Index: trunk/MagicSoft/GC-Proposal/Changelog =================================================================== --- trunk/MagicSoft/GC-Proposal/Changelog (revision 6851) +++ trunk/MagicSoft/GC-Proposal/Changelog (revision 6852) @@ -1,2 +1,10 @@ +2005/03/18 Sebastian +* GC.tex + Did some small corrections. Results of the preliminary analysis changed + and added two ALPHA plots for two different lower cuts in SIZE. +* added and committed the files + alpha_tmpl_s100_h006.eps and alpha_tmpl_s800_h02.eps + to the repository + 2005/03/16 Hendrik * GC.tex: Index: trunk/MagicSoft/GC-Proposal/GC.tex =================================================================== --- trunk/MagicSoft/GC-Proposal/GC.tex (revision 6851) +++ trunk/MagicSoft/GC-Proposal/GC.tex (revision 6852) @@ -62,5 +62,6 @@ At La Palma, the GC culminates at about 58 deg zenith angle (ZA). It can be observed with MAGIC at up to 60 deg ZA, between -April and late August, yielding a total of 150 hours per year. The expected integral flux above 700 GeV derived from +April and late August, yielding a total of 150 hours without moon per year. +The expected integral flux above 700 GeV derived from the HESS data is $(3.2 \pm 1.0)\cdot 10^{-12}\mathrm{cm}^{-2}\mathrm{s}^{-1}$. Comparing this to the expected MAGIC sensitivity from MC simulations, this @@ -69,5 +70,5 @@ The observations have to be conducted as early as possible in order to participate in the ongoing discussion about gamma radiation from the GC. -The main motivations for the observation of the GC are : +The main motivations for the observation of the GC are: \begin{itemize} @@ -84,5 +85,5 @@ In order to collect a data sample comparable in size to those of the other experiments and to be able to measure the energy spectrum, 40 hours of -observation time are requested. The 40 hours will be split into 20 hours ON +observation time are requested. This 40 hours will be split into 20 hours ON and 20 hours dedicated OFF data or they will be devoted to observations in the wobble mode. In addition, 60 hours of observation during moonshine are @@ -166,5 +167,7 @@ \end{figure} -The discrepancies between the measured flux spectra could indicate inter-calibration problems between the IACTs. It could indicate an apparent source variability of the order of one year or it could be due to the different regions in which the signal is integrated. +The discrepancies between the measured flux spectra could indicate +inter-calibration problems between the IACTs. But it could also indicate an +apparent source variability at a timescale of about of one year or it could be due to the different regions in which the signal is integrated. @@ -185,8 +188,8 @@ Investigator & Institution& E-mail & Assigned task\\ \hline Hendrik Bartko & MPI Munich & hbartko@mppmu.mpg.de & data analysis, spectra, wobble mode -\\ Adrian Biland & ETH Zurich & biland@particle.phys.ethz.ch & OFF pointing, Moon observations -\\ Erica Bisesi & Univ. Udine & bisesi@fisica.uniud.it & dark matter halo modelling, clumpness +\\ Adrian Biland & ETH Zurich & biland@particle.phys.ethz.ch & MC generation, Moon observations +\\ Erica Bisesi & Univ. Udine & bisesi@fisica.uniud.it & dark matter halo modelling, clumpness \\ Sebastian Commichau & ETH Zurich & commichau@particle.phys.ethz.ch & - data analysis, MC generation, spectra + data analysis, spectra, geomagnetic effects \\ Pepe Flix & IFAE Barcelona& jflix@ifae.es & data analysis, disp, spectra, dark matter \\ Sabrina Stark & ETH Zurich & lstark@particle.phys.ethz.ch & data analysis, spectra @@ -227,6 +230,6 @@ \begin{itemize} \item{source location, source extension} -\item{time variability of the gamma flux} -\item{energy spectrum.} +\item{energy spectrum} +\item{time variability of the gamma flux.