Index: trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6250) +++ trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6251) @@ -79,7 +79,7 @@ As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches with the one of \ma, -we cannot predict the alert frequency now to better than 100\% uncertainty. +we cannot predict the alert frequency now to better than 100\% uncertainty. This leads to an expected observation time -of 5$\pm$5 hours per month. This number includes observation during moon-time. +of 5$\pm$5 hours per month. This number includes observation during the moon-time. We give a detailed description of the observation procedures in La Palma and propose to spend one dedicated night to test the automatic alert procedure Index: trunk/MagicSoft/GRB-Proposal/Introduction.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6250) +++ trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6251) @@ -11,8 +11,8 @@ Very high energy (VHE) GRB observations have the potential to constrain the current GRB models -on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}. +on both prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}. Models based on both internal and external shocks predict VHE gamma-ray fluences comparable to, or in certain situations stronger than, the keV-MeV radiation, -with durations ranging from shorter than the keV-MeV burst to extended TeV +with durations ranging from shorter than the keV-MeV burst to extended TeV afterglows~\cite{DERMER, PILLA, ZHANG1, RAZZAQUE}. @@ -23,5 +23,5 @@ as well as photon-pion production~\cite{WAXMAN,BOETTCHER} and inverse-Compton scattering in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2,BELOBORODOV}. -Long-term HE $\gamma$-emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}. +Long-term high energy (HE) $\gamma$-emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}. This model predicts GeV inverse Compton emission even one day after the burst. Even considering pure electron-synchrotron radiation, measurable GeV-emission for a significant @@ -40,5 +40,5 @@ each indicating some excess over background but without stringent evidence. The only significant detection was performed by \eg which was able to observe seven GRBs -emitting high energy (HE) +emitting HE photons 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}. There have been results suggesting gamma rays beyond the GeV range from the TIBET air shower array @@ -57,23 +57,23 @@ and assuming an energy threshold of 15~GeV, a 5\,$\sigma$-signal rate of $0.5-2$ per year was obtained for an assumed observation delay between 15 and 60\,sec. and a \ba trigger rate -($\sim$\,360/year). As the \sw alert rate is about a factor~2 lower including even fainter bursts than -those observed by \ma, this number will still have to be lowered. +($\sim$\,360/year). As the \sw alert rate is about factor~2 lower, including even fainter bursts than +those observed by \ma, this number still have to be lowered. -Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from a +Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from a few tens of GRBs per year should be observable over the whole sky above our energy threshold. -The model of~\cite{ASAF2} predict delayed GeV-emission that should be significantly detectable by \ma +The model of~\cite{ASAF2} predict delayed GeV-emission that should be significantly detectable by \ma in 100\,sec. \subsection{Observation of XRFs} -While the major energy from the prompt GRBs is emitted in $\gamma$-rays with a peak energy of 200\,keV, +While the major energy from the prompt GRBs is emitted in $\gamma$-rays with a peak energy of 200\,keV, X-ray flashes (XRFs) are characterized -by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties, a connection -between XRFs and GRBs is suggested. +by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties, a connection +between XRFs and GRBs is suggested. The most popular theories ~\cite{DADO} suggest that XRFs are produced from GRBs observed ''off-axis''. Alternatively, an increase of the baryon load within the fireball itself ~\cite{HUANG} or low efficiency shocks ~\cite{BARRAUD} could produce XRFs. If 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}. \\ -Gamma-ray satellites react in the same way to XRFs and GRBs. +Gamma-ray satellites react in the same way to XRFs and GRBs. In case of a detection the coordinates are distributed to other observatories (see section 2.1). Only from later analysis the difference can be established. @@ -85,14 +85,14 @@ \subsection{Observation of SGRs} -Soft Gamma Repeaters (SGRs) are believed to be extremely rare strong magnetic neutron stars that -periodically emit $\gamma$-rays. Only four identified SGRs were discovered in the last 20 years: -SGR0526-66, SGR1806-20, SGR1900+14, SGR1627-41. -GRBs and SGRs can be explained within one same gamma jet model where the jet is observed at different +Soft Gamma Repeaters (SGRs) are believed to be extremely rare strong magnetic neutron stars that +periodically emit $\gamma$-rays. Only four identified SGRs were discovered in the last 20 years: +SGR0526-66, SGR1806-20, SGR1900+14, SGR1627-41. +GRBs and SGRs can be explained within one same gamma jet model where the jet is observed at different beam-angles and at different ages~\cite{FARGION}.\\ -The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30. January 2005. -The fluence was about $10^{-5}$\,erg/cm$^2$ in the range between 15 and 350\,keV. -This event was five orders of magnitude smaller than the giant flare from this source on the -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. +The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30. January 2005. +The fluence was about $10^{-5}$\,erg/cm$^2$ in the range between 15 and 350\,keV. +This event was five orders of magnitude smaller than the giant flare from this source on the +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 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.