Index: trunk/MagicSoft/GRB-Proposal/GRB_proposal_2003.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/GRB_proposal_2003.tex (revision 5965) +++ trunk/MagicSoft/GRB-Proposal/GRB_proposal_2003.tex (revision 5965) @@ -0,0 +1,795 @@ +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%%% magic-tdas.tex -- template to write MAGIC-TDAS documents +%%%----------------------------------------------------------------- +%%% Kopyleft (K) 2000 J C Gonzalez +%%% Max-Planck-Institut fuer Physik, +%%% Foehringer Ring 6, 80805 Muenchen, Germany +%%% E-mail: gonzalez@mppmu.mpg.de +%%%----------------------------------------------------------------- +%%% This program is free software; you can redistribute, copy, +%%% modify, use it and its documentation for any purpose, +%%% provided that the above copyright notice appear in all +%%% copies and that both that copyright notice and this +%%% permission notice appear in supporting documentation. +%%% +%%% This piece of code is distributed in the hope that it will +%%% be useful, but WITHOUT ANY WARRANTY; without even the +%%% implied warranty of FITNESS FOR A PARTICULAR PURPOSE. +%%% +%%% Although you can actually do whatever you want with this +%%% file (following the copyright notice above), your are +%%% strongly encouraged NOT to edit directly this file. +%%% Instead, make a copy and edit the copy for your purposes. +%%% +%%% Modifying thie original file means that you actually have +%%% the (very basic) knowledge needed to make things by your +%%% own, and therefore... you will not get _any_ additional +%%% support :-) +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%%% Last update: Time-stamp: +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% +\documentclass[12pt]{article} + +\usepackage{magic-tdas} +\usepackage{xspace} +%\usepackage[polish]{babel} +\newcommand{\he}{HETE-2\xspace} +\newcommand{\ig}{INTEGRAL\xspace} +\newcommand{\sw}{SWIFT\xspace} +\newcommand{\eg}{EGRET\xspace} +\newcommand{\ba}{BATSE\xspace} +\newcommand{\ma}{MAGIC\xspace} +\newcommand{\ip}{IPN\xspace} +\newcommand{\g}{GCN\xspace} + +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%% BEGIN DOCUMENT +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +\begin{document} + +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%% Please, for the formatting just include here the standard +%% elements: title, author, date, plus TDAScode +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +\title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope \\ + {\it \Large DRAFT 0.0 }} +\author{ N. Galante\\ \texttt{}\\ + M. Garczarczyk\\ \texttt{}\\ + M. Gaug\\ \texttt{} \\ + S. Mizobuchi\\ \texttt{} +} + +\date{December, 2003\\} +\TDAScode{MAGIC-TDAS 02-??\\ 0312??/NGalante} +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%% title %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +\maketitle + +%% abstract %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +\begin{abstract} +We give a detailed plan for the observation of Gamma Ray Bursts for the year +2004. All observations will be triggered by alerts of the satellites \he, \ig, +\sw or by other circulars by the \g. Based on \he experience from the year 2002, +we expect an alert rate of a total of about 50 per year out of which only about 20 will +be followed by a position. +%FIXME +{\it \bf THIS HAS STILL TO BE UPDATED FOR 2003 !!} +The majority of these alerts will be based on ground analysis and +arrive with a delay of about an hour or more. +\end{abstract} + +%% contents %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%\thetableofcontents + +\newpage + +%% body %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% + +%------------------------------------------------------------ +\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. !!} +\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). +\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}. +\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 +In the year 2004, mainly three satellites will produce the bulk of the GRB alerts: The \he +satellite, launched in October 2000, the \ig satellite, launched October 2002 and the +\sw satellite, scheduled for launch in May, 2004. +\par +% HERE +We will give an overview of the types of alarms, we expect from the three satellites +and add then our proposal for observation strategies. Note that while there is already some +experience accumulated from the \he and \ig alarms, we do not know yet how \sw will perform +since it is still not launched. Because the observation of GRBs will differ +from conventional observations in several aspects, we also propose a detailed plan to test + and calibrate the system in order to meet our purposes. +\par +{\ldots \it \bf THIS IS TO BE CHECKED BY NICOLA G. !! \ldots \\} +\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 ($\sim 100/year$). + + +\section{\he Alarms} + +{\it \bf THIS HAS TO BE UPDATED TO 2003 !!