Changeset 6780 for trunk/MagicSoft

Timestamp:

03/08/05 09:07:47 (20 years ago)

Author:

hbartko

Message:

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File:

• trunk/MagicSoft/GC-Proposal/GC.tex (modified) (3 diffs)

trunk/MagicSoft/GC-Proposal/GC.tex

@@ -256 +256 @@
 One scenario is related to protons accelerated to about $10^{18}$ eV \cite{Aharonian2005}. These protons produce gamma rays via photo-meson processes. This scenario also predicts detectable fluxes of  $10^{18}$ eV neutrons and perhaps gamma rays and neutrinos. A hint of an excess of highest energy neutrons from the galactic center has been reported in \cite{Hayashida1999}.
 
-TeV gamma rays can also be produced by significantly  lower energy protons, accelerated by the electric filed close to the gravitational radius or by strung shocks in the accretion disk. In this case the gamma-ray production is dominated by interactions of $10^{13}$ eV protons with the accretion plasma. This scenario predicts a neutrino flux which should be observable with northern neutrino telescopes like NEMO. It also predicts strong TeV--X-ray--IR correlations.
+TeV gamma rays can also be produced by significantly  lower energy protons, accelerated by the electric filed close to the gravitational radius or by strong shocks in the accretion disk. In this case the gamma-ray production is dominated by interactions of $10^{13}$ eV protons with the accretion plasma. This scenario predicts a neutrino flux which should be observable with northern neutrino telescopes like NEMO. It also predicts strong TeV--X-ray--IR correlations.
 
 
@@ -282 +282 @@
 Figure \ref{fig:exclusion_lmits} shows exclusion limits for MAGIC (straight lines) for the four most promising sources
 %taking the sensitivity of MAGIC from MC simulations into account for different sources and predictions from typical allowed SUSY models 
-in the plane $N_{\gamma}(E_{\gamma}>E_{\mathrm{thresh}})\langle \sigma v \rangle$ vs. $m_{\chi}$. Due to its proximity the Galactic Center yields the largest expected flux from particle dark matter annihilation. Nevertheless this flux is more than one order of magnitude below the current MAGIC sensitivity. Also the observed flux from the HESS experiment way above the theoretical expectation.
+in the plane $N_{\gamma}(E_{\gamma}>E_{\mathrm{thresh}})\langle \sigma v \rangle$ vs. $m_{\chi}$. Due to its proximity the Galactic Center yields the largest expected flux from particle dark matter annihilation. Nevertheless this flux is more than one order of magnitude below the current MAGIC sensitivity. Also the observed flux from the HESS experiment is way above the theoretical expectation.
 
 
@@ -293 +293 @@
 
 
-Detailed discussion of the observed gamma flux from the Galactic Center can be found in \cite{Hooper2004,Horns2004}. The observed spectrum extends to more than 18 TeV, well beyond the favored mass region of the lightest SUSY particle, and the observed flux is larger than the theoretical expectation in most models. This leads to the conclusion that most likely the dominating part of the observed gamma flux from the Galactic Center is not due to SUSY particle Dark Matter annihilation. Other dark matter scenarios like Kaluza-Klein Dark Matter can not be excluded.
+Detailed discussion of the observed gamma flux from the Galactic Center can be found in \cite{Hooper2004,Horns2004}. The observed spectrum extends to more than 18 TeV, well beyond the favored mass region of the lightest SUSY particle, and the observed flux is larger than the theoretical expectation in most models. This leads to the conclusion that most likely the dominating part of the observed gamma flux from the Galactic Center is not due to SUSY particle Dark Matter annihilation. Other dark matter scenarios like Kaluza-Klein Dark Matter cannot be excluded.