Changeset 6675 for trunk/MagicSoft/GC-Proposal/GC.tex

Timestamp:

02/24/05 19:07:26 (20 years ago)

Author:

hbartko

Message:

GC.tex

File:

• trunk/MagicSoft/GC-Proposal/GC.tex (modified) (12 diffs)

trunk/MagicSoft/GC-Proposal/GC.tex

@@ -30 +30 @@
 Key Programs: Galactic Center / Dark Matter
 }
-\author{H. Bartko, A. Biland, S. Commichau, P. Flix, W. Wittek, \\ \texttt{<name@host>}}
+\author{H. Bartko, A. Biland, S. Commichau, P. Flix, W. Wittek}
 \date{Month dd, 2005\\}
-\TDAScode{MAGIC-TDAS 05-xx\\ 04mmdd/HBartko}
+\TDAScode{}%MAGIC 05-xx\\ 04mmdd/HBartko
 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
 
@@ -56 +56 @@
 
 
-To get a comparable data set to the other experiments and to be able to reconstruct the spectrum an observation of 20 hours plus 20 hours of dedicated OFF-data would be needed and hereby applied for. Moreover due to the large threshold moon observations are envisaged and 60 hours are applied for.
+To get a comparable data set to the other experiments and to be able to reconstruct the spectrum an observation of 20 hours plus 20 hours of dedicated OFF data would be needed and hereby applied for. Moreover due to the large threshold moon observations are envisaged and 60 hours are applied for.
 \end{abstract}
 
@@ -104 +104 @@
 \begin{figure}[h!]
 \begin{center}
-\includegraphics[totalheight=10cm]{sgr_figure4.eps}
+\includegraphics[totalheight=7cm]{sgr_figure4.eps}
 \end{center}
 \caption[Gamma flux from GC.]{The observed VHE gamma flux with the other IACTs and the EGRET satellite \cite{GC_hess}.} \label{fig:GC_gamma_flux}
@@ -112 +112 @@
 \begin{figure}[h!]
 \begin{center}
-\includegraphics[totalheight=10cm]{gc_legend.eps}
+\includegraphics[totalheight=9cm]{gc_legend.eps}
 \end{center}
 \caption[Gamma flux from GC.]{The observed VHE source locations with the other IACTs \cite{Horns2004}.} \label{fig:GC_source_location}
@@ -126 +126 @@
 
 
-\begin{table}[h]{\normalsize\center
-\begin{tabular}{lll}
+\begin{table}[h]{
+\scriptsize{%
+\centering
+\begin{tabular}{llll}
  \hline
- Investigator & Institution & Assigned task
+ Investigator & Institution& email & Assigned task
 \\
-\\ Hendrik Bartko      & MPI Munich     & data analysis, spectra
-\\ Adrian Biland       & ETH Zurich     & OFF pointing, Moon observations
-\\ Sebastian Commichau & ETH Zurich     & data analysis, MC generation
-\\ Pepe Flix           & IFAE Barcelona & data analysis, disp
-\\ Wolfgang Wittek     & MPI Munich     & padding
+\\ Hendrik Bartko      & MPI Munich    & hbartko@mppmu.mpg.de & data analysis, spectra
+\\ Adrian Biland       & ETH Zurich    & biland@particle.phys.ethz.ch & OFF pointing, Moon observations
+\\ Sebastian Commichau & ETH Zurich    & commichau@particle.phys.ethz.ch & data analysis, MC generation
+\\ Pepe Flix           & IFAE Barcelona& jflix@ifae.es & data analysis, disp
+\\ Wolfgang Wittek     & MPI Munich    & wittek@mppmu.mpg.de & padding
 \\ 
 \hline
 \end{tabular}
+}
 \caption{The investigators and assigned tasks.}\label{table:GC_investigators}}
 \end{table}
@@ -184 +187 @@
 \begin{figure}[h!]
 \begin{center}
-\includegraphics[totalheight=10cm]{Dark_exclusion_limits.eps}
+\includegraphics[totalheight=7cm]{Dark_exclusion_limits.eps}
 \end{center}
 \caption[DM exclusion limits.]{Exclusion limits for different possible sources of dark matter annihilation radiation. The galactic center is expected to give the largest flux from all sources. Due to the possible flux con} \label{fig:GC_sources}
@@ -209 +212 @@
 \end{equation}
 