} + +The HETE mission has three instruments on board which can generate burst triggers: +Fregate, the WXM, and the SXC. +Fregate data are examined in two broad energy channels: +5-80 keV and 30-400 keV. +The WXM data are from 2-30 keV, +and the SXC data are from 1.5 to 12 keV. +\par +The Fregate data are searched for counts excesses on four different timescales: +20 ms, 160 ms, 1.3 s, and 5.2 s. +The threshold for a count excess to be considered significant is generally around 5 sigma. +Such an excess must be seen in two of the four Fregate detectors on the same timescale +for a burst to be considered real. +\par +The WXM data are examined on multiple timescales between 80 ms and 10 s. +The thresholds are all near 5 sigma. This analysis is done on one of the on-board transputers. +\par +Fregate data are also analyzed on multiple timescales in a manner identical +to that for the WXM data on the same transputer the WXM data are analyzed by. +\par +SXC data can be used to create a continuous series of cross-correlation maps using a dedicated DSP, +and a burst is registered when the peak of the cross-correlation map exceeds a threshold. +Because of the difficulties with the SXC hardware, SXC triggering is currently not operating. +\par +When a burst is detected, the real-time spacecraft notification will distribute +\begin{itemize} +\item the energy range of the burst (1.5-12 keV, 2-30 keV, 5-80 keV, or 30-400 keV) +\item the timescale of the trigger (from 20 ms to over 10 s) +\item the S/N or the peak count rate of the burst +\end{itemize} +\par + +In the year 2002, about 630 internal \he triggers occurred, out of which about 75 were +considered as GRBs or possible GRBs by the ground analysis. About 50 of these bursts +were subsequently considered as real\cite{HETE-SUM}. Note that about 40 of +another species of bursts called ``X-ray bursts'' (XRB) were detected, mainly while the +satellite was looking towards the Galactic center. +\par + +The real-time alerts sent to the \g by \he have the following signature~\cite{HETE}: +\begin{description} +\item[ALERT] If the burst is detected using photons in the 5-80 keV or 30-400 keV bands, +regardless whether a position has been determined or not. This type of alert has occurred +about 170 times in 2002. +\item[UPDATE] If a position is determined on board and it is considered significant enough, +the RA and declination of the burst will be distributed in this type to the \g. + Each additional position determined on board +(each with higher significance than all determined before) +will result in a new Notice of type UPDATE. In 2002, about 10 UPDATE's were sent to +the \g, two third of which had a position error of about 1 arcmin, one third with about +half an arcmin. +\item[LAST] Once the on-board processing of data near the time of the trigger is complete, +there will be no more immediate results from the spacecraft, +a summary Notice this type is distributed. In 2002, about 120 LAST's were sent out to the \g, +containing about 20 positions of bursts. +\end{description} +The quality of the real-time positions are assured by making a cut on the lightcurve S/N and the +image S/N in a way that with $>$90\% the real-time position is correct. +As a result, HETE positions distributed in real time from the spacecraft are in one of two categories: +\begin{itemize} +\item Category I: +The image and lightcurve S/N all exceed 3.0, +so the position is distributed with a 90\% error radius of 12-14 arcminutes. +\item Category II: +Not all of the image and lightcurve S/N exceeds 3.0, +but the quadrature sum of the image S/N from the WXM X and Y detectors is > 3.7, +and neither the X nor the Y incident angle exceeds 30 degrees, +so the position is distributed with a 90\% error radius of 30 arcminutes. +\end{itemize} + +In order to accommodate those observers who would like to make their own estimate +of the quality of a real-time burst localization, also included in the \g message are: +\begin{itemize} +\item The image S/N from the X and Y modules of the WXM +\item The lightcurve S/N from the X and Y modules of the WXM +\item The longitude of