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\newcommand{\assemblybias}{\tiny{M. Musso, \alert{C. Cadiou} \emph{et al.}, MNRAS}}
\newcommand{\filtorque}{\tiny{\alert{C. Cadiou}, C. Pichon \& S.Codis, in prep}}
\newcommand{\kraj}{\tiny{K. Kraljic, S. Arnouts, C. Pichon, C. Laigle, S. de la
      Torre, D.Vibert, \alert{C. Cadiou} et al.}, MNRAS}

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\title{How does the cosmic web impacts assembly~bias?}
\subtitle{%
  Impact of large-scale structures on halo \& galaxy evolution}
  \author{\textbf{Corentin Cadiou} -- PhD Student -- IAP, Paris, France\\
    \small{Supervisors: Yohan Dubois \& Christophe Pichon}\\
  \small{In collaboration with M.~Musso \& C.~Codis}}
% \institute{IAP, CNRS}
\date{Journée des Doctorants, March 23, 2017}

\begin{document}

{
  \setbeamercolor{author}{fg=white}
  \setbeamercolor{title}{fg=white}
  \setbeamercolor{subtitle}{fg=white}
  \setbeamercolor{date}{fg=white}
  \usebackgroundtemplate{\includegraphics[width=\paperwidth]{figures/full_hagn.png}}
  \begin{frame}
    \color{white}{\titlepage}
  \end{frame}
}
\begin{frame}[label=toc]{Table of contents}
\tableofcontents
\end{frame}

\section{Introduction}

\begin{frame}[standout]
  What's the link between galaxy/halo formation and large-scale structures?
\end{frame}
\begin{frame}
  \myframetitle{Describing galaxies?}
  \begin{columns}
    \column{.6\textwidth}
    \begin{block}{Theory}
    \includegraphics[width=\columnwidth]{figures/hubble_sequence.pdf}
    + star forming?\\
    + bulge?\\
    + mass?\\
    + DM halo mass?\\
    + DM profile?\\
    + \ldots
    \end{block}
    \column{.4\textwidth}
    \begin{block}{Observations (HDF)}
      \includegraphics[width=\columnwidth]{figures/HDF_galaxies}\\
    \end{block}
    \vspace{2em}
  \end{columns}
  \begin{center}
    \visible<2->{And all the properties \textbf{change with cosmic time}\ldots}
  \end{center}

\end{frame}

\begin{frame}
  \myframetitle{Cosmic Web}
  \begin{center}
    \includegraphics[width=\columnwidth]{figures/cosmic_web}\\
    \vspace{-.8em}
    \hfill{\tiny Horizon-AGN simulation with skeleton, Dubois+12}
  \end{center}
  And all the properties \textbf{change with cosmic time} and location
  w.r.t. \textbf{the cosmic web} (see .e.g K. Kraljic+2017)!
\end{frame}

\begin{frame}
  \myframetitle{Cosmic web}
  \begin{block}{}
    \begin{itemize}
    \item Geometry of the density/potential field
    \item Voids, walls, filaments, peaks (resp. 3, 2, 1, 0D)
      \uncover<3->{\\ or}
    \item<3-> Critical points (0D)
    \end{itemize}
  \end{block}
  \only<1>{
    \begin{center}
      \includegraphics[width=.5\columnwidth]{sloanbutterfly.jpg}
    \end{center}
    \vspace{-1.5em}
    {\hfill \unemph{SDSS}}
  }
  \only<2>{
    \begin{center}
      \includegraphics[width=.5\columnwidth]{{NHgal-insite.wide007}.jpg}
    \end{center}
    \vspace{-1.5em}
    {\hfill \unemph{New Horizon simulation}}
  }
  \only<3>{
    \begin{center}
      \includegraphics[width=.5\columnwidth]{pass}
    \end{center}
  }
\end{frame}

