic diffraction theory (see \cite{pd_rubino,pd_hurm}). +\end{itemize} + +\textbf{\scshape Deficiencies}: +\begin{itemize} +\item signal low, +\item resolution low (improved by convergent beam technique \cite{mcd_in_eels_2}), +\item long duration of measurement. +\end{itemize} + +\textbf{\scshape Needed Improvements}: +\begin{itemize} +\item higher intensity within +\item small specimen area +\item[$\Rightarrow$] focussed beams $\to$ STEM?! +\end{itemize} + +\section{Twin Aperture} +\textbf{\scshape Suggestion}: see fig. \ref{fig_twin} +\begin{itemize} +\item twin aperture $\to$ two coherent partial electron waves, +\item condenser lens $\to$ focussing, +\item electrostatic Boersch phase plate (annular electrode) \cite{phaseplate} $\to$ application of phase shift to one partial wave +\end{itemize} + +\begin{figure}[h] +\begin{center} +\label{fig_twin} +\includegraphics[width=\textwidth]{poster_aperture_twin.png} +\end{center} +\caption{setup -- twin aperture} +\end{figure} +% one electron wave is shifted in phase such that the phase difference of the two waves in the sample plane is $\pi/2$ and such that a similar diffraction pattern is observed in the diffraction plane as for the intrinsic method. + +%Therefor the possibility of a STEM operation with such a twin aperture was investigated due to the wish to perform EMCD measurement in a STEM mode in the future. + +\section{Numerical Calculations} + +\textbf{\scshape Intensity Distribution}: $|\psi_{BFP}|^2$, see fig. \ref{fig_linescan} +\begin{eqnarray} +\psi_{BFP}(X,\,Y) &=& \mathrm{J}_1\left(\frac{2\pi R\sqrt{X^2+Y^2}}{\lambda f}\right)\frac{\lambda f}{\pi R\sqrt{X^2+Y^2}} \nonumber \\ +&& \cdot\left( e^{-\frac{id_1X}{\lambda f}}+e^{-\frac{id_2X}{\lambda f}-i\varphi}\right),\nonumber \\ +\Delta\phi(X) &=& \left((d_2-d_1)\frac{X}{\lambda f}+\varphi+\pi\right)\mathrm{mod}(2\pi)-\pi \nonumber +\end{eqnarray} + +\begin{itemize} +\item in sample plane $\equiv$ back focal plane (BFP) +\item influence of phase shift on intensity in BFP +\item what are optimum parameters for $R$, $d_1$, $d_2$ and $\varphi$? +\end{itemize} + +\begin{figure}[h] +\includegraphics[width=\textwidth]{poster_linescan.png} +\caption{intensity distribution and phase difference} +\label{fig_linescan} +\end{figure} + +%As one can see the maximum of the intensity distribution and the $\pi/2$-polygon coincide. Thus it is possible to adjust a phase shift to one electron wave such that the phase difference in the BFP reaches it's optimum value of $\pi/2$ at the maximum of the intensity distribution in the BFP. + +\textbf{\scshape Definition}: quality parameter $U$ and weighting function $\Upsilon$: +\begin{eqnarray} +\label{eqn_usignal} +U &=& \frac{\int\limits_{-\infty}^\infty\Upsilon(X)|\psi_{BFP}(X,\,0)|^2\,\mathrm{d}X}{\int\limits_{-\infty}^\infty|\psi_{BFP}(X,\,0)|^2\,\mathrm{d}X} \nonumber\\ +\label{eqn_upsilon_1} +\Upsilon(X) &=& 2\,\mathrm{sgn}\left(\Delta\phi(X)\right)\left|\left(\frac{\Delta\phi(X)}{\pi}+\frac{1}{2}\right)\mathrm{mod}\,1-\frac{1}{2}\right| \nonumber\\ +\label{eqn_sn} +\mathrm{S/N} &=& \frac{\int\limits_a^b|\psi_{BFP}(X,\,0)|^2\,\mathrm{d}X}{\int\limits_{-\infty}^\infty|\psi_{BFP}(X,\,0)|^2\,\mathrm{d}X},\;[a,\,b]: \mathrm{FWHM} \nonumber +\end{eqnarray} + +\begin{itemize} +\item $U$: coarse measure for percentage of intensity with phase difference $= \pi/2$ , +\item S/N: ratio between intensity within FWHM and total intensity, +\item $\Upsilon$: zigzag weighting function (see fig. \ref{fig_upsilon}) defined to fulfill: + +\begin{equation} +\Upsilon(X) = \left\{\begin{array}{rcl} +\pm1 &\mathrm{for}& \Delta\phi(X) = \pm\frac{\pi}{2} \\ +0 &\mathrm{for}& \Delta\phi(X) = i\pi,\;i=0,\,\pm1 \\ +\end{array}\right. .