the HETE spacecraft at the time of the trigger. +\end{itemize} +The higher the image and lightcurve S/N, +the more reliable the localization will be. +Low values of image and lightcurve S/N are typically associated with events +localized at the edge of the instrument FOV. +\par +This method of distribution of \g Notices results in a few common situations: +\begin{itemize} +\item If there is no significant position calculated in real time on board, +there will be no burst coordinates in any \g Notice. +If ground analysis reveals a position, +it will be sent out as a type GND\_ANALYSIS Notice. +\item Because the Burst Alert Station coverage is not always 100\%, +there can be gaps in the reception of burst data from the spacecraft. +If the flight analysis of a burst is over before a Burst Alert Station is seen, +the full analysis of the burst will be sent in two Notices, +one of type ALERT and the other of type LAST. +This means that a Notice of type ALERT could, in principle, +contain the coordinates of the burst. +\end{itemize} +Both the WXM and SXC search data from seconds before the burst trigger to minutes after, +looking for the image of the burst. The WXM software matches the shadow pattern on the detector +with template patterns, looking for a best fit; the SXC looks for peaks in the cross-correlation map. +In either case, if a significant position is found in either instrument, +its location is sent to the ground in real time. +Once the positions and their significances are received on the ground, +the RA and declination of the image are calculated and, +if the significances are high enough, transmitted to the \g. +At present, SXC positions are not sent to the \g automatically, +but rather only after ground analysis. + +\par +Ground analysis of a burst begins as soon as the full burst data reach MIT after a +Primary Ground Station contact (from a few minutes to over an hour after the burst). +Automated software performs standard analyses of the downlinked data, +and a human is notified to make the final decisions. +A followup \g Notice, of type GND\_ANALYSIS, +will be distributed under the following circumstances: +\begin{itemize} +\item There was no position calculated on board, but ground analyses reveal a significant position. +\item There was a position calculated on board and ground analyses can improve the coordinates +and/or reduce the error box size. +\item There was a position calculated on board, but there is actually no significant position in the data. +\end{itemize} +In general, if there is a position in a real-time \g Notice, +it should be considered accurate. +If there is no position in a real-time \g Notice, +a position may be forthcoming within an hour or so of the original Notice. +If a burst position was distributed and it is wrong because of software or operator error, +a GND\_ANALYSIS message will be distributed; +if no position was distributed, no GND\_ANALYSIS message will be sent. +In 2002, about 25 ground analyses contained positions of GRB's and 5 further of XRB's. +\par + +From the 30 bursts with position sent to the \g in 2002, \ma would have had 7 in its FOV +which are listed in the following table: +\begin{table}[h] +\label{tab:heteoverlap} +\begin{center} +{\small +\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|} +\hline +\hline +GRB & date & UTC & RA & dec. & error & $\theta$ & $\phi$ & flag & comments\\ +name & (dd.mm)& & & & arc. & MA- & MA- & providing & \\ + & & & & & min. & GIC & GIC & position & \\ +\hline +-- & 27.11. & 1:20:39 & 53.78 & -15.84 & 60 & 48 & 198 & UPDATE & probable GRB \\ + & & & & & & & & & moon at:\\ + & & & & & & & & & $\theta= 77^\circ, \phi=77^\circ$\\ +\hline +GRB021113 & 13.11. & 06:38:57 & 23.47 & 40.4 & 28 & 85 & 314 & GND & no moon \\ +\hline +GRB021112 & 12.11. & 03:28:16 & 39.22 & 48.8 & 54 & 40 & 313 & GND & no moon \\ +\hline +GRB020813 & 13.08. & 02:44:19 & 296.66 & -19.6 & 28 & 67 & 229 & ALERT & no moon \\ +\hline +-- & 28.07. & 21:44:58 & 273.67 & -12.13 & 28 & 45 & 153 & UPDATE & probable GRB\\ + & & & & & & & & & no moon \\ +\hline +GRB020531 & 31.05. & 00:26:18 & 228.69 & -19.36 & 77 & 49 & 191 & GND & +moon at: \\ + & & & & & & & & & $\theta= 87^\circ, \phi=118^\circ$ \\ +\hline +GRB020127 & 27.01. & 20:57:24 & 123.77 & 36.74 & 240 & 51 & 64 & UPDATE & +moon at: \\ + & & & & & & & & & $\theta= 47^\circ, \phi=83^\circ$ \\ +\hline +\hline +\end{tabular} +} +\end{center} +\caption{\he bursts, which would have been in principle visible from the \ma telescope site at +night. No burst durations, alert delays, weather conditions, etc. are displayed. For more +detailed information on single bursts, see~\cite{NICOLAGRB}.