User: knarf Date: 2011/11/14 01:34 PM
Modified: / ET.tex
Log: don't specify paths to figures in \includegraphics
File Changes:
Directory: / ============
File [modified]: ET.tex Delta lines: +30 -23 =================================================================== --- ET.tex 2011-11-14 19:05:49 UTC (rev 239) +++ ET.tex 2011-11-14 19:34:05 UTC (rev 240) @@ -30,7 +30,14 @@ \usepackage[sort&compress,numbers]{natbib} \renewcommand{\bibfont}{\footnotesize}
-\graphicspath{{figures/}} +\graphicspath{{figures/} +{cactus-benchmarks/} +{examples/kerr/figs/} +{examples/bbh/figs/} +{examples/tov/} +{examples/collapse/} +{examples/cosmology/figs/} +}
\setcounter{secnumdepth}{5}
@@ -457,9 +464,9 @@
\begin{figure} \centering - \includegraphics[width=0.3\textwidth]{figures/carpet-timestepping} + \includegraphics[width=0.3\textwidth]{carpet-timestepping} \hspace{3em} - \includegraphics[width=0.3\textwidth]{figures/carpet-interpolation} + \includegraphics[width=0.3\textwidth]{carpet-interpolation} \caption{Berger-Oliger time stepping details, showing a coarse and a fine grid, with time advancing upwards. \textbf{Left:} Time stepping algorithm. First the coarse grid takes a large time step, then the @@ -476,7 +483,7 @@ used in production on up to several thousand cores~\cite{Reisswig:2010cd,Lousto:2010ut}. \begin{figure} \centering - \includegraphics[width=0.85\textwidth]{cactus-benchmarks/results-best} + \includegraphics[width=0.85\textwidth]{results-best} \caption{Results from weak scaling tests evolving the Einstein equations on a mesh refinement grid structure with nine levels. This shows the time required per grid point, @@ -2214,8 +2221,8 @@ Figure~\ref{fig:kerr_waves} shows the $\ell =2, m=0$ mode of $r\Psi_4$ extracted at $R=30M$, and its numerical convergence. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves_conv} + \includegraphics[width=0.9\textwidth]{waves} + \includegraphics[width=0.9\textwidth]{waves_conv} \caption{The extracted $\ell =2, m=0$ mode of $\Psi_4$ as function of time from the high resolution run (top plot). The extraction was done at $R=30M$. Shown is both the real (solid black curve) and the @@ -2242,8 +2249,8 @@ Figure~\ref{fig:kerr_waves_l4} shows similar plots for the $\ell =4, m=0$ mode of $r\Psi_4$, again extracted at $R=30 M$. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves_l4} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves_l4_conv} + \includegraphics[width=0.9\textwidth]{waves_l4} + \includegraphics[width=0.9\textwidth]{waves_l4_conv} \caption{Real part of the extracted $\ell =4, m=0$ mode of $\Psi_4$ as function of time (top plot) for the high (solid black curve), medium (dashed blue curve) and low (dotted red @@ -2279,8 +2286,8 @@ \codename{AHFinderDirect} as a function of time at the high (black solid curve), medium (blue dashed curve) and low (red dotted curve) resolutions. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/ah_mass} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/ah_mass_conv} + \includegraphics[width=0.9\textwidth]{ah_mass} + \includegraphics[width=0.9\textwidth]{ah_mass_conv} \caption{The top plot shows the irreducible mass of the apparent horizon as a function of time at low (black solid curve), medium (blue dashed curve) and high (red dotted curve) resolutions. The inset is a zoom in on the @@ -2311,8 +2318,8 @@ mass (top plot) and the change in the spin, $\Delta S = S(t) - S(t=0)$, as calculated by \codename{QuasiLocalMeasures}. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/qlm_mass} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/qlm_spin} + \includegraphics[width=0.9\textwidth]{qlm_mass} + \includegraphics[width=0.9\textwidth]{qlm_spin} \caption{The top plot shows the total mass and the bottom plot shows the change in spin (i.e.\ $\Delta S=S(t)-S(t=0)$ of the BH as a function of time. In both plots the black (solid) curve is for high, blue (dashed) for medium and red (dotted) for low resolution. In the bottom plot the green (dash-dotted) @@ -2502,8 +2509,8 @@ templates.
