Changeset 6715


Ignore:
Timestamp:
03/03/05 09:40:59 (20 years ago)
Author:
commichau
Message:
*** empty log message ***
Location:
trunk/MagicSoft/GC-Proposal
Files:
1 added
2 edited

Legend:

Unmodified
Added
Removed
  • trunk/MagicSoft/GC-Proposal/Changelog

    r6690 r6715  
     1
     22005/03/03
     3* committed GC_sources figure of better quality
     4  started to fill the Preparatory Work section - to be finished!
    15
    262005/03/01  Sebastian
  • trunk/MagicSoft/GC-Proposal/GC.tex

    r6690 r6715  
    99
    1010\usepackage{graphicx}
    11 
     11\usepackage{tabularx}
     12\usepackage{hhline}
    1213\usepackage{url}
     14\usepackage{subfigure}
    1315
    1416\setlength{\parindent}{0cm}
     
    98100\begin{figure}[h!]
    99101\begin{center}
    100 \includegraphics[totalheight=10cm]{GC_sources.eps}
     102\includegraphics[totalheight=9cm]{GC_sources_1.eps}
    101103\end{center}
    102104\caption[Sources near the Galactic Center.]{Overview about the sources near the Galactic Center \cite{GC_overview}.} \label{fig:GC_sources}
     
    108110\begin{figure}[h!]
    109111\begin{center}
    110 \includegraphics[totalheight=7cm]{sgr_figure4.eps}
     112\includegraphics[totalheight=6cm]{sgr_figure4.eps}
    111113\end{center}
    112114\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}
     
    116118\begin{figure}[h!]
    117119\begin{center}
    118 \includegraphics[totalheight=9cm]{gc_legend.eps}
     120\includegraphics[totalheight=8cm]{gc_legend.eps}
    119121\end{center}
    120122\caption[Gamma flux from GC.]{The observed VHE source locations with the other IACTs \cite{Horns2004}.} \label{fig:GC_source_location}
     
    135137\begin{tabular}{llll}
    136138 \hline
    137  Investigator & Institution& E-mail & Assigned task
    138 \\
    139 \\ Hendrik Bartko      & MPI Munich    & hbartko@mppmu.mpg.de & data analysis, spectra
     139 Investigator & Institution& E-mail & Assigned task\\ \hline
     140   Hendrik Bartko      & MPI Munich    & hbartko@mppmu.mpg.de & data analysis, spectra
    140141\\ Adrian Biland       & ETH Zurich    & biland@particle.phys.ethz.ch & OFF pointing, Moon observations
    141142\\ Sebastian Commichau & ETH Zurich    & commichau@particle.phys.ethz.ch &
     
    189190\begin{figure}[h!]
    190191\begin{center}
    191 \includegraphics[totalheight=7cm]{Dark_exclusion_limits.eps}
     192\includegraphics[totalheight=6cm]{Dark_exclusion_limits.eps}
    192193\end{center}
    193194\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}
    194195\end{figure}
    195196
    196 
    197 
     197\newpage
    198198\section{Preparatory Work}
    199199
    200 
    201 First analysis by Sebastian
    202 is not yet finished...
    203 
     200The Sgr A$^*$ data that has been taken in September 8, 9 and 10 2004, is
     201still being analysed. Preliminary results were presented at the MAGIC
     202collaboration meeting in Berlin, 21-25th February 2005.\\
     203Up to now there is only 2.9 hours of ON data available at a very large zenith
     204angle range. Some details of the data set are shown in table \ref{table:GC_dataset}.\\
     205
     206\begin{table}[!ht]{
     207\centering{
     208\begin{tabular}{l|l|l|l}
     209 \hline
     210   Date       & Time          & Az $[^\circ]$ & Zd $[^\circ]$\\ \hline
     211   09/08/2004 & 21:00 - 22:00 & 198.3 - 214.7 & 60.3 - 67.8
     212\\ 09/09/2004 & 21:17 - 22:12 & 203.4 - 214.7 & 62.2 - 67.7
     213\\ 09/10/2004 & 21:06 - 22:03 & 202.2 - 213.7 & 61.6 - 67.1
     214\\
     215\hline
     216\end{tabular}
     217\caption{The Sgr A$^*$ data set from September 2004.}\label{table:GC_dataset}}}
     218\end{table}
     219
     220In our preliminary analysis we used the Random Forest method for the gamma
     221hadron separation. For this purpose high
     222ZA (65$^\circ$ Zd and 205$^\circ$ Az) Monte Carlo gammas were generated,
     22399500 events in all, with energies between 200
     224and 30,000 GeV. The slope of the generated spectrum is $-2.6$, conforming the
     225energy spectrum of the Crab nebula...
     226
     227The MC sample is divided into trainings
     228and test sample. Since there is no dedicated OFF data available, we used a
     229subsample of Sgr A$^*$ ON data for the Random Forest training. As trainings
     230parameters we used SIZE, DIST, WIDTH, LENGTH, CONC, and M3Long...
     231
     232
     233%\begin{figure}[!h]
     234%\centering
     235%\subfigure[The Hadronness distribution.]{
     236%\includegraphics[scale= .3]{hadronness}}
     237%\subfigure[SIZE $> 300$ Phe]{
     238%\includegraphics[scale= .3]{size300}}
     239%\subfigure[SIZE $> 500$ Phe]{
     240%\includegraphics[scale= .3]{size500}}
     241%\subfigure[SIZE $> 1000$ Phe]{
     242%\includegraphics[scale= .3]{size1000}}
     243%\caption{Hadronness distribution and ALPHA plots for three different lower SIZE cuts. The
     244%  Hadronness cut is made at 0.4.}\label{fig:prelresults}
     245%\end{figure}
    204246
    205247
Note: See TracChangeset for help on using the changeset viewer.