} +\end{table} + +As one can see from table~\ref{tab:heteoverlap}, more overlap bursts +than expected from randomly superimposed fields of view ($\sim$1--2 bursts only), +have been found. As expected from the increase of covered solid angle at high +zenith angles, all bursts had rather larger zenith angles ($\theta \geq 40^\circ$) +culminating and cover the whole range of azimuths. +\par +Additionally, five bursts occurred during the day, but would have moved into the \ma FOV in a +delay of less than six hours (see table~\ref{tab:hetelongoverlap}): +\begin{table}[h] +\label{tab:hetelongoverlap} +\begin{center} +{\small +\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|} +\hline +\hline +GRB & date & UTC & RA & dec. & error & $\theta$ & $\phi$ & flag & comments\\ +name & (dd.mm)& & & & arc. & MA- & MA- & providing & \\ + & & & & & min. & GIC & GIC & position & \\ +\hline +-- & 15.07. & 18:45:40 & 273.7 & -12.1 & 2.0 & 51 & 138 & UPDATE & XRB \\ + & & & & & & & & & $\theta$ and $\phi$ at 21:43:00 UTC \\ + & & & & & & & & & moon at:\\ + & & & & & & & & & $\theta= 69^\circ, \phi=252^\circ$\\ +\hline +-- & 09.06. & 20:45:37 & 275.9 & -30.4 & 1.4 & 88 & 126 & LAST & possible GRB \\ + & & & & & & & & & $\theta$ and $\phi$ at 21:43:00 UTC \\ + & & & & & & & & & no moon \\ +\hline +-- & 08.06. & 16:02:39 & 275.9 & -30.4 & 2.2 & 89 & 125 & GND & XRB \\ + & & & & & & & & & $\theta$ and $\phi$ at 21:43:00 UTC \\ + & & & & & & & & & no moon \\ +\hline +GRB020331 & 31.03. & 16:32:28 & 199.1 & -17.9 & 20 & 86 & 113 & GND & $\theta$ and $\phi$ at 21:49:00 UTC \\ + & & & & & & & & & no moon \\ +\hline +GRB020317 & 17.03. & 18:15:31 & 155.8 & 12.7 & 36 & 46 & 101 & GND & $\theta$ and $\phi$ at 21:40:00 UTC \\ + & & & & & & & & & moon at:\\ + & & & & & & & & & $\theta= 19^\circ, \phi=271^\circ$\\ +\hline +\hline +\end{tabular} +} +\end{center} +\caption{\he bursts, which would have been in principle visible from the \ma telescope site occurring +during the day but moving into the \ma FOV in less than six hours. +No burst durations, alert delays, weather conditions, etc. are displayed. For more +detailed information on single bursts, see~\cite{NICOLAGRB,GCNARCHIVE}. Two bursts are marked +as XRB (X-ray bursts) a phenomenon seen regularly by the \he WXM while looking into the Galactic Center.} +\end{table} + +The \he field of view spans roughly 75$^\circ$ in DEC and and 5 hrs in RA. +Because \he is anti-solar pointing, its field-of view drifts along the ecliptic +at a rate of about one degree per day. Its maximum declination reaches 60$^\circ$ with the lower + border of its field of view at about -15$^\circ$. Its minimum declination reaches -60$^\circ$ +with the upper border at about +15$^\circ$~\cite{HETE}. +The best overlap between \ma and \he fields of view +is thus in the winter, between October and March. + +\section{\ig Alarms} + +{\ldots \it \bf THIS IS TO BE UPDATED TO 2003 !! \ldots \\} +\par +The \ig satellite was successfully commissioned in March 2003. +The use of INTEGRAL is planned for 2 years with a possible extension for up to 5 years. + +\par +The satellite contains four main instruments: +\begin{description} +\item[IBIS:\xspace] The imager IBIS (Imager on Board the INTEGRAL Satellite) +will achieve an angular resolution of 12 arcmin over an energy range between 15 keV and 10 MeV. +\item[SPI:\xspace] The spectrometer SPI (SPectrometer on INTEGRAL) +will provide spectral analysis of gamma-ray point sources +as well as extended sources over an energy range between 20 keV and 8 MeV. +\item[JEM-X:\xspace] +Two identical X-ray monitors, JEM-X (Joint European X-ray Monitor) will work +simultaneously with the other instruments in the energy range between 3 and 35 keV +and with an angular resolution of one arcmin. +\item[OMC:\xspace] +The optical monitoring camera, OMC, covers a field of 17.6 x 17.6 arcsec. +The total field of view of the OMC camera will be of 5 x 5 degrees. +\end{description} + +\par +Alerts with the coordinates of GRBs will be distributed via internet +with a small delay with respect to the GRB occurrence. +It is expected that this delay will be smaller than a few minutes. The alerts as +such can be delivered to the recipient within 1 second. +The expected rate of GRBs that will be localized with an accuracy of a few arcminutes +is of the order of 1-2 per month~\cite{GOTZ}. +\par +The IBAS alerts