-Cangaroo (own fit to Cangaroo data):
+Cangaroo (fit to Cangaroo data):
 
 \begin{equation}
@@ -220 +223 @@
 
 \begin{equation}
-\frac{\mathrm{d}N_{\gamma}(E>700 GeV)}{\mathrm{d}A\mathrm{d}t}=(3.2 \pm 1.0)\cdot 10^{-12}\frac{1}{\mathrm{cm}^2s}
+\frac{\mathrm{d}N_{\gamma}(E>700 \mathrm{GeV})}{\mathrm{d}A\mathrm{d}t}=(3.2 \pm 1.0)\cdot 10^{-12}\frac{1}{\mathrm{cm}^2s}
 \end{equation}
 
@@ -227 +230 @@
 
 \begin{equation}
-\frac{\mathrm{d}N_{\gamma}(E>700 GeV)}{\mathrm{d}A\mathrm{d}t}=(3 \pm 5)\cdot 10^{-12}\frac{1}{\mathrm{cm}^2s} \ .
+\frac{\mathrm{d}N_{\gamma}(E>700 \mathrm{GeV})}{\mathrm{d}A\mathrm{d}t}=(3 \pm 5)\cdot 10^{-12}\frac{1}{\mathrm{cm}^2s} \ .
 \end{equation}
 
@@ -236 +239 @@
 
 \begin{equation}
-\frac{\mathrm{d}N_{\gamma}(E>700 GeV)}{\mathrm{d}A\mathrm{d}t}\vline_{\mathrm{min}} \approx 6\cdot 10^{-13}\frac{1}{\mathrm{cm}^2s} \ .
+\frac{\mathrm{d}N_{\gamma}(E>700 \mathrm{GeV})}{\mathrm{d}A\mathrm{d}t}\vline_{\mathrm{min}} \approx 6\cdot 10^{-13}\frac{1}{\mathrm{cm}^2s} \ .
 \end{equation}
 
@@ -264 +267 @@
 \section{Requested Observation Time}
 
-Based on the above estimations a 5 $\sigma$ excess could be expected to be observed in about 2 hours assuming the HESS flux. To aquire a comparable data set to the other experiments at least 20 hours of good ON data and 20 hours of good dedicacted OFF data are needed. 
+Based on the above estimations a 5 $\sigma$ excess is expected to be observed in about 2 hours assuming the HESS flux. To aquire a comparable data set to the other experiments at least 20 hours of good ON data and 20 hours of good dedicated OFF data are needed. 
 
 To get the lowest possible threshold all data shall be taken under the smallest possible zenith angles between culmination at about 58 deg and 60 deg. This limits the data taking interval to about 1 hour per night between April and August. In order to have the most appropriate OFF data we propose to take OFF data each night directly before or after the ON observations under the same condition, i.e. ZA and azimuth.
 
-To extend the available observation time we propose to take moon ON and OFF data in addition. Nevertheless the proposed maximum ZA of 60 deg should not be exceeded during monn observations.
-
-In order to take part in exploring the exciting physics of the Galactic Center we propose to start taking data as soon as possible beginning in April. This way first results may be presented in the summer conferences 2005.
+To extend the available observation time we propose to take moon ON and OFF data in addition. Nevertheless the proposed maximum ZA of 60 deg should not be exceeded during moon observations.
+
+In order to take part in exploring the exciting physics of the galactic center we propose to start taking data as soon as possible beginning in April. This way first results may be presented in the summer conferences 2005.
 
 
@@ -279 +282 @@
 Conventional acceleration mechanisms are due to ... The galactic center is expected to be the brightest source of VHE gammas  from particle dark matter annihilation. Although the observed gamma radiation is most probably not due to dark matter annihilation, it is interesting to investigate and characterize the observed gamma radiation as it is not excluded that a part of the flux is due to dark matter annihilation.
 
-The MAGIC data could help to determine the nature of the source and to solve the flux discrepancies between the measurements by the other experiments. Due to the large Zenith angle MAGIC will have a large energy threshold but also a large collection area and good statistics for the highest energies. The observation results can also be used to inter-calibrate the different IACTs.
+The MAGIC data could help to determine the nature of the source and to solve the flux discrepancies between the measurements by the other experiments. Due to the large Zenith angle MAGIC will have a large energy threshold but also a large collection area and good statistics at the highest energies. The observation results can also be used to inter-calibrate the different IACTs.