Changeset 6835 for trunk/MagicSoft/GC-Proposal

Timestamp:

03/16/05 15:20:50 (20 years ago)

Author:

hbartko

Message:

*** empty log message ***

Location:

trunk/MagicSoft/GC-Proposal

Files:

• Changelog (modified) (1 diff)
• GC.tex (modified) (6 diffs)
• bibbib.bib (modified) (1 diff)

trunk/MagicSoft/GC-Proposal/Changelog

@@ +1 @@
+2005/03/16 Hendrik
+* GC.tex:
+  added E. Bisesi as author
+  some text modifications
+* bibbib.bib
+  new referece for Random Forrest
+
+2005/03/15 Wolfgang
+* GC.tex:
+  new text for Observation Mode
 
 2005/03/09 Sebastian

trunk/MagicSoft/GC-Proposal/GC.tex

@@ -274 +274 @@
 
 
-where $\langle \sigma v \rangle$ is the thermally averaged annihilation cross section, $m_{\chi}$ the mass and $\rho_{\chi}$ the spatial density distribution of the hypothetical dark matter particles. $N_{\gamma}(E_{\gamma}>E_{\mathrm{th}})$ is the gamma yield above the threshold energy per annihilation. The predicted flux depends on the SUSY parameters and on the spatial distribution of the dark matter. The energy spectrum 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.
-
-Numerical simulations of cold dark matter \cite{NFW1997,Stoehr2002,Hayashi2004,Moore1998} predict universal DM halo profiles with a density enhancement in the center of the dark halos. In the very center the dark matter density can be even more enhanced through an adiabatic compression due to the baryons \cite{Prada2004} present. All dark matter distributions that predict observable fluxes are cusped, yielding an approximately point-like source.
+where $\langle \sigma v \rangle$ is the thermally averaged annihilation cross section, $m_{\chi}$ the mass and $\rho_{\chi}$ the spatial density distribution of the hypothetical dark matter particles. $N_{\gamma}(E_{\gamma}>E_{\mathrm{th}})$ is the gamma yield above the threshold energy per annihilation. The predicted flux depends on the SUSY parameters and on the spatial distribution of the dark matter. The energy spectrum 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.
+
+Numerical simulations of cold dark matter \cite{NFW1997,Stoehr2002,Hayashi2004,Moore1998} predict universal DM halo profiles with a density enhancement in the center of the dark halo. In the very center the dark matter density can be even more enhanced through an adiabatic compression due to the baryons \cite{Prada2004} present. All dark matter distributions that predict observable fluxes are cusped, yielding an approximately point-like source.
 
 Using fits of these dark matter profiles to the rotation data of the Milky Way predictions for the density profile $\rho_{\chi}$ of the dark matter can be made \cite{Fornego2004,Evans2004}. On the other hand, for a given choice of SUSY parameters $m_{\chi},\;\langle \sigma v \rangle$ and $N_{\gamma}$ are determined. 
@@ -323 +323 @@
 \end{table}
 
-In our preliminary analysis we used the Random Forest method for the gamma
+In our preliminary analysis we used the Random Forest method \cite{RF} for the gamma
 hadron separation. For this purpose high
-ZA (65$^\circ$ ZA and 205$^\circ$ Az) Monte Carlo gammas were generated, 
+ZA (65$^\circ$ ZA and 205$^\circ$ Az) Monte Carlo gammas showers were generated, 
 99500 events in all, with energies between 200
 and 30,000 GeV. The differential spectral index of the generated spectrum is $-2.6$, conforming with the energy spectrum of the Crab nebula.
@@ -400 +400 @@
 
 
-Figure \ref{fig:MAGIC_flux_limits} shows the HESS and Cangaroo fluxes together with the minimum flux detectable by MAGIC in 20 hours observation time.
+Figure \ref{fig:MAGIC_flux_limits} shows the measured HESS and Cangaroo fluxes together with the minimum flux detectable by MAGIC in 20 hours observation time.
 
 
@@ -429 +429 @@
 
 
-The GC culminates at about 58 deg ZA in La Palma. Below 60 deg ZA, it is visible between April and late August for about 150 hours. The GC region has a quite high level of background light from the night sky. This together with the large ZA requires to take either dedicated OFF data or to take data in the wobble mode (see Section \ref{section:skydirections}). 
+The GC culminates at about 58 deg ZA in La Palma. Below 60 deg ZA, it is visible between April and late August for about 150 hours. The GC region has a quite high and non-uniform level of background light from the night sky. This together with the large ZA requires to take either dedicated OFF data or to take data in the wobble mode (see Section \ref{section:skydirections}). 
 %Since the LONS level is in any case very large moon observations are considered in addition to the normal observations.
-
-
-\section{Requested Observation Time}
-
-Based on the above estimates a 5$\sigma$ excess is expected to be observed in about 2 hours, under optimal conditions. To acquire a data set which is comparable in size to those of the other experiments at least 40 hours of observation time are requested. These 40 hours may be either split into 20 hours ON and 20 hours OFF data taking or be devoted exclusively to data taking in the wobble mode. At present, the prefered mode is the wobble mode. However, a final decision has not yet been taken.
-
-As pointed out in Section \ref{section:feasibility}, all data should be taken at 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. 
-
-
-To increase statistics we propose to take data during moonshine in addition. Also in this case, the maximum ZA of 60 deg should not be exceeded.
-
-In order to take part in exploring the exciting physics of the GC
-we propose to start taking data as soon as possible, beginning in April. In this way first results may be available at the time of the summer conferences 2005.
 
 
@@ -518 +502 @@
 
 
+\section{Requested Observation Time}
+
+Based on the above estimates, a 5$\sigma$ excess is expected to be observed in about 2 hours, under optimal conditions. To acquire a data set which is comparable in size to those of the other experiments at least 40 hours of observation time are requested. These 40 hours may be either split into 20 hours ON and 20 hours OFF data taking or be devoted exclusively to data taking in the wobble mode. At present, the prefered mode is the wobble mode. However, a final decision has not yet been taken.
+
+As pointed out in Section \ref{section:feasibility}, all data should be taken at 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. 
+
+
+To increase statistics we propose to take data during moonshine in addition. Also in this case, the maximum ZA of 60 deg should not be exceeded.
+
+In order to take part in exploring the exciting physics of the GC
+we propose to start taking data as soon as possible, beginning in April. In this way first results may be available at the time of the summer conferences 2005.
+
+
 
 \section{Outlook and Conclusions}
@@ -540 +540 @@
 The authors thank A. Moralejo for helpful discussions about the Monte Carlo simulations. 
 
-\newpage
+%\newpage
 
 \bibliography{bibbib}

trunk/MagicSoft/GC-Proposal/bibbib.bib

@@ +1 @@
+@Article{RF,
+     author    = "Bock, R. K. and others",
+     title     = "Methods for multidimensional event classification: A case
+                  study using images from a Cherenkov gamma-ray telescope",
+     journal   = "Nucl. Instrum. Meth.",
+     volume    = "A516",
+     year      = "2004",
+     pages     = "511-528",
+     SLACcitation  = "%%CITATION = NUIMA,A516,511;%%"
+}
+
 @Article{Hooper2002,
      author    = "Hooper, Dan and Dingus, Brenda",