Changeset 6675 for trunk


Ignore:
Timestamp:
02/24/05 19:07:26 (20 years ago)
Author:
hbartko
Message:
GC.tex
Location:
trunk/MagicSoft/GC-Proposal
Files:
3 edited

Legend:

Unmodified
Added
Removed

  • trunk/MagicSoft/GC-Proposal/GC.log

    r6672 r6675  
    1 This is e-TeX, Version 3.14159-2.1 (Web2C 7.3.1) (format=latex 1999.10.11)  24 FEB 2005 17:52
     1This is e-TeX, Version 3.14159-2.1 (Web2C 7.3.1) (format=latex 1999.10.11)  24 FEB 2005 19:06
    22**GC.tex
    33(GC.tex
    … …  
    293293
    294294[4]
    295 Overfull \vbox (2.49998pt too high) has occurred while \output is active []
    296 
    297 
    298 [5]
    299295File: Dark_exclusion_limits.eps Graphic file (type eps)
    300296 <Dark_exclusion_limits.eps>
     297
     298LaTeX Warning: `!h' float specifier changed to `!ht'.
     299
     300
     301Overfull \vbox (2.49998pt too high) has occurred while \output is active []
     302
     303
     304[5]
    301305Overfull \vbox (2.49998pt too high) has occurred while \output is active []
    302306
    … …  
    320324 )
    321325Here is how much of TeX's memory you used:
    322  2239 strings out of 10789
    323  25339 string characters out of 71018
     326 2237 strings out of 10789
     327 25316 string characters out of 71018
    324328 81354 words of memory out of 263001
    325  5129 multiletter control sequences out of 10000+0
    326  15172 words of font info for 59 fonts, out of 400000 for 1000
     329 5128 multiletter control sequences out of 10000+0
     330 15003 words of font info for 58 fonts, out of 400000 for 1000
    327331 14 hyphenation exceptions out of 1000
    328332 39i,11n,27p,734b,450s stack positions out of 300i,100n,500p,50000b,4000s
    329333
    330 Output written on GC.dvi (9 pages, 21592 bytes).
     334Output written on GC.dvi (9 pages, 21588 bytes).