\nonumber +\end{equation} +\end{itemize} + +\textbf{\scshape Optimum Parameter Set}: determined by brute-force method +\begin{itemize} +\item numerical calculation: $U$, FWHM and S/N for each parameter set, +\item saving results in MySQL database $\to$ graphical evaluation: fig. \ref{fig_sql_1} and \ref{fig_sql_2} +\item[$\Rightarrow$] \textbf{aperture}: maximum radius and minimum spacing +%(see fig. \ref{fig_linescan}) +\item[$\Rightarrow$] chosen parameters: Radius = $28.5\mu$m, Spacing = $60.7\mu$m, Phase shift = $0.57\pi$ +\end{itemize} + +\begin{figure}[h] +\begin{center} +\includegraphics[width=\textwidth]{poster_upsilon.png} +\end{center} +\caption{weighting function $\Upsilon$ (for legend see fig. \ref{fig_linescan})} +\label{fig_upsilon} +\end{figure} + +%whereby $J_1$ is the Bessel function, $\Delta\phi$ is the phase difference between two electron waves in the diffraction plane, $X$ is an coordinate in that plane, $d_{1,2}$ are the spacings of the apertures' centers from the optical axis, $R$ is the aperture radius, $\lambda$ is the electron wave length, $f$ is the focal length of the lens and $\varphi$ is the phase shift due to a phase plate. + +\begin{figure}[hbt] +\label{fig_sql_1} +%\includegraphics[width=.8\textwidth]{poster_sql_u.png} +\includegraphics[width=\textwidth]{poster_usignal_2.png} +\caption{evaluation -- $U$} +\end{figure} + +\begin{figure}[hbt] +%\includegraphics[width=.8\textwidth]{poster_sql_sn.png} +\includegraphics[width=\textwidth]{poster_sn_2.png} +\caption{evaluation -- Signal/Noise (for legend see fig. \ref{fig_sql_1})} +\label{fig_sql_2} +\end{figure} + +%The data sets generated in this way are stored in a MySQL database and are plotted in dependence of the spacing between the apertures in figures \ref{fig_sql_1} and \ref{fig_sql_2}. Figure \ref{fig_sql_1} shows the dependence of the quantity $\mathfrak{U}$ and figure \ref{fig_sql_2} the dependence of the S/N ratio for different aperture radii (7, 11, 17, 21 and 27 $\mu$m) on the aperture spacing. + +%These results suggest the use of large aperture radii but small aperture spacings. According to that the parameters given in the legend of figure \ref{fig_linescan} (Radius: 28$\mu$m, Spacing: 62$\mu$m) were chosen further regarding the available area on the used SiN membrane for production of a twin aperture. + +\section{Experiments} +\textbf{\scshape Production}: electron lithography +\begin{itemize} +\item holes in SiN membrane (100$\mu$m$\times$100$\mu$m) +\item evaporation of gold +\end{itemize} + +\textbf{\scshape STEM}: operation with condenser twin aperture +\begin{itemize} +\item sample: gold particles on a carbon foil. +\item comparison: conventional aperture $\leftrightarrow$ twin aperture +\item[$\Rightarrow$] no influence on image quality +\end{itemize} + +\begin{figure}[hbt] +\label{fig_goldstem} +\subfigure[twin aperture]{\label{fig_goldstem_a} +%\includegraphics[width=.475\textwidth]{gold_einzel_50k.png} +\includegraphics[width=.45\textwidth]{8061-5png.png}} +\subfigure[STEM image]{\label{fig_goldstem_b}\includegraphics[width=.45\textwidth]{gold_twin_50k.png}} +\caption{twin aperture (w/o phase plate) \& STEM image of gold particles using twin aperture.