Changeset 6251 for trunk/MagicSoft/GRB-Proposal
- Timestamp:
- 02/04/05 12:30:47 (20 years ago)
- Location:
- trunk/MagicSoft/GRB-Proposal
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- 2 edited
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trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
r6237 r6251 79 79 As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches 80 80 with the one of \ma, 81 we cannot predict the alert frequency now to better than 100\% uncertainty. 81 we cannot predict the alert frequency now to better than 100\% uncertainty. 82 82 This leads to an expected observation time 83 of 5$\pm$5 hours per month. This number includes observation during moon-time.83 of 5$\pm$5 hours per month. This number includes observation during the moon-time. 84 84 We give a detailed description of the observation procedures in La Palma and 85 85 propose to spend one dedicated night to test the automatic alert procedure -
trunk/MagicSoft/GRB-Proposal/Introduction.tex
r6239 r6251 11 11 12 12 Very high energy (VHE) GRB observations have the potential to constrain the current GRB models 13 on both theprompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}.13 on both prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}. 14 14 Models based on both internal and external shocks predict VHE gamma-ray fluences comparable to, 15 15 or in certain situations stronger than, the keV-MeV radiation, 16 with durations ranging from shorter than the keV-MeV burst to extended TeV 16 with durations ranging from shorter than the keV-MeV burst to extended TeV 17 17 afterglows~\cite{DERMER, PILLA, ZHANG1, RAZZAQUE}. 18 18 … … 23 23 as well as photon-pion production~\cite{WAXMAN,BOETTCHER} and inverse-Compton scattering 24 24 in 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}.25 Long-term high energy (HE) $\gamma$-emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}. 26 26 This model predicts GeV inverse Compton emission even one day after the burst. 27 27 Even considering pure electron-synchrotron radiation, measurable GeV-emission for a significant … … 40 40 each indicating some excess over background but without stringent evidence. 41 41 The only significant detection was performed by \eg which was able to observe seven GRBs 42 emitting high energy (HE)42 emitting HE 43 43 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}. 44 44 There have been results suggesting gamma rays beyond the GeV range from the TIBET air shower array … … 57 57 and assuming an energy threshold of 15~GeV, a 5\,$\sigma$-signal rate of $0.5-2$ per year 58 58 was 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 than60 those observed by \ma, this number willstill have to be lowered.59 ($\sim$\,360/year). As the \sw alert rate is about factor~2 lower, including even fainter bursts than 60 those observed by \ma, this number still have to be lowered. 61 61 62 Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from a 62 Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from a 63 63 few 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 64 The model of~\cite{ASAF2} predict delayed GeV-emission that should be significantly detectable by \ma 65 65 in 100\,sec. 66 66 67 67 \subsection{Observation of XRFs} 68 68 69 While the major energy from the prompt GRBs is emitted in $\gamma$-rays with a peak energy of 200\,keV, 69 While the major energy from the prompt GRBs is emitted in $\gamma$-rays with a peak energy of 200\,keV, 70 70 X-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. 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. 73 73 The most popular theories ~\cite{DADO} suggest that XRFs are produced from GRBs observed ''off-axis''. 74 74 Alternatively, an increase of the baryon load within the fireball itself ~\cite{HUANG} or low efficiency shocks ~\cite{BARRAUD} could produce XRFs. 75 75 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}. \\ 76 76 77 Gamma-ray satellites react in the same way to XRFs and GRBs. 77 Gamma-ray satellites react in the same way to XRFs and GRBs. 78 78 In case of a detection the coordinates are distributed 79 79 to other observatories (see section 2.1). Only from later analysis the difference can be established. … … 85 85 \subsection{Observation of SGRs} 86 86 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 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 91 91 beam-angles and at different ages~\cite{FARGION}.\\ 92 92 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.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 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. 97 97 98 98
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