Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6096) +++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6097) @@ -54,11 +54,11 @@ %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope \\ - {\it \Large DRAFT 1.0 }} -\author{ N. Galante\\ \texttt{}\\ + {\it \Large DRAFT 2.0 }} +\author{ N. Galante\\ \texttt{}\\ M. Garczarczyk\\ \texttt{}\\ M. Gaug\\ \texttt{} \\ - S. Mizobuchi\\ \texttt{} + S. Mizobuchi\\ \texttt{} } - + \date{January, 2005\\} \TDAScode{MAGIC-TDAS 05-??\\ 0312??/NGalante} @@ -69,16 +69,16 @@ %% abstract %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{abstract} -We give a detailed plan for the observation of Gamma Ray Bursts for the year -2005. All observations will be triggered mainly by alerts of the satellites \he, \ig -and above all \sw. we expect an alert rate of a total of about +We give a detailed strategy for the observation of Gamma Ray Bursts (GRBs) for the first +half year of 2005. All observations will be triggered mainly by alerts of the satellites +\he, \ig and above all \sw. We expect an alert rate in total of about \par \ldots HOW MANY??? \ldots \par -per year out of which only about +per year out of which only about \par \ldots HOW MANY??? \ldots \par -will be followed by a position. -We give a detailed description of the observation procedures in La Palma and +will contain the GRB coordinates. +We give a detailed description of the observation procedures in La Palma and propose to review the situation in half a year from now. \end{abstract} @@ -109,31 +109,53 @@ %\theBibliography -%%>>>> Or the following if you include here by hand your +%%>>>> Or the following if you include here by hand your %%>>>> bibliographic entries \begin{thebibliography}{900} -\bibitem{design} The MAGIC Telescope, Design study for the construction of a 17~xm Cherenkov +\bibitem{design} The MAGIC Telescope, Design study for the construction of a 17~m diameter Cherenkov telescope for Gamma-Astronomy above 10~GeV, March 1998, Version 5 -\bibitem{PETRY} The MAGIC Telescope - Prospects for GRB research +\bibitem{PETRY} The MAGIC Telescope - Prospects for GRB research, D. Petry for the MAGIC collaboration, Astron. Astrophys. Suppl. Ser. 138, 601, 1999. +\bibitem{HARTMANN} Gamma-Ray Bursts and Cosmic Radiation Backgrounds, +Hartmann D.H., Kneiske T.M., Mannheim K.,Watanabe K., AIP Conference Proceedings, 662, 442, 2003. +\bibitem{MANNHEIM} Mannheim K., Hartmann D., Burkhardt F., AsJ, 467, 532, 1996. +\bibitem{SALOMON} Absorption of HE Gamma Rays by Interactions with Extragalactic Starlight Photons at High Redshifts and the HE Gamma-Ray Background, Salomon M.H., Stecker F.J., ApJ, 493, 547, 1998. +\bibitem{DERMER} Beaming, Baryon loading, and the Synchrotron Self-Compton Component in Gamma-Ray Bursts, +Dermer \& Chiang, ApJ, 537, 785, 2000. +\bibitem{PILLA} Emission Spectra from Internal Shocks in Gamma-Ray Burst Sources, +Pilla R.P., Loeb A., ApJ, 494, L167, 1998. +\bibitem{ZHANG1} High-Energy Spectral Components in Gamma-Ray Burst Afterglows, +Zhang \& Meszaros, ApJ, 559, 110, 2001. \bibitem{EGRET} Hurley K. et al., Nature, 372, 652 -\bibitem{HEGRA} Search for gamma-ray brusts above 20 TeV with the HEGRA AIROBICC -Cherenkov array, -L. Padilla et al., FAMN-97-1, Jul 1998, -submitted to A\&A, -astro-ph/9807342 -\bibitem{TIBET} Search for 10 TeV burst-like events coincident with the BATSE bursts -using the TIBET Air Shower Array, -Amenomori M. et al., -AIP Conf.Proc.558:8; -``Heidelberg 2000, High energy gamma-ray astronomy'' 844-849, 2001. -\bibitem{MILAGRO} The high-energy gamma-ray fluence and energy spectrum of GRB 970417A -from observations with Milagrito, -Milagro Collaboration (R. Atkins et al.). July 2002, -submitted to Astrophys. J., available at astro-ph/0207149 -\bibitem{GRAND} A Search for Sub-TeV Gammas in Coincidence with Gamma Ray Bursts, -Poirier J, et al., -submitted to Physical Review D -astro-ph/0004379 -\bibitem{TASC} M.M. Gonz{\'a}lez et al., Nature, 424, 749 (2002) +\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{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. +\bibitem{CONNAUGHTON1} A Search for TeV Counterparts to BATSE GRBs, +Connaughton at al., ApJ, 479, 859, 1997. +\bibitem{PADILLA} Search for Gamma-Ray Bursts above 20~TeV with the HEGRA AIROBICC