} +\end{figure} + +%Figure \ref{fig_goldstem} shows images observed in STEM-mode with the CM30 at a magnification of $5\cdot10^4$. By means of red arrows two particles are marked in both figures. Figure \ref{fig_goldstem}(a) shows the image obtained with an einzel aperture and \ref{fig_goldstem}(b) the image obtained using the twin aperture. + +%As one can see the use of a twin aperture has no apparent negative influence on image quality. + +\section{Outlook} +\begin{multicols}{2} +\textbf{\scshape Electron Lithography}: phase plate +\begin{itemize} +\item negative resist PMMA\cite{pmma} +\item[$\Rightarrow$] deposition of gold $\to$ annular electrode +\item deposition of insulating layers and gold overlays +\end{itemize} +\textbf{\scshape EMCD}: record spectra in +\begin{itemize} +\item diffraction mode +\item STEM-mode +\end{itemize} +\end{multicols} + +\begin{multicols}{2} +\tiny +\bibliographystyle{plain} +\bibliography{literature} +\end{multicols} + +\end{multicols} +\end{document} + +% \documentclass[a2,landscape]{a0poster} +% +% \usepackage{multicol} +% \columnsep=100pt +% \columnseprule=3pt +% +% \usepackage[svgnames]{xcolor} +% +% \usepackage{times} % Times New Roman +% \usepackage{graphicx} % Required for including images +% \graphicspath{{figs/}} % Location of the graphics files +% \usepackage{booktabs} % Top and bottom rules for table +% \usepackage[font=small,labelfont=bf]{caption} % Required for specifying captions to tables and figures +% \usepackage{amsfonts, amsmath, amsthm, amssymb} % For math fonts, symbols and environments +% \usepackage{wrapfig} % Allows wrapping text around tables and figures +% +% \usepackage[english,ngerman]{babel} +% \usepackage[utf8]{inputenc} +% +% \begin{document} +% +% % Header | 55% | 25% | 19% | +% +% \begin{minipage}[b]{0.45\linewidth} +% \veryHuge \color{NavyBlue} \textbf{Galaxy Generation} \color{Black}\\ % Title +% \Huge\textit{Visualizierung und Generierung von Galaxien}\\[1cm] % Subtitle +% \huge \textbf{Emile Hansmaennel}\\ % Author(s) +% \huge Theodor Fliedner Gymnasium\\ % University/organization +% \end{minipage} +% % +% \begin{minipage}[b]{0.35\linewidth} +% \includegraphics[height=7.5cm]{logos} +% \vspace{5cm} +% \end{minipage} +% % +% \begin{minipage}[b]{0.19\linewidth} +% \includegraphics[height=15cm]{galaxy} % Logo or a photo of you, adjust its dimensions here +% \end{minipage} +% +% \vspace{1cm} % A bit of extra whitespace between the header and poster content +% +% %---------------------------------------------------------------------------------------- +% +% \begin{multicols}{4} % This is how many columns your poster will be broken into, a poster with many figures may benefit from less columns whereas a text-heavy poster benefits from more +% +% %---------------------------------------------------------------------------------------- +% % ABSTRACT +% %---------------------------------------------------------------------------------------- +% +% \color{Navy} % Navy color for the abstract +% +% \begin{abstract} +% +% Das Ziel meines Projektes ist es, Realitätsgetreue Galaxien und Dunkle Materie +% Halos zu generieren. +% Hierzu verwende ich das sogenannte ''Navarro-Frenk-White'' Profil welches in +% Kombination mit der ''Random Sampling'' Methode die Dichteverteilung +% der Sternenpositionen in Koordinaten für einzelne Sterne umgewandelt. +% \par +% Vergleicht man die generierten Galaxien mit echten Galaxien fällt auf das +% die Sterne sich anders verhalten. Dies lässt sich durch Dunkle Materie erklären, +% welche man jedoch nicht direkt beobachten kann. Es kann also +% nur aufgrund ihrer Auswirkungen auf andere Objekte auf sie geschlossen werden, +% weshalb es nicht