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Timestamp:
02/04/05 12:30:47 (20 years ago)
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garcz
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trunk/MagicSoft/GRB-Proposal
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  • trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex

    r6237 r6251  
    7979As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches
    8080with the one of \ma,
    81 we cannot predict the alert frequency now to better than 100\% uncertainty. 
     81we cannot predict the alert frequency now to better than 100\% uncertainty.
    8282This leads to an expected observation time
    83 of 5$\pm$5 hours per month. This number includes observation during moon-time.
     83of 5$\pm$5 hours per month. This number includes observation during the moon-time.
    8484We give a detailed description of the observation procedures in La Palma and
    8585propose to spend one dedicated night to test the automatic alert procedure
  • trunk/MagicSoft/GRB-Proposal/Introduction.tex

    r6239 r6251  
    1111
    1212Very high energy (VHE) GRB observations have the potential to constrain the current GRB models
    13 on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}.
     13on both prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}.
    1414Models based on both internal and external shocks predict VHE gamma-ray fluences comparable to,
    1515or in certain situations stronger than, the keV-MeV radiation,
    16 with durations ranging from shorter than the keV-MeV burst to extended TeV 
     16with durations ranging from shorter than the keV-MeV burst to extended TeV
    1717afterglows~\cite{DERMER, PILLA, ZHANG1, RAZZAQUE}.
    1818
     
    2323as well as photon-pion production~\cite{WAXMAN,BOETTCHER} and inverse-Compton scattering
    2424in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2,BELOBORODOV}.
    25 Long-term HE $\gamma$-emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}.
     25Long-term high energy (HE) $\gamma$-emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}.
    2626This model predicts GeV inverse Compton emission even one day after the burst.
    2727Even considering pure electron-synchrotron radiation, measurable GeV-emission for a significant
     
    4040each indicating some excess over background but without stringent evidence.
    4141The only significant detection was performed by \eg which was able to observe seven GRBs
    42 emitting high energy (HE)
     42emitting HE
    4343photons in the 100\,MeV to 18\,GeV range~\cite{EGRET, DINGUS1}. The data shows no evidence of a HE cut-off in the GRB spectrum~\cite{DINGUS2}. Recent results indicate that the spectrum of some GRBs contains a very hard, luminous, long-duration component~\cite{GONZALES}.
    4444There have been results suggesting gamma rays beyond the GeV range from the TIBET air shower array
     
    5757and assuming an energy threshold of 15~GeV, a 5\,$\sigma$-signal rate of $0.5-2$ per year
    5858was obtained for an assumed observation delay between 15 and 60\,sec. and a \ba trigger rate
    59 ($\sim$\,360/year). As the \sw alert rate is about a factor~2 lower including even fainter bursts than
    60 those observed by \ma, this number will still have to be lowered.
     59($\sim$\,360/year). As the \sw alert rate is about factor~2 lower, including even fainter bursts than
     60those observed by \ma, this number still have to be lowered.
    6161
    62 Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from a 
     62Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from a
    6363few tens of GRBs per year should be observable over the whole sky above our energy threshold.
    64 The model of~\cite{ASAF2} predict delayed GeV-emission that should be significantly detectable by \ma 
     64The model of~\cite{ASAF2} predict delayed GeV-emission that should be significantly detectable by \ma
    6565in 100\,sec.
    6666
    6767\subsection{Observation of XRFs}
    6868
    69 While the major energy from the prompt GRBs is emitted in $\gamma$-rays with a peak energy of 200\,keV, 
     69While the major energy from the prompt GRBs is emitted in $\gamma$-rays with a peak energy of 200\,keV,
    7070X-ray flashes (XRFs) are characterized
    71 by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties, a connection 
    72 between XRFs and GRBs is suggested. 
     71by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties, a connection
     72between XRFs and GRBs is suggested.
    7373The most popular theories ~\cite{DADO} suggest that XRFs are produced from GRBs observed ''off-axis''.
    7474Alternatively, an increase of the baryon load within the fireball itself ~\cite{HUANG} or low efficiency shocks ~\cite{BARRAUD} could produce XRFs.
    7575If there is a connection between XRFs and GRBs, they should originate at rather low redshifts (z $<$ 0.6). Because If XRFs lie at large distances, their energies would not fit the observed correlation between GRB peak energy and isotropic energy release~\cite{LEVAN}. \\
    7676
    77 Gamma-ray satellites react in the same way to XRFs and GRBs. 
     77Gamma-ray satellites react in the same way to XRFs and GRBs.
    7878In case of a detection the coordinates are distributed
    7979to other observatories (see section 2.1). Only from later analysis the difference can be established.
     
    8585\subsection{Observation of SGRs}
    8686
    87 Soft Gamma Repeaters (SGRs) are believed to be extremely rare strong magnetic neutron stars that 
    88 periodically emit $\gamma$-rays. Only four identified SGRs were discovered in the last 20 years: 
    89 SGR0526-66, SGR1806-20, SGR1900+14, SGR1627-41. 
    90 GRBs and SGRs can be explained within one same gamma jet model where the jet is observed at different 
     87Soft Gamma Repeaters (SGRs) are believed to be extremely rare strong magnetic neutron stars that
     88periodically emit $\gamma$-rays. Only four identified SGRs were discovered in the last 20 years:
     89SGR0526-66, SGR1806-20, SGR1900+14, SGR1627-41.
     90GRBs and SGRs can be explained within one same gamma jet model where the jet is observed at different
    9191beam-angles and at different ages~\cite{FARGION}.\\
    9292
    93 The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30. January 2005. 
    94 The fluence was about $10^{-5}$\,erg/cm$^2$ in the range between 15 and 350\,keV. 
    95 This event was five orders of magnitude smaller than the giant flare from this source on the 
    96 December 27$^{th}$, 2004~\cite{GCN3002}. MAGIC have a enough sensitivity for observing the event which have a fluence more than 2.5 $\times$ 10 $^{-2}$ erg/cm$^{2} \cdot sec$ at 100keV, when power law index of -2.0 and 100 sec. observation time are assumpted. Therefore if a giant flare from SGR occurs as SGR1806-20, MAGIC would be able to detect the $\gamma$-ray emission from these source.
     93The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30. January 2005.
     94The fluence was about $10^{-5}$\,erg/cm$^2$ in the range between 15 and 350\,keV.
     95This event was five orders of magnitude smaller than the giant flare from this source on the
     96December 27$^{th}$, 2004~\cite{GCN3002}. MAGIC have a enough sensitivity for observing the event which have a fluence more than 2.5 $\times$ 10 $^{-2}$ erg/cm$^{2} \cdot$\,sec at 100\,keV, when power law index of -2.0 and 100 sec. observation time are assumpted. Therefore if a giant flare from SGR occurs as SGR1806-20, MAGIC would be able to detect the $\gamma$-ray emission from these source.
    9797
    9898
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