Cherenkov Array, +Padilla at al., A\&A, 337, 43, 1998. +\bibitem{CONNAUGHTON2} A Search for TeV GRBs on a 1-second time-scale, +Connaughton at al., Astroparticle Physics, vol. 8, no. 3, 179, 1998. +\bibitem{MILAGRO} The high-energy gamma-ray fluence and energy spectrum of GRB 970417A +from observations with Milagrito, R. Atkins et al., ApJ, 533, L119, 2000. +\bibitem{GRAND} Sub-TeV Gammas in Coincidence with BATSE Gamma Ray Bursts, +Poirier J, et al., Physical Review D, 67, 042001, 2003. +\bibitem{TOTANI} Totani T., Astrophys. J. 502 L13 (1998), 509 L81 (1998), +536, L23, 2000. +\bibitem{WAXMAN} Waxman E., Phys. Rev. Lett. 75, 386, 1995. +\bibitem{BAHCALL} Waxman E., Bahcall J., Phys. Rev. Lett 78, 2292, 1997. +\bibitem{BOETTCHER} Boettcher M, Dermer C.D., Astrophys. J. 499 L131, 1998. +\bibitem{MESZAROS93} Meszaros P., Rees M., Astrophys. J. 418 L59, 1993. +\bibitem{CHIANG} Chiang J., Dermer C.D., Astrophys. J. 512 699, 1999. +\bibitem{ZHANG2} Zhang B., Meszaros P., Astrophys. J. 559 110, 2001. +\bibitem{LI} Li Z., Dai G., Lu T., accepted for A\&A, astro-ph/0208435, 2002. +\bibitem{ICRC} The MAGIC Telescope and the Observation of GRBs, +Galante N. et al., Proceedings of the 28$^{th}$ ICRC, Tsukuba, Japan, 2003. +\bibitem{NICOLA} Il Telescopio MAGIC per l'osservazione dei Gamma Ray Bursts, +Nicola Galante, tesi di laurea, (available at: http://www.pd.infn.it/magic/publi.html), 2002. + +%End of the list in the introduction + \bibitem{PAZCYNSKI} Pazcy\'{n}ski B., Astrophys. J. 308 L43 (1986) \bibitem{GOODMAN} Goodman J., Astrophys. J. 308 L47 (1986) @@ -141,39 +163,14 @@ \bibitem{XU} Pazcy\'{n}ski B., Xu G., Astrophys. J. 427 708 (1994) \bibitem{REES} Rees M., Meszaros P., MNRAS 258 P41 (1992) -\bibitem{MESZAROS93} Meszaros P., Rees M., Astrophys. J. 418 L59 (1993) \bibitem{MESZAROS94} Meszaros P., Rees M., MNRAS 289 L41 (1994) -\bibitem{WAXMAN} Waxman E., Phys. Rev. Lett. 75, 386 (1995) -\bibitem{TOTANI} Totani T., Astrophys. J. 502 L13 (1998), 509 L81 (1998), -536 L23 (2000) -\bibitem{BAHCALL} Waxman E., Bahcall J., Phys. Rev. Lett 78, 2292 (1997) -\bibitem{CHIANG} Chiang J., Dermer C.D., Astrophys. J. 512 699 (1999) -\bibitem{BOETTCHER} Boettcher M, Dermer C.D., Astrophys. J. 499 L131 (1998) -\bibitem{DERMER} Beaming, baryon-loading, and the synchrotron self-compton component in gamma-ray burst blast waves energized by external shocks, -Dermer C.D., Chiang J., Mitman K.E., 1999, submitted to ApJ., -astro-ph/9910240 -\bibitem{PILLA} Emission spectra from internal shocks in gamma-ray burst sources, -Pilla R.P., Loeb A., 1998, ApJ 494, L167 (astro-ph/9710219). -\bibitem{ZHANG} Zhang B., Meszaros P., Astrophys. J. 559 110 (2001) -\bibitem{HARTMANN} Hartmann D.H., Kneiske T.M., Mannheim K.,Watanabe K., -2002, -astro-ph/0201299 -\bibitem{LI} Li Z., Dai G., Lu T., accepted for A\&A, astro-ph/0208435 (2002) -\bibitem{MANNHEIM} Mannheim K., Hartmann D., Burkhardt F., Astrophys. J. 467 532 (1996) -\bibitem{SALOMON} Salomon M.H., Stecker F.J., Astrophys. J. 493 547 (1998) -\bibitem{PRIMACK} Primack J.R., Sommerville R.S., MacMinn D., Astrophys. J. 11 93 (1999) -\bibitem{ICRC} The MAGIC Telescope and the Observation of GRBs, -Galante N. et al., Proceedings of the 28$^{th}$ ICRC, Tsukuba, Japan, 31\,July\ -\ 1\, August, 2003. -\bibitem{NICOLA} Il Telescopio MAGIC (Major Atmospheric Gamma Imaging Cherenkov Telescope) -per l'osservazione dei Gamma Ray Bursts, Nicola Galante, tesi di laurea, July 2002. -(available at: http://www.pd.infn.it/magic/publi.html) \bibitem{NICOLAGRB} http://www.pd.infn.it/magic/GRB/grb.html \bibitem{GCNARCHIVE} http://lheawww.gsfc.nasa.gov/docs/gamcosray/legr/bacodine/gcn3\_archive.html \bibitem{GOTZ} D. Gotz, S. Mereghetti 2002 Observation of Gamma-ray Bursts with INTEGRAL -Contribution to the XXII Moriond Astrophysics Meeting, +Contribution to the XXII Moriond Astrophysics Meeting, The Gamma Ray Universe, Les Arcs 9-16 March 2002. -\bibitem{IBAS} IBAS Client Software, Users Manual, -available at: +\bibitem{IBAS} IBAS Client Software, Users Manual, +available at: http://isdc.unige.ch/$\sim$isdc\_cms/icms/releases/public/ibas\_client/1.1.2/ibas\_client\_um-1.1.2.ps.gz -\bibitem{HETE} +\bibitem{HETE} (see also: http://space.mit.edu/HETE/mission\_status.htm \\ http://space.mit.edu/HETE/ban.html ) @@ -182,5 +179,5 @@ \bibitem{SWIFT} The SWIFT homepage http://swift.gsfc.nasa.gov/science/ -\bibitem{SWIFT2} +\bibitem{SWIFT2} http://swiftsc.gsfc.nasa.gov/docs/swift/swiftsc.html \end{thebibliography} Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6096) +++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6097) @@ -1,77 +1,54 @@ \section{Introduction} -The MAGIC telescope has been designed especially light with a special focus on -being able to react fastly to GRB alerts from the satellites. -In \cite{design} and~\cite{PETRY}, -the objective was set to turn the telescope to the burst position in 10-30~s -in order to have a fair chance of detecting a burst with the MAGIC telescope. -The current possible value is 20 sec. for full turn-around -%FIXME -{\it \bf THIS HAS TO BE CHECKED FROM THOMAS B. !!} + +\subsection{Observation of GRBs} + +The MAGIC telescope has been designed especially light with a special focus on +being able to react quickly to GRB alerts from the satellites. +In \cite{design} and~\cite{PETRY}, +the objective was set to turn the telescope to the burst position within 10-30~s +in order to have a fair chance of detecting a burst when the emission is still ongoing. +During the comissioning phase we have proven that our goal was reached. +The telescope is able to turn 180 degrees in azimuth and 160 degrees in zenith within 20s.\\ + + +Very high energy (VHE) GRB observations have the potential to constrain the theoretical models +on both the prompt and extendend phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}. Models based on both internal and external shocks predicts VHE fluence comperable to, or 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 -Several attempts have been made in the past to observe GRBs at energies -from the GeV range upwards each indicating some excess over background but -without stringent evidence. The only secured detection was performed by EGRET -which detected seven GRBs emitting high energy photons in the -100~MeV to 18~GeV range~\cite{EGRET}. There have been -results suggesting gamma rays beyond the GeV range from the TIBET array~\cite{TIBET} and -from HEGRA-AIROBICC~\cite{HEGRA}. Evidence for TeV emission of one burst was claimed by -the MILAGRITO experiment~\cite{MILAGRO}. Recently, the GRAND array has reported some -excess of observed muons during seven BATSE bursts~\cite{GRAND}. In this context, note -especially a recent publication from the TASC detector on \eg~\cite{TASC}, -finding a high-energy 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 limit (200 MeV). + +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 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}.\\ + +GeV energy emission in GRBs is particulary sensitive to the Lorentz factor and to the photon density of the emitting material - and thus to the distance of the radiating shock from the source - owing to $\gamma~\gamma \rightarrow$ +\textit{e$^+$~e$^-$} absorption in the emission region. And, Comparison of the prompt GRB flux at $\sim$ 1GeV and $\sim$ 100keV may allow to determine the magnetic field strength~\cite{ASAF1}. + \par -The nowadays most widely accepted model for gamma emission from GRB suggests a bursts -environment involving collisions of an ultra-relativistic e$^+$-e$^-$ -plasma fireball~\cite{PAZCYNSKI,GOODMAN,SARI}. These fireballs may produce -low-energy gamma rays either by ``internal'' collisions of multiple -shocks~\cite{XU,REES} or by ``external'' collisions of a single shock -with the ambient circum burst medium (CBM)~\cite{MESZAROS94}. + +Several attempts have been made in the past to observe GRBs at energies from the GeV range upwards, each indicating some excess over background but without stringent evidence. The only secured detection was performed by EGRET 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 rollover 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 Cerenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA}, Whipple~\cite{CONNAUGHTON2} and the Milagro prototype~\cite{MILAGRO}. +The GRAND array has reported some excess of observed muons during seven BATSE bursts~\cite{GRAND}. In this context, note especially the publication from the TASC detector on \eg~\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 limit (200 MeV).