ganz Trivial ist sie sichtbar darzustellen. +% \par +% Im Verlauf des Projektes haben sich mir jedoch auch andere Teilbereiche +% eröffnet wie z. B. die Generation von Spiralgalaxien, die Optimierung von +% Rechenprozessen und die Nutzung von einem neuronalen Netz zur Anpassung der +% generierten Galaxie an eine reale Galaxie. +% +% \end{abstract} +% +% %---------------------------------------------------------------------------------------- +% % INTRODUCTION +% %---------------------------------------------------------------------------------------- +% +% \color{SaddleBrown} % SaddleBrown color for the introduction +% +% \section*{Einleitung} +% +% Das Hauptziel des Projektes war es, Galaxien dreidimensional darzustellen um +% diese mit echten Galaxien vergleichen zu können. Dies ist vorallem interessant, +% um echte real vorhandene Galaxien zu untersuchen, da man diese nur aus einer +% Perspektive beobachten kann (von der Erde aus). +% \par +% Dazu verwendete ich die sogennante Random-Sampling-Methode um aus einer +% Warscheinlichkeitsverteilung (dem Narvarro-Frenk-White Profil) Koordinaten +% zu generieren. +% \par +% Ein wichtiger Aspekt der beim generieren von Galaxien ist die Effizienz des +% verwendeten Programms extrem stark zu erhöhen, sodass in einer vergleichsweisen +% geringen Zeit, z.B. sehr viele Sterne generiert werden können. Um dies zu +% erreichen können sehr viele verschieden Ansätze mit eingebracht werden wie +% zum Beispiel die nutzung von mehreren sogennanten "Threads`` zum parralellisieren +% der Rechenarbeit. +% \par +% Um die genauigkeit der generierten galaxie im vergleich zu echten galaxien +% zu erhöhen, können Neuronale Netze verwendet werden. Diese beanspruchen jedoch +% sehr viel Rechenarbeit weshalb sich ihre nutzung erst in ein paar Jahren +% lohnen wird. +% \par +% Das Generieren von Spiralgalaxien führt ebenfalls zu einem Problem: der +% Rechenaufwand steigt mit der Anzahl der Sterne proportional exponentiall an. +% Die Lösung dieses Problems führt zu einer unterteilung der Galaxie in +% verschiedene Zellen, in denen die Kräfte gemittelt werden und anschließend mit +% den anderen Zellen interagieren. +% +% %---------------------------------------------------------------------------------------- +% % OBJECTIVES +% %---------------------------------------------------------------------------------------- +% +% \color{DarkSlateGray} % DarkSlateGray color for the rest of the content +% +% \section*{Hauptziele} +% +% \begin{enumerate} +% \item Generieren von Elliptischen Punktwolken mithilfe des Narvarro-Frenk-White +% profils in verbindung mit der Random-Sampling Methode +% +% \item Verbesserung des Generierungsprozesses mithilfe von "Threadding`` +% +% \item Generierund von Dunkle-Materie-Halos +% +% \item Nutzung von Neuronalen Netzen zum unbeaufsichtigten generieren von +% Galaxien +% \end{enumerate} +% +% %---------------------------------------------------------------------------------------- +% % MATERIALS AND METHODS +% %---------------------------------------------------------------------------------------- +% +% \section*{Materialien und Methoden} +% +% Die verwendete Hardware die zum erstellen der Skripte wervendet wurde war ein +% Acer Laptop mit 2 Rechenkernen welche jeweils 2 Threads enthalten und mit bis +% zu 3,1 GHZ Takten. Die Simulationen wurden während des Praktikums in Heidelberg +% auf dem Laptop im kleinen stil getestet und anschließen auf einem Cluster marke +% eigenbau über einen längeren Zeitraum laufen gelassen. Im Cluster