  • trunk/MagicSoft/GC-Proposal/GC.tex

    r6674 r6675  
    3030Key Programs: Galactic Center / Dark Matter
    3131}
    32 \author{H. Bartko, A. Biland, S. Commichau, P. Flix, W. Wittek, \\ \texttt{<name@host>}}
     32\author{H. Bartko, A. Biland, S. Commichau, P. Flix, W. Wittek}
    3333\date{Month dd, 2005\\}
    34 \TDAScode{MAGIC-TDAS 05-xx\\ 04mmdd/HBartko}
     34\TDAScode{}%MAGIC 05-xx\\ 04mmdd/HBartko
    3535%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
    3636
    … …  
    5656
    5757
    58 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.
     58To 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.
    5959\end{abstract}
    6060
    … …  
    104104\begin{figure}[h!]
    105105\begin{center}
    106 \includegraphics[totalheight=10cm]{sgr_figure4.eps}
     106\includegraphics[totalheight=7cm]{sgr_figure4.eps}
    107107\end{center}
    108108\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}
    … …  
    112112\begin{figure}[h!]
    113113\begin{center}
    114 \includegraphics[totalheight=10cm]{gc_legend.eps}
     114\includegraphics[totalheight=9cm]{gc_legend.eps}
    115115\end{center}
    116116\caption[Gamma flux from GC.]{The observed VHE source locations with the other IACTs \cite{Horns2004}.} \label{fig:GC_source_location}
    … …  
    126126
    127127
    128 \begin{table}[h]{\normalsize\center
    129 \begin{tabular}{lll}
     128\begin{table}[h]{
     129\scriptsize{%
     130\centering
     131\begin{tabular}{llll}
    130132 \hline
    131  Investigator & Institution & Assigned task
     133 Investigator & Institution& email & Assigned task
    132134\\
    133 \\ Hendrik Bartko      & MPI Munich    & data analysis, spectra
    134 \\ Adrian Biland       & ETH Zurich    & OFF pointing, Moon observations
    135 \\ Sebastian Commichau & ETH Zurich    & data analysis, MC generation
    136 \\ Pepe Flix           & IFAE Barcelona & data analysis, disp
    137 \\ Wolfgang Wittek     & MPI Munich    & padding
     135\\ Hendrik Bartko      & MPI Munich    & hbartko@mppmu.mpg.de & data analysis, spectra
     136\\ Adrian Biland       & ETH Zurich    & biland@particle.phys.ethz.ch & OFF pointing, Moon observations
     137\\ Sebastian Commichau & ETH Zurich    & commichau@particle.phys.ethz.ch & data analysis, MC generation
     138\\ Pepe Flix           & IFAE Barcelona& jflix@ifae.es & data analysis, disp
     139\\ Wolfgang Wittek     & MPI Munich    & wittek@mppmu.mpg.de & padding
    138140\\
    139141\hline
    140142\end{tabular}
     143}
    141144\caption{The investigators and assigned tasks.}\label{table:GC_investigators}}
    142145\end{table}
    … …  
    184187\begin{figure}[h!]
    185188\begin{center}
    186 \includegraphics[totalheight=10cm]{Dark_exclusion_limits.eps}
     189\includegraphics[totalheight=7cm]{Dark_exclusion_limits.eps}
    187190\end{center}
    188191\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}
    … …  
    209212\end{equation}
    210213
    211 Cangaroo (own fit to Cangaroo data):
     214Cangaroo (fit to Cangaroo data):
    212215
    213216\begin{equation}
    … …  
    220223
    221224\begin{equation}
    222 \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}
     225\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}
    223226\end{equation}
    224227
    … …  
    227230
    228231\begin{equation}
    229 \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} \ .
     232\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} \ .
    230233\end{equation}
    231234
    … …  
    236239
    237240\begin{equation}
    238 \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} \ .
     241\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} \ .
    239242\end{equation}
    240243
    … …  
    264267\section{Requested Observation Time}
    265268
    266 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.
     269Based 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.
    267270
    268271To 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.
    269272
    270 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.
    271 
    272 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.
     273To 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.
     274
     275In 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.
    273276
    274277
    … …  
    279282Conventional 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.
    280283
    281 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.
     284The 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.
    282285
    283286

  • trunk/MagicSoft/GC-Proposal/GC.toc

    r6672 r6675  
    11\select@language {english}
    22\contentsline {section}{\numberline {1}Introduction}{3}
    3 \contentsline {section}{\numberline {2}Investigators and Affiliations}{4}
     3\contentsline {section}{\numberline {2}Investigators and Affiliations}{5}
    44\contentsline {section}{\numberline {3}Scientific Case}{5}
    55\contentsline {subsection}{\numberline {3.1}Leptonic Models}{5}
    66\contentsline {subsection}{\numberline {3.2}Hadronic Models}{5}
    77\contentsline {subsection}{\numberline {3.3}Dark Matter}{5}
    8 \contentsline {section}{\numberline {4}Preparatory Work}{6}
     8\contentsline {section}{\numberline {4}Preparatory Work}{5}
    99\contentsline {section}{\numberline {5}Feasibility}{6}
    1010\contentsline {section}{\numberline {6}Observational Constraints}{7}
    11 \contentsline {section}{\numberline {7}Requested Observation Time}{8}
     11\contentsline {section}{\numberline {7}Requested Observation Time}{7}
    1212\contentsline {section}{\numberline {8}Outlook and Conclusions}{8}
    1313\contentsline {section}{\numberline {A}Acknowledgements}{8}
Note: See TracChangeset for help on using the changeset viewer.