Changeset 6726


Ignore:
Timestamp:
03/03/05 18:11:47 (20 years ago)
Author:
hbartko
Message:
Changelog
Location:
trunk/MagicSoft/GC-Proposal
Files:
6 edited

Legend:

Unmodified
Added
Removed

  • trunk/MagicSoft/GC-Proposal/Changelog

    r6716 r6726  
     1
     22005/03/03 Hendrik
     3* text about Dark Matter, new references
    14
    252005/03/03  Sebastian

  • trunk/MagicSoft/GC-Proposal/GC.blg

    r6672 r6726  
    33The style file: GC.bst
    44Database file #1: bibbib.bib
     5Warning--string name "d10" is undefined
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     7Warning--string name "d69" is undefined
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    59You can't pop an empty literal stack for entry Aharonian2005
    610while executing---line 1972 of file GC.bst
    … …  
    2226You can't pop an empty literal stack for entry GC_hess
    2327while executing---line 1972 of file GC.bst
     28You can't pop an empty literal stack for entry Pohl1997
     29while executing---line 1972 of file GC.bst
    2430You can't pop an empty literal stack for entry GC_black_hole
     31while executing---line 1972 of file GC.bst
     32You can't pop an empty literal stack for entry jung96
     33while executing---line 1972 of file GC.bst
     34You can't pop an empty literal stack for entry Klypin2002
     35while executing---line 1972 of file GC.bst
     36You can't pop an empty literal stack for entry Ellis1984
    2537while executing---line 1972 of file GC.bst
    2638You can't pop an empty literal stack for entry Kaluza_Klein
    2739while executing---line 1972 of file GC.bst
     40You can't pop an empty literal stack for entry NFW1997
     41while executing---line 1972 of file GC.bst
     42You can't pop an empty literal stack for entry Stoehr2002
     43while executing---line 1972 of file GC.bst
     44You can't pop an empty literal stack for entry Hayashi2004
     45while executing---line 1972 of file GC.bst
     46You can't pop an empty literal stack for entry Moore1998
     47while executing---line 1972 of file GC.bst
    2848You can't pop an empty literal stack for entry Prada2004
    2949while executing---line 1972 of file GC.bst
    30 You've used 13 entries,
     50You can't pop an empty literal stack for entry Fornego2004
     51while executing---line 1972 of file GC.bst
     52You can't pop an empty literal stack for entry Evans2004
     53while executing---line 1972 of file GC.bst
     54You can't pop an empty literal stack for entry Hooper2004
     55while executing---line 1972 of file GC.bst
     56You've used 25 entries,
    3157            1987 wiz_defined-function locations,
    32             671 strings with 6871 characters,
    33 and the built_in function-call counts, 2681 in all, are:
    34 = -- 186
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     58            747 strings with 8805 characters,
     59and the built_in function-call counts, 5316 in all, are:
     60= -- 366
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    3662< -- 0
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    41 add.period$ -- 13
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     66:= -- 705
     67add.period$ -- 25
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    4369change.case$ -- 0
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    45 cite$ -- 14
    46 duplicate$ -- 147
    47 empty$ -- 274
    48 format.name$ -- 36
    49 if$ -- 615
     71cite$ -- 26
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     74format.name$ -- 76
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    5076int.to.chr$ -- 0
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    54 num.names$ -- 12
    55 pop$ -- 57
     77int.to.str$ -- 25
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     80num.names$ -- 24
     81pop$ -- 104
    5682preamble$ -- 1
    5783purify$ -- 0
    5884quote$ -- 0
    59 skip$ -- 109
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    6086stack$ -- 0
    61 substring$ -- 124
    62 swap$ -- 47
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     88swap$ -- 93
    6389text.length$ -- 0
    6490text.prefix$ -- 0
    … …  
    6692type$ -- 0
    6793warning$ -- 1
    68 while$ -- 22
    69 width$ -- 15
    70 write$ -- 117
    71 (There were 12 error messages)
     94while$ -- 45
     95width$ -- 27
     96write$ -- 226
     97(There were 23 error messages)

  • trunk/MagicSoft/GC-Proposal/GC.log

    r6675 r6726  
    1 This is e-TeX, Version 3.14159-2.1 (Web2C 7.3.1) (format=latex 1999.10.11)  24 FEB 2005 19:06
     1This is e-TeX, Version 3.14159-2.1 (Web2C 7.3.1) (format=latex 1999.10.11)  3 MAR 2005 18:09
    22**GC.tex
    33(GC.tex
    … …  
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     224Package: array 1998/05/13 v2.3m Tabular extension package (FMi)
     225\col@sep=\dimen137
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     239(/mnt/local/i386_linux2/tex/texmf/tex/latex/tools/hhline.sty
     240Package: hhline 1994/05/23 v2.03 Table rule package (DPC)
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    221243Package: url 1999/03/02  ver 1.4  Verb mode for urls, email addresses, and file
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    224 
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     247Package: subfigure 1995/03/06 v2.0 subfigure package
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     250\c@subfigure=\count112
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     254) (GC.aux)
    228255\openout1 = `GC.aux'.
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    243270 <magiclogo.eps>
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    325359Here is how much of TeX's memory you used:
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     368Output written on GC.dvi (10 pages, 29836 bytes).

