Changeset 6734 for trunk/MagicSoft/GC-Proposal
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- 03/04/05 08:09:44 (20 years ago)
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trunk/MagicSoft/GC-Proposal/GC.tex (modified) (7 diffs)
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trunk/MagicSoft/GC-Proposal/GC.tex
r6726 r6734 154 154 155 155 156 High energy gamma rays can be produced in the GC in the non-thermal radio filaments by high-energy leptons which scatter background infrared photons from the nearby ionized clouds \cite{Pohl1997,Aharonian2005}, or by hadrons colliding with dense matter. These high energy hadrons can be accelerated by the massive black hole \cite{GC_black_hole}, associated with the Sgr A$^*$, supernovae or an energetic pulsar. Alternative mechanisms invoke the hypothetical annihilation of super-symmetric dark matter particles (for a review see \cite{jung96}) or curvature radiation of protons in the vicinity of the central super massive black hole \cite{}.156 High energy gamma rays can be produced in the GC in the non-thermal radio filaments by high-energy leptons which scatter background infrared photons from the nearby ionized clouds \cite{Pohl1997,Aharonian2005}, or by hadrons colliding with dense matter. These high energy hadrons can be accelerated by the massive black hole \cite{GC_black_hole}, associated with the Sgr A$^*$, supernovae or an energetic pulsar. Alternative mechanisms invoke the hypothetical annihilation of super-symmetric dark matter particles (for a review see \cite{jung96}) or curvature radiation of protons in the vicinity of the central super-massive black hole \cite{}. 157 157 158 158 … … 190 190 191 191 192 where ... is ... . The flux prediction depends on the cho ise of SUSY paramters and the spatial distribution of the dark matter. The spectra of the produced gamma radiation has a very characteristic feature a sharp cut-off at the mass of the dark matter particle. Also the flux should be absolutely stable in time.192 where ... is ... . The flux prediction depends on the choose of SUSY parameters and the spatial distribution of the dark matter. The spectra of the produced gamma radiation has a very characteristic feature a sharp cut-off at the mass of the dark matter particle. Also the flux should be absolutely stable in time. 193 193 194 194 Numerical simulations of cold dark matter \cite{NFW1997,Stoehr2002,Hayashi2004,Moore1998} predict universal DM halo profiles with density enhancement in the center of the dark halos. In the very center the dark matter density can even more enhanced through an adiabatic compression due to the baryons \cite{Prada2004}. All dark matter distributions that predict observable fluxes are very cusped yielding a point-like source. … … 196 196 Using fits of these dark matter profiles to the rotation data of the milky way predictions for the gamma flux from SUSY particle dark matter annihilation can be made \cite{Fornego2004,Evans2004}. 197 197 198 Figure \ref{fig:exclusion_lmits} shows exclusion limits taking the sensitivity of MAGIC from MC simulations into account. Due to its relative vicinity the Galactic Center yield 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 expect ion.198 Figure \ref{fig:exclusion_lmits} shows exclusion limits taking the sensitivity of MAGIC from MC simulations into account. Due to its relative vicinity the Galactic Center yield 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. 199 199 200 200 … … 207 207 208 208 209 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 favo ured mass region of the lightest SUSY particle, and the observed flux is larger than the theoretical expection 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.209 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. 210 210 211 211 … … 215 215 216 216 The Sgr A$^*$ data that has been taken in September 8, 9 and 10 2004, is 217 still being analy sed. Preliminary results were presented at the MAGIC217 still being analyzed. Preliminary results were presented at the MAGIC 218 218 collaboration meeting in Berlin, 21-25th February 2005.\\ 219 219 Up to now there is only 2.9 hours of ON data available at a very large zenith … … 241 241 energy spectrum of the Crab nebula... 242 242 243 The MC sample is divided into training s243 The MC sample is divided into training 244 244 and test sample. Since there is no dedicated OFF data available, we used a 245 245 subsample of Sgr A$^*$ ON data for the Random Forest training. As trainings … … 331 331 \section{Requested Observation Time} 332 332 333 Based on the above estimations a 5 $\sigma$ excess is expected to be observed in about 2 hours assuming the HESS flux. To a quire 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.333 Based on the above estimations a 5 $\sigma$ excess is expected to be observed in about 2 hours assuming the HESS flux. To acquire 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. 334 334 335 335 To get the lowest possible threshold all data shall be taken under the
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