Changeset 6852
- Timestamp:
- 03/18/05 13:56:50 (20 years ago)
- Location:
- trunk/MagicSoft/GC-Proposal
- Files:
-
- 2 added
- 2 edited
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trunk/MagicSoft/GC-Proposal/Changelog
r6835 r6852 1 2005/03/18 Sebastian 2 * GC.tex 3 Did some small corrections. Results of the preliminary analysis changed 4 and added two ALPHA plots for two different lower cuts in SIZE. 5 * added and committed the files 6 alpha_tmpl_s100_h006.eps and alpha_tmpl_s800_h02.eps 7 to the repository 8 1 9 2005/03/16 Hendrik 2 10 * GC.tex: -
trunk/MagicSoft/GC-Proposal/GC.tex
r6851 r6852 62 62 At La Palma, the GC culminates at about 58 deg zenith angle (ZA). It can be 63 63 observed with MAGIC at up to 60 deg ZA, between 64 April and late August, yielding a total of 150 hours per year. The expected integral flux above 700 GeV derived from 64 April and late August, yielding a total of 150 hours without moon per year. 65 The expected integral flux above 700 GeV derived from 65 66 the HESS data is $(3.2 \pm 1.0)\cdot 10^{-12}\mathrm{cm}^{-2}\mathrm{s}^{-1}$. 66 67 Comparing this to the expected MAGIC sensitivity from MC simulations, this … … 69 70 The observations have to be conducted as early as possible in order to 70 71 participate in the ongoing discussion about gamma radiation from the GC. 71 The main motivations for the observation of the GC are 72 The main motivations for the observation of the GC are: 72 73 73 74 \begin{itemize} … … 84 85 In order to collect a data sample comparable in size to those of the other 85 86 experiments and to be able to measure the energy spectrum, 40 hours of 86 observation time are requested. Th e40 hours will be split into 20 hours ON87 observation time are requested. This 40 hours will be split into 20 hours ON 87 88 and 20 hours dedicated OFF data or they will be devoted to observations in 88 89 the wobble mode. In addition, 60 hours of observation during moonshine are … … 166 167 \end{figure} 167 168 168 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. 169 The discrepancies between the measured flux spectra could indicate 170 inter-calibration problems between the IACTs. But it could also indicate an 171 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. 169 172 170 173 … … 185 188 Investigator & Institution& E-mail & Assigned task\\ \hline 186 189 Hendrik Bartko & MPI Munich & hbartko@mppmu.mpg.de & data analysis, spectra, wobble mode 187 \\ Adrian Biland & ETH Zurich & biland@particle.phys.ethz.ch & OFF pointing, Moon observations188 \\ Erica Bisesi 190 \\ Adrian Biland & ETH Zurich & biland@particle.phys.ethz.ch & MC generation, Moon observations 191 \\ Erica Bisesi & Univ. Udine & bisesi@fisica.uniud.it & dark matter halo modelling, clumpness 189 192 \\ Sebastian Commichau & ETH Zurich & commichau@particle.phys.ethz.ch & 190 data analysis, MC generation, spectra193 data analysis, spectra, geomagnetic effects 191 194 \\ Pepe Flix & IFAE Barcelona& jflix@ifae.es & data analysis, disp, spectra, dark matter 192 195 \\ Sabrina Stark & ETH Zurich & lstark@particle.phys.ethz.ch & data analysis, spectra … … 227 230 \begin{itemize} 228 231 \item{source location, source extension} 229 \item{ time variability of the gamma flux}230 \item{ energy spectrum.}232 \item{energy spectrum} 233 \item{time variability of the gamma flux.} 231 234 \end{itemize} 232 235 … … 258 261 \subsubsection{Hadronic Models} 259 262 260 Onescenario 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}.263 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}. 261 264 262 265 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. … … 318 321 \hline 319 322 Date & Time & Az $[^\circ]$ & ZA $[^\circ]$\\ \hline 320 09/08/2004 & 21:00 - 22: 00& 198.3 - 214.7 & 60.3 - 67.8321 \\ 09/09/2004 & 21:17 - 22:12 & 203.4 - 214.7 & 62. 2- 67.7323 09/08/2004 & 21:00 - 22:16 & 198.3 - 214.7 & 60.3 - 67.8 324 \\ 09/09/2004 & 21:17 - 22:12 & 203.4 - 214.7 & 62.0 - 67.7 322 325 \\ 09/10/2004 & 21:06 - 22:03 & 202.2 - 213.7 & 61.6 - 67.1 323 326 \\ … … 334 337 335 338 The MC sample was divided into a training 336 and a test sample . Since no dedicated OFF data were available, we used a339 and a test sample and its slope was normalized to $-2.21$. Since no dedicated OFF data were available, we used a 337 340 subsample of Sgr A$^*$ ON data to represent the hadronic background in the Random Forest training. As training 338 parameters we used SIZE, DIST, WIDTH, LENGTH, CONC, and M3Long... 339 340 341 %\begin{figure}[!h] 342 %\centering 343 %\subfigure[The Hadronness distribution.]