  • trunk/MagicSoft/GC-Proposal/GC.tex

    r6715 r6726  
    4545
    4646Various possibilities for the acceleration of the very high energy gamma rays
    47 are discussed in the literature (like...). Although the observed VHE gamma
     47are discussed in the literature, like accretion flow onto the central black hole, supernova shocks in Sgr A East, proton acceleration near the event horizon of the black hole, or WIMP dark matter annihilation. Although the observed VHE gamma
    4848radiation from the GC is most probably not due to SUSY-neutralino particle
    4949dark matter (DM) annihilation, other models like Kaluza-Klein dark matter are not ruled out. Moreover, assuming a universal DM distribution profile, the GC is expected to yield the largest DM flux due to its relative vicinity.
    … …  
    106106
    107107
    108 In fact, EGRET has detected a strong source in direction of the GC, 3 EG J1745-2852 \cite{GC_egret}, which has a broken power law spectrum extending up to at least 10 GeV, with the index 1.3 below the bread at a few GeV. If in the GC, the gamma ray luminosity of this source is very large $~2 \cdot 10^{37} \mathrm{erg}/\mathrm{s}$, which is equivalent to about 10 Crab pulsars. Up to now, the GC has been observed at energies above 200 GeV by Veritas, Cangaroo and HESS, \cite{GC_whipple,GC_cangaroo,GC_hess}. Figure \ref{fig:GC_gamma_flux} shows the reconstructed spectra by the other IACTs while figure \ref{fig:GC_source_location} shows the different reconstructed positions of the GC source.
     108In fact, EGRET has detected a strong source in direction of the GC, 3 EG J1745-2852 \cite{GC_egret}, which has a broken power law spectrum extending up to at least 10 GeV, with the index 1.3 below the bread at a few GeV. If in the GC, the gamma ray luminosity of this source is very large $~2 \cdot 10^{37} \mathrm{erg}/\mathrm{s}$, which is equivalent to about 10 Crab pulsars. Up to now, the GC has been observed at energies above 200 GeV by Veritas, Cangaroo and HESS, \cite{GC_whipple,GC_cangaroo,GC_hess}. Figure \ref{fig:GC_gamma_flux} shows the reconstructed spectra by the other IACTs while figure \ref{fig:GC_source_location} shows the different reconstructed positions of the GC source. Recently a second TeV gamma source only about 1 degree away from the Galactic Center has been discovered \cite{SNR_G09+01}. Its integral flux above 200 GeV represents about 2\% of the gamma flux from the Crab nebula.
    109109
    110110\begin{figure}[h!]
    … …  
    138138 \hline
    139139 Investigator & Institution& E-mail & Assigned task\\ \hline
    140    Hendrik Bartko      & MPI Munich    & hbartko@mppmu.mpg.de & data analysis, spectra
     140   Hendrik Bartko      & MPI Munich    & hbartko@mppmu.mpg.de & data analysis, spectra, wobble mode
    141141\\ Adrian Biland       & ETH Zurich    & biland@particle.phys.ethz.ch & OFF pointing, Moon observations
    142142\\ Sebastian Commichau & ETH Zurich    & commichau@particle.phys.ethz.ch &
    … …  
    154154
    155155
    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{}, (cite also Aharonia, ...) 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.
     156High 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 supermassive black hole \cite{}.
     157
     158
    157159In order to shed new light on the high energy phenomena in the GC region, and constrain the models mentioned above, new observations with high sensitivity, good spectra reconstruction and angular resolution are necessary.
    158160
    … …  
    177179
    178180\subsection{Dark Matter}
    179  
    180 something about DM. Kaluza-Klein \cite{Kaluza_Klein}.
    181 
    182 adiabatic compression: \cite{Prada2004}
    183 
    184 
    185 Motivation for Dark Matter searches (cosmology).
    186 
    187 Neutralino as DM particle. Production of gamma radiation from neutralino annihilation.
    188  
     181
     182
     183The presence of a Dark Matter halo of the Galaxy is well established by stellar dynamics \cite{Klypin2002}. At present, the nature of Dark Matter is unknown, but a number of viable candidates have been advocated within different theoretical frameworks mainly motivated by particle physics (for a review see \cite{jung96}) including the widely studied models of supersymmetric (SUSY) Dark Matter \cite{Ellis1984}. Also models involving extra dimensions are discussed like Kaluza-Klein Dark Matter \cite{Kaluza_Klein}.
     184
     185The supersymmetric particle dark matter candidates might self-annihilate into boson or fermion pairs yielding very high energy gammas in subsequent decays and from hadronisation. The gamma flux above an energy threshold per solid angle is given by:
     186
     187\begin{equation*}
     188\frac{\text{d} N_{\gamma}(E_{\gamma}>E_{\mathrm{thresh}})}{\text{d}t\  \text{d}A\  \text{d}\Omega }= N_{\gamma}(E_{\gamma}>E_{\mathrm{thresh}}) \cdot \frac{1}{2} \cdot \frac{\langle \sigma v \rangle}{4 \pi m_{\chi}^2} \cdot  \int_{\text{los}}\rho_{\chi}^2(\vec{r}(s,\Omega)) \text{d}s \ ,
     189\end{equation*}
     190
     191
     192where ... is ... . The flux prediction depends on the choise 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.
     193
     194Numerical 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.
     195
     196Using 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
     198Figure \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 expection.
     199
    189200
    190201\begin{figure}[h!]
    … …  
    192203\includegraphics[totalheight=6cm]{Dark_exclusion_limits.eps}
    193204\end{center}
    194 \caption[DM exclusion limits.]{Exclusion limits for different possible sources of dark matter annihilation radiation. The galactic center is expected to give the largest flux from all sources. Due to the possible flux con} \label{fig:GC_sources}
     205\caption[DM exclusion limits.]{Exclusion limits for different possible sources of dark matter annihilation radiation. The galactic center is expected to give the largest flux from all sources. Due to the possible flux con} \label{fig:exclusion_lmits}
    195206\end{figure}
     207
     208
     209Detailed 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 favoured 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.
     210
     211
    196212
    197213\newpage