\section{Effect on assembly}
\begin{frame}
  \myframetitle{Theoretical setup}
  \begin{block}{Excursion set theory}
    Galaxy properties \& evolution from \alert{initial conditions}\\
    $\Rightarrow$ Find \alert{largest mass} that will collapse by \alert{$z$}
    at \alert{given location}
  \end{block}

  \begin{columns}
    \column{.55\textwidth}
    \begin{center}
      \includegraphics[width=.7\columnwidth]{figures/3d_excursion_set}\\
      \vspace{-1em}
      {\tiny Courtesy of C. Pichon}
      \begin{tabular}{cc}
        Simulation & Theory \\
        \hline
        $M$ & $R$ \\
        $z,t$ & $\delta = \frac{\rho-\bar{\rho}}{\bar{\rho}}$
      \end{tabular}
    \end{center}

    \column{.45\textwidth}
    \includegraphics[width=.8\columnwidth]{figures/crit_point_standalone}
  \end{columns}
\end{frame}


\subsection{Typical mass}
\begin{frame}
  \myframetitle{Typical mass of DM halo}
  \begin{columns}
    \column{0.5\textwidth}
    \begin{center}
      \includegraphics[width=\columnwidth]{figures/sigma_star_xz_simple}\\
      The typical mass at $z=0$.
    \end{center}
    \assemblybias
    \column{0.5\textwidth}
    \begin{enumerate}
    \item Larger galaxies in nodes
    \item Smaller galaxies in voids
    \end{enumerate}

    In agreement with $n$-body simulations.
  \end{columns}

  % \begin{columns}
  %   \column{.6\textwidth}
  %   \begin{equation*}
  %     \Delta M_\star(\rr)
  %     \propto \delta_\S \xi_{20}(r){\cal Q}
  %   \end{equation*}
  %   \column{.4\textwidth}
  %   $\xi_{20}$: corr. density-tide + density
  % \end{columns}
\end{frame}


\subsection{Effect on (DM) accretion rate}
\begin{frame}
  \myframetitle{Effect on (DM) accretion rate}
   \begin{columns}
    \column{0.5\textwidth}
    \begin{center}
      \includegraphics[width=\columnwidth]{figures/accretion_xz_simple}\\
      Accretion rate at {\bf fixed} final mass $M\simeq \SI{3e11}{\Msun}$.
    \end{center}
    \assemblybias
    \column{0.5\textwidth}
    \begin{enumerate}
    \item High accretion rate in node
    \item Small accretion rate in voids
    \end{enumerate}
  \end{columns}
\end{frame}

\subsection{Effect of halo formation time}

\begin{frame}
  \myframetitle{Effect of halo formation time}
 \begin{columns}
    \column{0.5\textwidth}
    \begin{center}
      \includegraphics[width=\columnwidth]{figures/Dhalf_xz}\\
      Formation time at {\bf fixed} final mass $M\simeq \SI{3e11}{\Msun}$.
    \end{center}
    \assemblybias
    \column{0.5\textwidth}
      \begin{enumerate}
      \item Late formation in node (low $z$)
      \item Early formation in voids (high $z$)
      \end{enumerate}

    \uncover<2->{\alert{Tension with observations?}}
  \end{columns}
\end{frame}

\subsection{Tension with observations?}
\begin{frame}
  \myframetitle{Tension with observations?}
  \begin{columns}
    \column{0.5\textwidth}
    \begin{alertblock}{Theory}
      Higher DM accretion + late formation:\\
      blue central galaxy?
    \end{alertblock}
    \column{0.5\textwidth}
    \begin{exampleblock}{Observations}
      Massive red central galaxies\\
      ~ \\
      ~
    \end{exampleblock}
  \end{columns}