\\ + +Concerning estimates about the MAGIC observability of GRBs, a very detailed study of GRB spectra obtained from the third and fourth \ba catalogue has been made in~\cite{ICRC,NICOLA}. The spectra were extrapolated to \ma energies with a simple continuation of the observed high-energy power law behaviour and the calculated fluxes compared with \ma sensitivities. Setting conservative cuts on observation times and significances, +and assuming an energy threshold of 15~GeV, a GRB detection rate of $0.5-2$ per year +was obtained for an assumed observation delay between 15 and 60 sec. and a BATSE trigger rate ($\sim 360/year$). + +Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, an late afterglow emission from few tens of GRB's per year should be observable above our energy threshold. The model of Name~\cite{ASAF2} predict delayed GeV photon 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 dominated X-ray fluence. Because of similar properties a connection between XRFs and GRBs is strongly suggested. The most popular theories say that XRFs are produced from GRBs observed ''off-axis''. +Alternativly, 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 low redshifts (z < 0.6).\\ + +Gamma-ray satellites react in the same way on 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. + \par -In many publications, -the possibility that more energetic gamma-rays come along with the (low-energy) gamma-ray -burst, have been explored. -Proton-synchrotron emission~\cite{TOTANI} have -been suggested as well as photo-pion production~\cite{WAXMAN,BAHCALL,BOETTCHER} -and inverse-Comption -scattering in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG}. -Long-term high-energy gamma emission from accelerated protons in forward-shock -has been predicted in~\cite{LI}. -Even considering pure electron-synchrotron radiation predicts measurable GeV emission for a -significant fraction of GRBs~\cite{ZHANG}. -Implications of the observation of a high-energy gamma-ray component on -distance scale, energy production in the GRB and distinction between internal and -external shock models have been treated in~\cite{HARTMANN,MANNHEIM,SALOMON,PRIMACK}. -\par -\ldots {\bf MORE ELABORATE TREATMENT OF HE-EMISSION: WHICH MODELS, WHAT TIME DIFFERENCE TO -GRB, TIME DEVELOPMENT, EXPECTED FLUXES, SPECTRA } \ldots -\par -\ldots {\bf UPDATE CURRENT PAPERS} \ldots -\par -\par -\ldots {\bf MORE DETAILED DESCRIPTION OF GEV-EMISSION MODELS }\ldots -\par -\par -\ldots {\bf SATOKO AND MARKUS GARCZ.}\ldots -\par -In the year 2005, three satellites will produce GRB alerts: The \he -satellite, launched in October 2000, the \ig satellite, launched October 2002 and the -\sw satellite, launched in October, 2004 and expected to be fully operational in March, 2005. -\par -Concerning estimates about the MAGIC observability of GRBs, a very detailed study -of GRB spectra obtained from the third and fourth \ba catalogue has been made -in~\cite{ICRC,NICOLA}. The spectra were extrapolated to \ma energies with a simple continuation -of the observed high-energy power law behaviour and the calculated fluxes compared -with \ma sensitivities. Setting conservative cuts on observation times and significances, -and assuming an energy threshold of 15~GeV, a GRB detection rate of $0.5--2$ per year -was obtained for an assumed observation delay of 15~sec. and the \sw GRB trigger rate ($\sim 100/year$). -\subsection{Observing XRFs} +In this case we include also observation of XRFs by MAGIC in our proposal. -{\ldots \it \bf CAN BE MAYBE GO INTO A SEPARATE PROPOSAL \ldots \\} -\subsection{Observing SGRs} -{\ldots \it \bf CAN BE MAYBE GO INTO A SEPARATE PROPOSAL \ldots \\} - Index: /trunk/MagicSoft/GRB-Proposal/Requirements.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/Requirements.tex (revision 6096) +++ /trunk/MagicSoft/GRB-Proposal/Requirements.tex (revision 6097) @@ -1,3 +1,6 @@ \section{Requirements to start the full GRB Observations} + +\subsection{Status now} +\subsection{What is still missing:} \ldots {\bf Communication AMC-CC } \ldots @@ -5,2 +8,6 @@ \ldots {\bf Fast slewing } \ldots +\ldots {\bf Test GRB Monitor } \ldots +\ldots {\bf Test fast telescope movement} \ldots +\ldots {\bf Simulation with fake alerts to ...CRAB???...} \ldots +