207 lines
6.1 KiB
TeX
207 lines
6.1 KiB
TeX
%\documentclass[alwaysshowauthor=true,spp=2,showdate=true,slidenumbers=relative]{beamerruhuisstijl}
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\documentclass{beamer}
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\usepackage{amsmath}
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\usepackage{amssymb}
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\usepackage{tikz}
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\usepackage[english]{babel}
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%\title{Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector}
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\title{ IceCube Neutrino Astronomy }
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\author{Eric Teunis de Boone}
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\addtobeamertemplate{navigation symbols}{}{%
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\usebeamerfont{footline}%
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\usebeamercolor[fg]{footline}%
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\hspace{1em}%
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\insertframenumber
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}
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\begin{document}
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\begin{frame}[noframenumbering]
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\titlepage
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\end{frame}
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\note{}
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%%%%%%% Outline
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% History of Neutrino Astronomy - (Instruments)
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% Introduction into Neutrino Astronomy
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% + Cherenkov
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% IceCube, IceTop, DeepCore
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% + IceTop
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% + IceCube
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% + DeepCore
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%
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%
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%
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%
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%
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%%%%%%%%%%%%%%%%%%%%%
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\begin{frame}[noframenumbering]{Overview}
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\tableofcontents
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\end{frame}
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\section{ Neutrino Astronomy }
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\begin{frame}{ Why Neutrino Astronomy }
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\includegraphics[width=\textwidth]{images/icecube-3-fig9-multimessenger-spectrum.png}
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\end{frame}
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\begin{frame}{ Neutrino Astronomy: History }
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\begin{itemize}
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\item First observation of neutrino in 1956
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\item Deep Underwater Muon and Neutrino Detector, Hawaii (1990)
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failed, but proof of concept for ANTARES, KM3NeT
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\item Antarctic Muon and Neutrino Detector Array (, now part of IceCube)
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\end{itemize}
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\end{frame}
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\begin{frame}{ Neutrino Astronomy: Basics }
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\begin{itemize}
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\item Neutrino interacts in atmosphere, ice or water
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\item Charged particle gets into the ice or water and emit Cherenkov photons
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\item Cherenkov photons detected by DOMs in the matter
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\end{itemize}
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\begin{columns}[t]
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\begin{column}{0.9\textwidth}
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\begin{figure}[hbtp]
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\centering
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\includegraphics[width=\textwidth]{images/icecube-3-fig1-initial-outline.png}
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\includegraphics[width=0.3\textwidth]{images/prinicipal_idea_neutrino_telescope.png}
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\caption{\small Cherenkov cone propagating through the IceCube Detector}
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\end{figure}
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\end{column}
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\end{columns}
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\end{frame}
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\begin{frame}{ Neutrino Astronomy: Production }
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Neutrinos produced in sources and CR interactions
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\begin{itemize}
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\item Main CR interactions:
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\begin{itemize}
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\item $ p + \gamma_{bg} \to p + \pi^0 \to p + \gamma + \gamma $
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\item $ p + \gamma_{bg} \to n + \pi^+ \to n + \mu^ + \nu_\mu \to n + \nu_\mu + e^ + \bar{\nu_\mu} + \nu_e $
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\end{itemize}
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\end{itemize}
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\end{frame}
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\section{IceCube observatory}
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\begin{frame}{IceCube observatory}
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\includegraphics[width=0.9\textwidth]{images/icecube-array-fancy.png}
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\end{frame}
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\begin{frame}{IceCube observatory}
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Divided into three parts:
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\begin{itemize}
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\item IceTop: detects CR airshower above IceCube
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\item IceCube: the main detector for $E_\nu > 100$ GeV
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\item DeepCore: sensitive for $E_\nu \raise.17ex\hbox{$\scriptstyle\sim$} 10$ GeV due to tight spacing
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\end{itemize}
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\includegraphics[width=\textwidth]{images/icecube-3-fig2-architecture-and-dom.png}
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\end{frame}
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%\begin{frame}{IceCube observatory: Digital Optical Module}
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% \includegraphics[width=\textwidth]{images/icecube-4-Aartsen_2017_DOM.pdf}
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%\end{frame}
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\subsection{Event Detection and Background}
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\begin{frame}{Event Detection}
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Event selection and simulation needed to identify particles.\\
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IceTop and outer region of IceCube are veto regions.
