Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6175) +++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6176) @@ -129,8 +129,8 @@ \bibitem{ZHANG2} HE Spectral Components in GRB Afterglows, Zhang B., Meszaros P., Astrophys. J. 559, 110, 2001. +\bibitem{BELOBORODOV} Optical and GeV-TeV Flashes from GRBs, Beloborodov A., ApJ, 618, L13, 2005. \bibitem{EGRET} Hurley K. et al., Nature, 372, 652 \bibitem{DINGUS} ESLAB29, Towards the Source of Gamma-Ray Bursts, Dingus, Ap\&SS, 231, 187, 1995. -\bibitem{GONZALES} A GRB with high-energy Spectral Component Inconsistent with the Synchrotron Shock Model, -Gonzales at al., Nature, 424, 749, 2003. +\bibitem{GONZALES} A GRB with high-energy Spectral Component Inconsistent with the Synchrotron Shock Model, Gonzales at al., Nature, 424, 749, 2003. \bibitem{AMENOMORI} Search for 10 TeV burst-like events coincident with the BATSE bursts using the TIBET Air Shower Array, Amenomori M., et al., A\&A, 311, 919, 1996. Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6175) +++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6176) @@ -12,18 +12,17 @@ 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,SALOMON}. -Models based on both internal and external shocks predicts VHE fluence comparable to, -or in certain situations stronger than, the keV-MeV radiation, +on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}. +Models based on both internal and external shocks predicts VHE fluence comparable to, +or in certain situations stronger than, the keV-MeV radiation, with duration ranging from shorter than the keV-MeV burst to extended TeV afterglows~\cite{DERMER, PILLA, ZHANG1}. \par -In many publications, the possibility that more energetic $\gamma$-rays come along with the -(low-energy) GRB, have been explored. Proton-synchrotron emission~\cite{TOTANI} have been suggested +In many publications, the possibility that more energetic $\gamma$-rays come along with the +(low-energy) GRB, have been explored. Proton-synchrotron emission~\cite{TOTANI} have been suggested as well as photon-pion production~\cite{WAXMAN,BAHCALL,BOETTCHER} and inverse-Compton scattering in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2}. -Long-term 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 predicts measurable GeV emission for a significant fraction of GRBs~\cite{ZHANG2}.\\ +Long-term 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 predicts measurable GeV emission for a significant fraction of GRBs~\cite{ZHANG2}. In order to be able to describe prompt synchrotron optical flashes (like observed in GRB990123 by ROTSE), GeV--TeV emission by inverse Compton scattering of the MeV photons should be produced at the same time~\cite{BELOBORODOV}.\\ GeV emission in GRBs is particularly sensitive to the Lorentz factor and the photon density of the emitting material - @@ -37,14 +36,8 @@ The only significant detection was performed by \eg which detected seven GRBs emitting high energy (HE) photons in the 100\,MeV to 18\,GeV range~\cite{EGRET}. The data shows no evidence of a HE cut-off -in the GRB spectrum~\cite{DINGUS}. Recent results indicate that the spectrum of some GRBs contains a very hard, -luminous, long-duration component~\cite{GONZALES}. +in the GRB spectrum~\cite{DINGUS}. 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 -in coincidence with BATSE bursts~\cite{AMENOMORI}, rapid follow-up observations by the -Whipple Air Cherenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA}, -Whipple~\cite{CONNAUGHTON2} and the Milagro prototype Milagrito~\cite{MILAGRO}. -The GRAND array has reported some excess of observed muons during seven BATSE bursts~\cite{GRAND}. -In this context, especially the publication from the TASC detector on \eg is important~\cite{GONZALES}, -finding a HE spectral component presumably due to ultra-relativistic acceleration -of hadrons and producing a spectral index of $-1$ with no cut-off up to the detector energy limit (200\,MeV).\\ +in coincidence with BATSE bursts~\cite{AMENOMORI}, rapid follow-up observations by the +Whipple Air Cherenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA}, Whipple~\cite{CONNAUGHTON2} and the Milagro prototype Milagrito~\cite{MILAGRO}. The GRAND array has reported some excess of observed muons during seven BATSE bursts~\cite{GRAND}. In this context, especially the publication from the TASC detector on \eg is important~\cite{GONZALES}, finding a HE spectral component presumably due to ultra-relativistic acceleration of hadrons and producing a spectral index of $-1$ with no cut-off up to the detector energy limit (200\,MeV).\\ Concerning estimates about the \ma observability of GRBs, a very detailed study of GRB spectra obtained from the @@ -55,16 +48,15 @@ Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from few tens of GRBs per year -should be observable above our energy threshold. The model of~\cite{ASAF2} predict delayed GeV emission that -should be significantly detectable by MAGIC in 100\,seconds. +should be observable above our energy threshold. The model of~\cite{ASAF2} predict delayed GeV emission that should be significantly detectable by MAGIC in 100\,seconds. \subsection{Observation of XRFs} While the major energy from the prompt GRBs is emitted in $\gamma$-rays ($E_p \sim$ 200~keV), 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 +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 say that XRFs are produced from GRBs observed ''off-axis''. -Alternatively, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. +Alternatively, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. If there is a connection between the XRFs and GRBs, they should originate at rather low redshifts (z $<$ 0.6).\\ -Gamma-ray satellites react in the same way to XRFs and GRBs. In case of a detection the coordinates are distributed +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. @@ -73,20 +65,7 @@ In this case we include also the observation of XRFs by MAGIC in our proposal. +\subsection{Observation of SGRs} +Soft Gamma Repeaters (SGRs) are 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 with an unique processing gamma jet model observed at different beam-angle and at different ages.\\ -\subsection{Observation of SGRs} -A stronger magnetic neutron star, a so-called ``Soft Gamma Repeaters (SGRs)'' periodically emit gamma-ray, and are extremely rare stars. Only four identified -SGRs are discovered in the last 20 years: SGR0526-66, SGR1806-20, SGR1900+14, SGR1627-41. GRBs and SGRs can be explained with an unique processing gamma jet model observed at different beam-angle and at different ages.\\ -\par -The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30 Jan 05. The fluence is $\sim$ 1$\times$10$^{-5}$erg/cm$^2$(15-350keV). This event have five orders of magnitude smaller than the giant flare from this source on 27 Dec 04. If a giant flare from SGR occurs as SGR1806-20, MAGIC has enough sensitivity for 100 second observation time.\\ -\par -MAGIC and Gamma-ray satellites react in the same way for also SGRs. - - - - - - - - - +The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30. January 2005. The fluence was $\sim$ 1$\times$10$^{-5}$erg/cm$^2$(15-350keV). This event was five orders of magnitude smaller than the giant flare from this source on the 27. December 2004. If a giant flare from SGR occurs as SGR1806-20, MAGIC would be able to detect the 100\,seconds delayed $\gamma$-emission from the source.