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Moving to Science computers

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Eric Teunis de Boone 2019-05-23 11:50:57 +02:00
parent f501c0cb3f
commit 18ca312dcd
2 changed files with 55 additions and 18 deletions
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presentation/images/charged_and_neutral_neutrino_interactions.pdf
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presentation/presentation.tex
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@ -2,8 +2,9 @@
\documentclass{beamer} \documentclass{beamer}
\usepackage{amsmath} \usepackage{amsmath}
\usepackage{amssymb}
\usepackage{tikz} \usepackage{tikz}
%\usepackage[english]{babel} \usepackage[english]{babel}
%\title{Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector} %\title{Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector}
\title{ IceCube Neutrino Astronomy } \title{ IceCube Neutrino Astronomy }
@ -19,7 +20,7 @@
\begin{document} \begin{document}
\begin{frame} \begin{frame}[noframenumbering]
\titlepage \titlepage
\end{frame} \end{frame}
\note{} \note{}
@ -39,12 +40,12 @@
% %
% %
%%%%%%%%%%%%%%%%%%%%% %%%%%%%%%%%%%%%%%%%%%
\begin{frame}{Overview} \begin{frame}[noframenumbering]{Overview}
\tableofcontents \tableofcontents
\end{frame} \end{frame}
\section{ Neutrino Astronomy } \section{ Neutrino Astronomy }
\begin{frame}{ History of Neutrino Astronomy } \begin{frame}{ Neutrino Astronomy: History }
\begin{itemize} \begin{itemize}
\item First observation of neutrino in 1956 \item First observation of neutrino in 1956
\item Deep Underwater Muon and Neutrino Detector, Hawaii (1990) \item Deep Underwater Muon and Neutrino Detector, Hawaii (1990)
@ -54,7 +55,7 @@
\end{itemize} \end{itemize}
\end{frame} \end{frame}
\begin{frame}{ Basics of Neutrino Astronomy} \begin{frame}{ Neutrino Astronomy: Basics }
\begin{itemize} \begin{itemize}
\item Neutrino interacts in atmosphere, ice or water \item Neutrino interacts in atmosphere, ice or water
\item Charged particle gets into the ice or water and emit Cherenkov photons \item Charged particle gets into the ice or water and emit Cherenkov photons
@ -70,16 +71,13 @@
\end{column} \end{column}
\end{columns} \end{columns}
\end{frame} \end{frame}
\begin{frame}{ Production of Neutrinos } \begin{frame}{ Neutrino Astronomy: Production }
Many sources of neutrinos Neutrinos produced in sources and CR interactions
\begin{itemize} \begin{itemize}
\item CR interactions: \item Main CR interactions:
\begin{itemize} \begin{itemize}
\item \begin{equation*} p + \gamma_{bg} \to p + \pi^0 \to p + \gamma + \gamma \item $ p + \gamma_{bg} \to p + \pi^0 \to p + \gamma + \gamma $
\end{equation*} \item $ p + \gamma_{bg} \to n + \pi^+ \to n + \mu^ + \nu_\mu \to n + \nu_\mu + e^ + \bar{\nu_\mu} + \nu_e $
\item \begin{equation*}
p + \gamma_{bg} \to n + \pi^+ \to n + \mu^ + \nu_\mu \to n + \nu_\mu + e^ + \bar{\nu_\mu} + \nu_e
\end{equation*}
\end{itemize} \end{itemize}
\end{itemize} \end{itemize}
\end{frame} \end{frame}
@ -99,6 +97,9 @@ p + \gamma_{bg} \to n + \pi^+ \to n + \mu^ + \nu_\mu \to n + \nu_\mu + e^ + \bar
\end{itemize} \end{itemize}
\end{frame} \end{frame}
\begin{frame}{IceCube observatory: Digital Optical Module}
\includegraphics[width=\textwidth]{images/icecube-4-Aartsen_2017_DOM.pdf}
\end{frame}
\subsection{Event Detection and Background} \subsection{Event Detection and Background}
@ -114,14 +115,46 @@ p + \gamma_{bg} \to n + \pi^+ \to n + \mu^ + \nu_\mu \to n + \nu_\mu + e^ + \bar
\end{frame} \end{frame}
\begin{frame}{Event Detection} \begin{frame}{Event Detection}
\begin{itemize} \begin{columns}[t]
\item Tracklike: distinct track \begin{column}{.5\textwidth}
\item Showerlike: spherical light pattern due to well-localised particle shower \begin{block}{Tracklike}
\end{itemize} \begin{itemize}
\item Distinct track -- caused by $\mu^{-}$
\item Angular resolution $\lesssim 1\deg$
\item Energy resolution not so good
\end{itemize}
\end{block}
\end{column}
\begin{column}{.5\textwidth}
\begin{block}{Showerlike}
\begin{itemize}
\item Spherical light pattern due to well-localised particle shower
\item Angular resolution $\sim 15\deg$
\item Energy resolution $\sim 15\%$
\end{itemize}
\end{block}
\end{column}
\end{columns}
\includegraphics[width=\textwidth]{images/simulation_of_cherenkov_propagation.png} \includegraphics[width=\textwidth]{images/simulation_of_cherenkov_propagation.png}
\end{frame} \end{frame}
\begin{frame}{Event Detection} \begin{frame}{Event Detection}
\begin{columns}[t]
\begin{column}{.5\textwidth}
\begin{block}{Tracklike}
\begin{itemize}
\item d
\end{itemize}
\end{block}
\end{column}
\begin{column}{.5\textwidth}
\begin{block}{Showerlike}
\begin{itemize}
\item d
\end{itemize}
\end{block}
\end{column}
\end{columns}
\begin{columns}[t] \begin{columns}[t]
\begin{column}{.5\textwidth} \begin{column}{.5\textwidth}
@ -144,7 +177,11 @@ p + \gamma_{bg} \to n + \pi^+ \to n + \mu^ + \nu_\mu \to n + \nu_\mu + e^ + \bar
\end{frame} \end{frame}
\begin{frame}{Background} \begin{frame}{Background}
$10^{-6}$ events due to neutrino interaction \begin{itemize}
\item 2500 to 2900 events per second
\item $\sim 10^{5}$ atmospheric neutrinos vs. $\lesssim 10^3$ cosmic neutrinos per year
\item $10^{-6}$ events due to neutrino interaction
\end{itemize}
\end{frame} \end{frame}