  • trunk/MagicSoft/GC-Proposal/GC.toc

    r6675 r6726  
    11\select@language {english}
    22\contentsline {section}{\numberline {1}Introduction}{3}
    3 \contentsline {section}{\numberline {2}Investigators and Affiliations}{5}
     3\contentsline {section}{\numberline {2}Investigators and Affiliations}{4}
    44\contentsline {section}{\numberline {3}Scientific Case}{5}
    55\contentsline {subsection}{\numberline {3.1}Leptonic Models}{5}
    66\contentsline {subsection}{\numberline {3.2}Hadronic Models}{5}
    77\contentsline {subsection}{\numberline {3.3}Dark Matter}{5}
    8 \contentsline {section}{\numberline {4}Preparatory Work}{5}
    9 \contentsline {section}{\numberline {5}Feasibility}{6}
    10 \contentsline {section}{\numberline {6}Observational Constraints}{7}
    11 \contentsline {section}{\numberline {7}Requested Observation Time}{7}
    12 \contentsline {section}{\numberline {8}Outlook and Conclusions}{8}
    13 \contentsline {section}{\numberline {A}Acknowledgements}{8}
     8\contentsline {section}{\numberline {4}Preparatory Work}{7}
     9\contentsline {section}{\numberline {5}Feasibility}{7}
     10\contentsline {section}{\numberline {6}Observational Constraints}{8}
     11\contentsline {section}{\numberline {7}Requested Observation Time}{8}
     12\contentsline {section}{\numberline {8}Outlook and Conclusions}{9}
     13\contentsline {section}{\numberline {A}Acknowledgements}{9}

  • trunk/MagicSoft/GC-Proposal/bibbib.bib

    r6672 r6726  
     1@Article{Ellis1984,
     2     author    = "Ellis, John R. and Hagelin, J. S. and Nanopoulos, D. V. and
     3                  Olive, Keith A. and Srednicki, M.",
     4     title     = "Supersymmetric relics from the big bang",
     5     journal   = "Nucl. Phys.",
     6     volume    = "B238",
     7     year      = "1984",
     8     pages     = "453-476",
     9     SLACcitation  = "%%CITATION = NUPHA,B238,453;%%"
     10}
     11
     12@ARTICLE{Klypin2002,
     13   author = {{Klypin}, A. and {Zhao}, H. and {Somerville}, R.~S.},
     14    title = "{{$\Lambda$}CDM-based Models for the Milky Way and M31. I. Dynamical Models}",
     15  journal = "ApJ",
     16     year = 2002,
     17    month = jul,
     18   volume = 573,
     19    pages = {597-613},
     20   adsurl = {http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2002ApJ...573..597K&db_key=AST},
     21  adsnote = {Provided by the NASA Astrophysics Data System}
     22}
     23
     24@ARTICLE{Pohl1997,
     25   author = {{Pohl}, M.},
     26    title = "{The galactic center arc as source of high energy {$\gamma$}-rays.}",
     27  journal = "A\&A",
     28     year = 1997,
     29    month = jan,
     30   volume = 317,
     31    pages = {441-447},
     32   adsurl = {http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997A%26A...317..441P&db_key=AST},
     33  adsnote = {Provided by the NASA Astrophysics Data System}
     34}
     35
     36@Article{SNR_G09+01,
     37     author    = "Aharonian, F. and others",
     38 collaboration = "The H.E.S.S.",
     39     title     = "Very high energy gamma rays from the composite SNR
     40                  G0.9+0.1",
     41     year      = "2005",
     42     eprint    = "astro-ph/0501265",
     43     SLACcitation  = "%%CITATION = ASTRO-PH 0501265;%%"
     44}
     45
     46
    147@manual{MC-Camera,
    248     author    = "Blanch,O. and Moralejo,A.",
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