{ 344 %\includegraphics[scale= .3]{hadronness}} 345 %\subfigure[SIZE $> 300$ Phe]{ 346 %\includegraphics[scale= .3]{size300}} 347 %\subfigure[SIZE $> 500$ Phe]{ 348 %\includegraphics[scale= .3]{size500}} 349 %\subfigure[SIZE $> 1000$ Phe]{ 350 %\includegraphics[scale= .3]{size1000}} 351 %\caption{Hadronness distribution and ALPHA plots for three different lower SIZE cuts. The 352 % Hadronness cut is made at 0.4.}\label{fig:prelresults} 353 %\end{figure} 354 355 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. 356 357 Studies are going on concerning appropriate OFF data, the false-source plot and better estimates of the energy threshold and the effective collection area. 341 parameters we used SIZE, DIST, WIDTH, LENGTH, CONC, and M3Long. The training 342 was done for SIZE $>100$ p.e.. 343 344 \begin{figure}[!h] 345 \centering 346 \subfigure[SIZE $> 300$ p.e.]{ 347 \includegraphics[scale= .3]{alpha_tmpl_s100_h006}} 348 \subfigure[SIZE $> 500$ p.e.]{ 349 \includegraphics[scale= .3]{alpha_tmpl_s800_h02}} 350 \caption{Preliminary ALPHA distributions for lower SIZE cuts of 100 and 800 p.e..}\label{fig:prelresults} 351 \end{figure} 352 353 The results of the preliminary analysis can be summarized as follows. After 354 the gamma/hadron separation, the ALPHA distributions of the ON data show 355 excess signals of 60 and 12 events, with significances of 3.5 and 2.5 356 $\sigma$, for SIZE values above 100 p.e. and 800 p.e., respectively (figure \ref{fig:prelresults}). If the 357 SIZE cut at 100 p.e. corresponds to an energy threshold of 900 GeV and if the 358 effective collection area is assumed to be $10^5$ m$^2$ the observed excess is 359 by a factor of 5 higher than that expected on the basis of the HESS flux. 360 361 Studies are going on concerning appropriate OFF data, the false-source plot 362 and better estimates of the energy threshold and the effective collection area. 358 363 359 364 … … 392 397 & $T_{5\sigma}$ \\ 393 398 & & above $E_{\mathrm{th}}$ & &\\ 394 $[^{\circ}]$ & $[{\rm GeV}]$ & $[{\rm cm}^ 2\;{\rm s}]^{-1}$395 & $[{\rm cm}^ 2\;{\rm s}]^{-1}$399 $[^{\circ}]$ & $[{\rm GeV}]$ & $[{\rm cm}^{-2}\;{\rm s}^{-1}]$ 400 & $[{\rm cm}^{-2}\;{\rm s}^{-1}]$ 396 401 & $ [{\rm hours}]$ \\ 397 402 \hline … … 400 405 \hline 401 406 \end{tabular} 402 \caption{Energy threshold $E_{\mathrm{th}}$ and sensitivity for MAGIC for 2zenith 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}}407 \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}} 403 408 \end{table} 404 409 … … 476 481 \includegraphics[totalheight=16cm]{GCregion14.eps} 477 482 \end{center} 478 \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 yaxis 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.483 \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. 479 484 } \label{fig:GC_starfield} 480 485 \end{figure} … … 484 489 \includegraphics[totalheight=16cm]{GCregion14largeW.eps} 485 490 \end{center} 486 \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 yaxis into the direction of increasing declination. The grid spacing in the declination is 1 degree.491 \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. 487 492 } \label{fig:GC_starfield_largeW} 488 493 \end{figure} … … 492 497 \includegraphics[totalheight=16cm]{GCregionOFF1.eps} 493 498 \end{center} 494 \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 yaxis into the direction of increasing declination. The grid spacing in the declination is 1 degree.499 \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. 495 500 } \label{fig:GC_starfield_OFF1} 496 501 \end{figure} … … 518 523 519 524 520 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.525 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. 521 526 522 527 In order to take part in exploring the exciting physics of the GC
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