  \uncover<2->{
    \begin{center}
      \includegraphics[width=0.8\textwidth]{figures/H-noAGN.png}\\
      \tiny Dubois+16
    \end{center}
  }
\end{frame}

\begin{frame}
  \myframetitle{Beyond Mass-Density}
  4 parameters dictate mass/accretion/formation time/\dots:
  \begin{columns}
    \column{.4\textwidth}
    \begin{itemize}
    \item<1-> mean density $\delta$
    \item<1-> mean derived density $\delta' = \frac{\d \delta}{\d R}$
    \item<2-> variance of density
    \item<2-> variance of accretion
    \end{itemize}%
    \column{.6\textwidth}%
    \only<1>{\includegraphics[width=\columnwidth]{figures/constrained_no_var}}%
    \only<2>{\includegraphics[width=\columnwidth]{figures/constrained}}%
    \only<3->{\includegraphics[width=\columnwidth]{figures/constrained_with_draws}}%
  \end{columns}
  \uncover<3->{
    Environments with \alert{different variance} do not behave the same: what matters is $(\delta-\langle\delta\rangle)/\sqrt{\mathrm{Var}(\delta)}$
  }
\end{frame}

\section{Filamentary accretion at high $z$}

\subsection{Simple 2D setup}


\begin{frame}
  \myframetitle{From simulations}

  \includegraphics[width=\columnwidth]{figures/3_filaments/4x2}
  \centering{\tiny Density maps of galaxies from New Horizon simulation @ $z=6$, \gray{Dubois+, in prep.}}

  Typical setup: \alert{planar} with \alert{3} filaments

\end{frame}

\begin{frame}
  \myframetitle{Simple 2D model}
  \begin{columns}
    \column{0.5\textwidth}
      \begin{alertblock}{Open questions}
      \begin{itemize}
      \item \alert{Net} torque on filaments?
      \item Galaxy spin-up or down?
      \item Typical coherence scale?
      \end{itemize}
    \end{alertblock}
    \column{0.5\textwidth}
    \uncover<2->{
    \begin{exampleblock}{Model}
      \begin{itemize}
      \item Planar (2D)
      \item 3 voids $\rightarrow$ 3 filaments
      \item 1 central peak
      \end{itemize}
    \end{exampleblock}
    }
  \end{columns}

  \begin{center}
    \includegraphics[width=.9\columnwidth]{figures/filament_torque}\\
    \filtorque
  \end{center}

\end{frame}

\subsection{Predicting the torque}

\begin{frame}
  \myframetitle{Predicting the torque}
  \vspace{-2em}
  Using constrained theory + $\Lambda$-CDM power spectrum
  \vspace{.5em}
  \begin{columns}
    \column{0.45\textwidth}
    \includegraphics[width=\columnwidth]{figures/filament_torque_numerical}\\
    \filtorque
    \column{0.55\textwidth}
    \alert{Voids} are pushing filaments
    \pause

    \begin{center}
      \def\svgwidth{.8\columnwidth}
      \input{figures/schema_1D.pdf_tex}
    \end{center}

  \end{columns}

\end{frame}


\section{Conclusions}

\begin{frame}
  \myframetitle{Conclusions}
  \begin{columns}
    \column{.5\textwidth}
    \begin{exampleblock}{Assembly of DM halo}
      \begin{itemize}
      \item Influenced by LSS
      \item Recovers $n$-body sim
      \item Still need baryonic physics
      \end{itemize}
    \end{exampleblock}
    \column{.5\textwidth}
    \begin{exampleblock}{Torque on filament}
      \begin{itemize}
      \item Expect torque on filament
      \item Quantitative results?
      \item Compare with simulations?
      \end{itemize}
    \end{exampleblock}
  \end{columns}
  \hspace*{-\beamerleftmargin}%
  \includegraphics[width=\paperwidth]{figures/NH-composite-auto-14.jpg}
\end{frame}

\begin{frame}[standout]
  Thank you!
\end{frame}

\appendix

\section{More torque plots}
\begin{frame}
  \myframetitle{Torque on filament}
  \begin{center}
    \includegraphics[height=.8\textheight]{torque-full.pdf}
  \end{center}

\end{frame}


\begin{frame}
  \myframetitle{Effect of AGN}
  \begin{columns}
    \column{0.5\textwidth}
    \includegraphics[width=\columnwidth]{figures/conclusion_accretion}
    \column{0.05\textwidth}
    $\xRightarrow[]{\text{AGN}}$
    \column{0.5\textwidth}
    \includegraphics[width=\columnwidth]{figures/conclusion_color_low_z}
  \end{columns}
\end{frame}

\end{document}
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