} \end{itemize} @@ -258,5 +261,5 @@ \subsubsection{Hadronic Models} -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 GC has been reported in \cite{Hayashida1999}. +Another 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 GC 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 of the black hole or by strong shocks in the accretion disk \cite{Aharonian2005}. 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 and Antares. It also predicts strong TeV--X-ray--IR correlations. @@ -318,6 +321,6 @@ \hline Date & Time & Az $[^\circ]$ & ZA $[^\circ]$\\ \hline - 09/08/2004 & 21:00 - 22:00 & 198.3 - 214.7 & 60.3 - 67.8 -\\ 09/09/2004 & 21:17 - 22:12 & 203.4 - 214.7 & 62.2 - 67.7 + 09/08/2004 & 21:00 - 22:16 & 198.3 - 214.7 & 60.3 - 67.8 +\\ 09/09/2004 & 21:17 - 22:12 & 203.4 - 214.7 & 62.0 - 67.7 \\ 09/10/2004 & 21:06 - 22:03 & 202.2 - 213.7 & 61.6 - 67.1 \\ @@ -334,26 +337,28 @@ The MC sample was divided into a training -and a test sample. Since no dedicated OFF data were available, we used a +and a test sample and its slope was normalized to $-2.21$. Since no dedicated OFF data were available, we used a subsample of Sgr A$^*$ ON data to represent the hadronic background in the Random Forest training. As training -parameters we used SIZE, DIST, WIDTH, LENGTH, CONC, and M3Long... - - -%\begin{figure}[!h] -%\centering -%\subfigure[The Hadronness distribution.]{ -%\includegraphics[scale= .3]{hadronness}} -%\subfigure[SIZE $> 300$ Phe]{ -%\includegraphics[scale= .3]{size300}} -%\subfigure[SIZE $> 500$ Phe]{ -%\includegraphics[scale= .3]{size500}} -%\subfigure[SIZE $> 1000$ Phe]{ -%\includegraphics[scale= .3]{size1000}} -%\caption{Hadronness distribution and ALPHA plots for three different lower SIZE cuts. The -% Hadronness cut is made at 0.4.}\label{fig:prelresults} -%\end{figure} - -The results of the preliminary analysis can be summarized as follows. After the gamma/hadron separation, the ALPHA distributions of the ON data show excess signals of 121 and 32 events, with significances of 5.2 and 3.7 $\sigma$, for SIZE values above 300 p.e. and 800 p.e., respectively. If the SIZE cut at 300 p.e. corresponds to an energy threshold of 1.9 TeV and if the effective collection area is assumed to be 1.e5 m$^2$ the observed excess is by a factor of 10 higher than that expected on the basis of the HESS flux. - -Studies are going on concerning appropriate OFF data, the false-source plot and better estimates of the energy threshold and the effective collection area. +parameters we used SIZE, DIST, WIDTH, LENGTH, CONC, and M3Long. The training +was done for SIZE $>100$ p.e.. + +\begin{figure}[!h] +\centering +\subfigure[SIZE $> 300$ p.e.]{ +\includegraphics[scale= .3]{alpha_tmpl_s100_h006}} +\subfigure[SIZE $> 500$ p.e.]{ +\includegraphics[scale= .3]{alpha_tmpl_s800_h02}} +\caption{Preliminary ALPHA distributions for lower SIZE cuts of 100 and 800 p.e..}\label{fig:prelresults} +\end{figure} + +The results of the preliminary analysis can be summarized as follows. After +the gamma/hadron separation, the ALPHA distributions of the ON data show +excess signals of 60 and 12 events, with significances of 3.5 and 2.5 +$\sigma$, for SIZE values above 100 p.e. and 800 p.e., respectively (figure \ref{fig:prelresults}). If the +SIZE cut at 100 p.e. corresponds to an energy threshold of 900 GeV and if the +effective collection area is assumed to be $10^5$ m$^2$ the observed excess is +by a factor of 5 higher than that expected on the basis of the HESS flux. + +Studies are going on concerning appropriate OFF data, the false-source plot +and better estimates of the energy threshold and the effective collection area. @@ -392,6 +397,6 @@ & $T_{5\sigma}$ \\ & & above $E_{\mathrm{th}}$ & &\\ -$[^{\circ}]$ & $[{\rm GeV}]$ & $[{\rm cm}^2\;{\rm s}]^{-1}$ - & $[{\rm cm}^2\;{\rm s}]^{-1}$ +$[^{\circ}]$ & $[{\rm GeV}]$ & $[{\rm cm}^{-2}\;{\rm s}^{-1}]$ + & $[{\rm cm}^{-2}\;{\rm s}^{-1}]$ & $ [{\rm hours}]$ \\ \hline @@ -400,5 +405,5 @@ \hline \end{tabular} -\caption{Energy threshold $E_{\mathrm{th}}$ and sensitivity for MAGIC for 2 zenith angles ZA. The 4th and 5th column contain the expected integrated flux above $E_{\mathrm{th}}$ and the time needed for observing a 5$\sigma$ excess, respectively.