befanden sich +% ca. 14 Rechner mit wahlweise 4 oder 6 Kernen welche ebenfalls alle +% Hyperthreading unterstützten. Nach dem Praktikum verwendete ich zum großteil +% den Laptop und einen Server der mir von einem Freund gestellt wurde. Dieser +% verfüht über 2 mal 6 Kerne die ebenfalls Hyperthreading unterstützen was zu +% 24 logischen Prozessoren mit einer Taktrate von 2,5 GHZ führt. +% +% \par +% +% Zum generieren der Punktwolken verwendete ich das NFW-Profile in kombination +% mit der Random Sampling Methode wodurch die potentielle Koordinaten von Sternen +% entweder akzepriert oder verworfen wurden. Die Koordinated wurden in einer +% .csv Datei gespeichert welche von einem anderem Script weiterverwendet wurde um +% die Sterne in der 3D-Software Suite Blender darzustellen. +% Die Generierung von Spiralgalaxien ist (zurzeit) zu anspruchsvoll, weshalb die +% Daten aus der Punktwolke nicht genutzt werden können, da die quantitative Menge +% zu groß ist. Es wird deshalb eine andere Galaxie mit weniger Sternen generiert. +% +% %------------------------------------------------ +% +% \subsection*{Random Sampling des Narvarro Frenk White Profils} +% +% Das Navarro-Frenk-White Profile (NFW-Profile) wird dazu genutzt, einem Stern +% in einem Abstand \( r \) vom Mittelpunkt der Galaxie eine Warscheinlichkeit +% \( \rho(r) \) zuzuweisen. Diese Warscheinlichkeit ist in Abbildung +% \ref{fig:lookup_NFW} in abhängigkeit zur Entfernung des Mittelpunkt der Galaxie +% dargestellt. +% +% \begin{center}%\vspace{0.5cm} +% \begin{equation*} \label{eq:NFW_profile} +% \rho_{NFW}(r) = \frac{ 1 }{ \sqrt{ 2 \pi } \cdot \sigma } \cdot +% \exp \left( \frac{ -\phi(r) }{ \sigma^{ 2 } } \right) +% \end{equation*} +% +% \begin{equation*} +% \phi(r) = \frac{ 4\pi \cdot G \cdot f_{0} \cdot R_{s}^3 }{ r } \cdot +% ln{ \left( 1 + \frac{ r }{ R_{s} } \right) } +% \end{equation*} +% \end{center}%\vspace{0.5cm} +% +% \begin{center}\vspace{0.5cm} +% \includegraphics[width=0\linewidth]{1e6_6} +% \captionof{figure}{Das Navarro-Frenk-White Profile} +% \label{fig:equation_NFW} +% \end{center}\vspace{0.5cm} +% +% \begin{center}\vspace{0.5cm} +% \includegraphics[width=0.8\linewidth]{1e6_6} +% \captionof{figure}{Der Entsprechende Funktionsgraph zum NFW-Profile} +% \label{fig:lookup_NFW} +% \end{center}\vspace{0.5cm} +% +% \section*{Ergebnisse} +% +% \section*{Feststellungen} +% +% \begin{itemize} +% +% \item Pellentesque\cite{stickley} eget orci eros. Fusce ultricies, tellus et pellentesque +% fringilla, ante massa luctus libero, quis tristique purus urna nec nibh. +% Phasellus fermentum rutrum elementum. Nam quis justo lectus. +% +% \item Vestibulum\cite{schwarzmeier07} sem ante, hendrerit a gravida ac, blandit quis magna. +% +% \item Donec sem metus, figureacilisis at condimentum eget, vehicula ut massa. Morbi +% consequat, diam sed convallis tincidunt, arcu nunc. +% +% \item Nunc at convallis urna. isus ante. Pellentesque condimentum dui. Etiam +% sagittis purus non tellus tempor volutpat. Donec et dui non massa tristique adipiscing. +% +% \end{itemize} +% +% \section*{Zukunft} +% +% \nocite{*} % Print all references regardless of whether they were cited in the poster or not +% \bibliographystyle{plain} % Plain referencing style +% \bibliography{poster} % Citation database is inside poster.bib +% +% \section*{Danksagungen} +% +% Hier möchte ich mich bei Tim Tugendhat und Konstantin Bosbach bedanken ohne die +% das Praktikum in Heidelberg nicht möglich gewesen wäre. +% +% \end{multicols} +% \end{document} -- cgit 1.4.1