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\begin{figure}[hbtp]
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\centering
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\includegraphics[width=0.75\textwidth]{images/icecube_veto_regions.png}
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%\caption{\ref{}}
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\end{figure}
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\end{frame}
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\begin{frame}{Event Detection}
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\begin{columns}[t]
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\begin{column}{.5\textwidth}
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\begin{block}{Tracklike}
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\begin{itemize}
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\item Distinct track -- caused by $\mu^{-}$
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\item Angular resolution $\lesssim 1\deg$
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\item Energy resolution not so good
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\end{itemize}
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\end{block}
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\end{column}
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\begin{column}{.5\textwidth}
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\begin{block}{Showerlike}
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\begin{itemize}
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\item Spherical light pattern due to well-localised particle shower
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\item Angular resolution $\sim 15\deg$
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\item Energy resolution $\sim 15\%$
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\end{itemize}
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\end{block}
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\end{column}
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\end{columns}
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\includegraphics[width=\textwidth]{images/simulation_of_cherenkov_propagation.png}
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\end{frame}
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\begin{frame}{Event Detection}
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\begin{columns}[t]
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\begin{column}{.5\textwidth}
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\begin{block}{Tracklike}
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\begin{itemize}
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\item Mostly CC of $\nu_\mu$
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\item Through-going Muons
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\end{itemize}
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\end{block}
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\end{column}
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\begin{column}{.5\textwidth}
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\begin{block}{Showerlike}
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\begin{itemize}
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\item NC of all $\nu$ flavours
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\item CC of $\nu_e$ (and $\nu_\tau$ if $E \lesssim 100 TeV$)
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\end{itemize}
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\end{block}
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\end{column}
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\end{columns}
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both: Glashow resonance of $\overline{\nu_e}$ at $E \sim 6.3 PeV$ on $e^{-}$ to $W$
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\begin{columns}[t]
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\begin{column}{.5\textwidth}
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\begin{block}{Charged Current}
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\includegraphics[width=\textwidth]{feynman_diags/charged_current.pdf}
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\end{block}
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\end{column}
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\begin{column}{.5\textwidth}
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\begin{block}{Neutral Current}
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\includegraphics[width=\textwidth]{feynman_diags/neutral_current.pdf}
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\end{block}
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\end{column}
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\end{columns}
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%\begin{figure}
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% \includegraphics[width=0.5\textwidth]{images/charged_and_neutral_neutrino_interactions.pdf}
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% \caption{From \url{http://inspirehep.net/record/1236362/files/TwoDiagrams.png}}
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%\end{figure}
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\end{frame}
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\begin{frame}{Background vs Signals}
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\begin{itemize}
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\item 2500 to 2900 events per second
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\item $\sim 10^{5}$ atmospheric neutrinos vs. $\lesssim 10^3$ cosmic neutrinos per year
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\item $10^{-6}$ events due to neutrino interaction
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\end{itemize}
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\end{frame}
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\section{High Energy Extraterrestrial Neutrinos}
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\begin{frame}{High Energy Extraterrestrial Neutrinos}
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\small{ 28 neutrino candidate events, ranging from 30 to $1200 TeV$ in a 2-year dataset }
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\includegraphics[width=\textwidth]{images/icecube-3-table1-28events.png}
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\end{frame}
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\begin{frame}{High Energy Extraterrestrial Neutrinos}
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\includegraphics[width=\textwidth]{images/icecube-3-fig3-vertical-deposition.png}
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\end{frame}
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%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
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% Appendix
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%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
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\end{document}
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