}\label{table:MAGIC_sensitivity}} +\caption{Energy threshold $E_{\mathrm{th}}$ and sensitivity for MAGIC for two zenith angles ZA. The 4th and 5th column contain the expected integrated flux above $E_{\mathrm{th}}$ and the time needed for observing a 5$\sigma$ excess, respectively.}\label{table:MAGIC_sensitivity}} \end{table} @@ -476,5 +481,5 @@ \includegraphics[totalheight=16cm]{GCregion14.eps} \end{center} -\caption[Star field around the GC.]{Star field around the GC. Stars up to a magnitude of 14 are plotted. The 2 big circles correspond to distances of 1$^{\circ}$ and 1.75$^{\circ}$ from the GC, respectively. The x axis is pointing into the direction of decreasing RA, the y axis into the direction of increasing declination. The grid spacing in the declination is 20 arc minutes. The Galactic Plane is given by the dotted line. +\caption[Star field around the GC.]{Star field around the GC. Stars up to a magnitude of 14 are plotted. The 2 big circles correspond to distances of 1$^{\circ}$ and 1.75$^{\circ}$ from the GC, respectively. The $x$ axis is pointing into the direction of decreasing RA, the $y$ axis into the direction of increasing declination. The grid spacing in the declination is 20 arc minutes. The Galactic Plane is given by the dotted line. } \label{fig:GC_starfield} \end{figure} @@ -484,5 +489,5 @@ \includegraphics[totalheight=16cm]{GCregion14largeW.eps} \end{center} -\caption[Star field around the GC.]{Star field around the GC. Stars up to a magnitude of 14 are plotted. The 2 big circles correspond to distances of 1$^{\circ}$ and 1.75$^{\circ}$ from the GC, respectively. The wobble positions WGC1 and WGC2 are given by the full circles. The x axis is pointing into the direction of decreasing RA, the y axis into the direction of increasing declination. The grid spacing in the declination is 1 degree. +\caption[Star field around the GC.]{Star field around the GC. Stars up to a magnitude of 14 are plotted. The 2 big circles correspond to distances of 1$^{\circ}$ and 1.75$^{\circ}$ from the GC, respectively. The wobble positions WGC1 and WGC2 are given by the full circles. The $x$ axis is pointing into the direction of decreasing RA, the $y$ axis into the direction of increasing declination. The grid spacing in the declination is 1 degree. } \label{fig:GC_starfield_largeW} \end{figure} @@ -492,5 +497,5 @@ \includegraphics[totalheight=16cm]{GCregionOFF1.eps} \end{center} -\caption[Star field around the GC.]{Star field around the GC. Stars up to a magnitude of 14 are plotted. The ON region is indicated by the bigger circle in the center. A possible OFF region is shown by the bigger circle in the left upper part of the figure. The x axis is pointing into the direction of decreasing RA, the y axis into the direction of increasing declination. The grid spacing in the declination is 1 degree. +\caption[Star field around the GC.]{Star field around the GC. Stars up to a magnitude of 14 are plotted. The ON region is indicated by the bigger circle in the center. A possible OFF region is shown by the bigger circle in the left upper part of the figure. The $x$ axis is pointing into the direction of decreasing RA, the $y$ axis into the direction of increasing declination. The grid spacing in the declination is 1 degree. } \label{fig:GC_starfield_OFF1} \end{figure} @@ -518,5 +523,5 @@ -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. +To increase statistics at high energies we propose to take additional data during moonshine. Also in this case, the maximum ZA of 60 deg should not be exceeded. 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