diff --git a/documents/thesis/chapters/introduction.tex b/documents/thesis/chapters/introduction.tex
index 3883707..b8c8ae9 100644
--- a/documents/thesis/chapters/introduction.tex
+++ b/documents/thesis/chapters/introduction.tex
@@ -8,7 +8,7 @@
 }
 
 \begin{document}
-\chapter{Introduction}
+\chapter{Cosmic Rays and Extensive Air Showers}
 \label{sec:introduction}
 %<<<
 % Intro Cosmic Ray
@@ -20,7 +20,7 @@ With many discoveries following, the field of (astro-)particle physics evolved.
 Large collaborations are now detecting cosmic rays with a variety of methods over a large range of energy (see Figure~\ref{fig:cr_flux}).
 \\
 % Radio
-In the last decade, the detection using radio antennas has received significant attention \Todo{ref}, such that collaborations such as the~\gls{GRAND}\Todo{more?} are building observatoria that fully rely on radio measurements.
+In the last two decades, the detection using radio antennas has received significant attention \Todo{ref}, such that collaborations such as the~\gls{GRAND}\Todo{more?} are building observatoria that fully rely on radio measurements.
 %
 For such radio arrays, the analyses require an accurate timing of signals within the array.
 Generally, \glspl{GNSS} are used to synchronise the detectors.
@@ -68,9 +68,10 @@ Unfortunately, this weak interaction also troubles the detection of the neutrino
 	\includegraphics[width=\textwidth]{astroparticle/The_CR_spectrum_2023.pdf}
 	\caption{
 		From \protect \cite{The_CR_spectrum}.
-		The diffuse cosmic ray spectrum as measured by various experiments.
+		The diffuse cosmic ray spectrum (upper line) as measured by various experiments.
 		The intensity and fluxes can generally be described by rapidly decreasing power laws.
-		The grey shading indicates the order of magnitude of the particle flux, such that from the ankle onwards ($E>10^9\GeV$) the flux reaches $1/km^2/yr$.
+		The grey shading indicates the order of magnitude of the particle flux, such that from the ankle onwards ($E>10^9\GeV$) the flux reaches $1$~particle per~square~kilometer per~year.
+		\protect \Todo{Knee - (inter)galactic}
 	}
 	\label{fig:cr_flux}
 \end{figure}%>>>
@@ -79,7 +80,7 @@ Unfortunately, this weak interaction also troubles the detection of the neutrino
 % Energy
 Cosmic rays span a large range of energy and flux as illustrated in Figure~\ref{fig:cr_flux}.
 At lower energies, the flux is high enough for direct detection.
-At energies above $10^{6}\GeV$, the flux decrease requires indirect detection methods.
+At energies above $10^{6}\GeV$, however, the flux decrease requires indirect detection to obtain decent statistics.
 \\
 % Acceleration
 The acceleration of high energy cosmic rays is thought to occur in highly energetic regions.