\begin{figure} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/tracks} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/mp_psi4_l2_m2_r60} + \includegraphics[width=0.45\textwidth]{tracks} + \includegraphics[width=0.45\textwidth]{mp_psi4_l2_m2_r60} \caption{In the left panel, we plot the tracks corresponding to the evolution of two punctures initially located on the $x$-axis at $x=\pm 3$. The solid blue line represents puncture 1, and the dashed red line @@ -2517,8 +2524,8 @@ \end{figure}
\begin{figure} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/amp_convergence_all_8th} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/phase_convergence_all_8th} + \includegraphics[width=0.45\textwidth]{amp_convergence_all_8th} + \includegraphics[width=0.45\textwidth]{phase_convergence_all_8th} \caption{Weyl scalar amplitude (left panel) and phase (right panel) convergence. The long dashed red curves represent the difference between the medium and low-resolution runs. The short dashed orange curves show @@ -2574,7 +2581,7 @@
\begin{figure} \label{fig:tov_rho_max} - \includegraphics[width=0.9\textwidth]{examples/tov/rho_max} + \includegraphics[width=0.9\textwidth]{rho_max} \caption{Evolution of the central density for the TOV star. Clearly visible is an initial spike, produced by the interpolation of the one-dimensional equilibrium solution onto the three-dimensional evolution grid. The remainder of the evolution @@ -2598,7 +2605,7 @@
\begin{figure} \label{fig:tov_mode_spectrum} - \includegraphics[width=0.9\textwidth]{examples/tov/mode_spectrum} + \includegraphics[width=0.9\textwidth]{mode_spectrum} \caption{Eigenfrequency mode spectrum of a TOV star. Shown is the power spectral density of the central matter density, computed from a full 3D relativistic hydrodynamics simulation and compared to the values obtained by @@ -2627,7 +2634,7 @@
\begin{figure} \label{fig:tov_ham_conv} - \includegraphics[width=0.9\textwidth]{examples/tov/ham_conv} + \includegraphics[width=0.9\textwidth]{ham_conv} \caption{Convergence factor of Hamiltonian constraint violation at $r=0\mathrm{M}$ and $r=5\mathrm{M}$. The observed convergence order of about $1.5$ at the center of the star is lower then the general @@ -2686,7 +2693,7 @@ than second order, but higher than first order. \begin{figure} \label{fig:tov_collapse_radii} - \includegraphics[width=0.9\textwidth]{examples/collapse/radii} + \includegraphics[width=0.9\textwidth]{radii} \caption{Coordinate radius of the surface of the collapsing star and radius of the forming apparent horizon. The stellar surface is defined as the point where $\rho$ is @@ -2700,7 +2707,7 @@ \end{figure} \begin{figure} \label{fig:tov_collapse_H_convergence_at0} - \includegraphics[width=0.9\textwidth]{examples/collapse/H_convergence_at0} + \includegraphics[width=0.9\textwidth]{H_convergence_at0} \caption{Convergence factor for the Hamiltonian constraint violation at the center of the collapsing star. We plot convergence factors computed using a set of 4 runs covering the diameter of the star @@ -2773,8 +2780,8 @@ time resolutions.
\begin{figure} - \includegraphics[width=0.9\textwidth]{examples/cosmology/figs/kasner.pdf} - \includegraphics[width=0.9\textwidth]{examples/cosmology/figs/err.pdf} + \includegraphics[width=0.9\textwidth]{kasner.pdf} + \includegraphics[width=0.9\textwidth]{err.pdf} \caption{Top: the evolution of a vacuum spacetime of the type~\eref{eq:gowdyT3}, with $P=Q=\lambda=0$; the initial data are chosen as $\gamma_{ij}=\delta_{ij}$ and $K_{ij}={\rm diag}(-2/3,-2/3,1/3)$.