are sent via internet, using the UDP transport protocol. The Client Software +made available by \ig together with the first real alerts are currently being tested in Barcelona. +Five Alert Types have been defined so far~\cite{IBAS}: +\begin{description} +\item[POINTDIR] Gives the \ig pointing direction (e.g. to obtain reference images of the pre-GRB sky). No +alert is attached with this type. +\item[SPIACS] +SPIACS alert packets will be sent after positive triggers detected with the +SPI Anti-Coincidence Shield (ACS). No position information will be available, +unless the same GRB also triggers some of the imaging instruments +and in such a case the position will come through other packet types. +\item[WAKEUP] +WAKEUP packets are generated only once for each GRB +and only if the GRB position information is available. +They contain the preliminary position derived for the GRB. +These are the alerts with the shortest time delay. +Any (potential) GRB will generate only one WAKEUP packet. +\item[REFINED] +REFINED packets provide refined information on a GRB event. +Zero to several REFINED packets can be generated for a given GRB. +\item[OFFLINE] +OFFLINE packets are generated manually after interactive analysis of the data has been performed +offline by a Duty Scientist. +The time delay might be from one to a few hours (or even longer in some cases). +\end{description} + +One \ig burst was delivered to the GCN up to now. It would have been visible +by \ma with a delay of about 1.5 hours (see table~\ref{tab:integraloverlap}). + +\begin{table}[ht] +\begin{center} +{\small +\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|} +\hline +\hline +GRB & date & UTC & RA & dec. & error & $\theta$ & $\phi$ & flag & comments\\ +name & (dd.mm)& & & & arc. & MA- & MA- & providing & \\ + & & & & & min. & GIC & GIC & position & \\ +\hline +GRB021125 & 25.11. & 17:58:30 & 19.78 & 28.1 & 30 & 51 & 280 & --- & no moon \\ + & & & & & & & & & $\theta$ and $\phi$ at 19:37:00 UTC \\ +\hline +\hline +\end{tabular} +} +\end{center} +\label{tab:integraloverlap} +\caption{\ig bursts, which would have been in principle visible from the \ma telescope site at +night. No burst durations, alert delays, weather conditions, etc. are displayed. For more +detailed information on single bursts, see~\cite{NICOLAGRB,GCNARCHIVE}.} +\end{table} + +The period of the INTEGRAL orbit is 3 sideral days, +so that the perigee occurs always above the same geographical point on Earth. + +%It is a highly eccentric orbit, +%with a perigee height of 10'000 km and +%an apogee height of 152'600 km +%with an inclination of 51.6 degrees with respect to the equatorial plane. + + +\section{\sw Alarms} + +{\ldots \it \bf THIS IS TO BE UPDATED !! \ldots \\} + +The \sw satellite~\cite{SWIFT} is scheduled for launch in May, 2004 for a nominal two-years mission. +\par +It contains three instruments: +\begin{description} +\item[BAT:\xspace] The BAT has an large field of view (1.4~sr) in an energy range of 15-150~keV. +It has an angular resolution of 22 arcmin. and is itself able to determine GRB source locations (of +5$\sigma$ or higher) to a resolution of 4 arcmin. It is predicted to locate more than 100 sources +per year. +\item[XRT:\xspace] The X-Ray Telescope on \sw provides afterglow positions of 5 arcsec. accuracy within +100 sec. of the burst alert from BAT in an energy range of 0.2-10~keV. +\item[UVOT:\xspace] +The UVOT is designed for optical images of the GRB field 20-60 sec. after the GRB alert and +in a wavelength range between 170 and 650~nm. +\end{description} + +1--4 arcmin. position estimates of the GRB coordinates are predicted to arrive at ground within +15 seconds~\cite{SWIFT2}. +\par +\sw autonomously sends preliminary information to the GCN, including a crude optical finding chart +populated with postage stamp images around detected stars in UVOT, and BAT and XRT source positions +and spectra. Within hours of the next ground pass, the Swift Science Data Center (SDC) +initiates autonomous pipeline processing of the telemetry and serves it immediately +to the community on its Quick-Look area, available to the community (FITS-files). + +\section{Further Possible Alarms} + +\subsection{IPN position notices} + +These notices are sent out by the GCN itself with GRB positions obtained +after triangulation of at least three satellites +using the individual arrival times and positions of the spacecrafts \he, \ig, +KONUS, NEAR, MARS and ULYSSES. +Usually, these messages arrive +after previous alerts by the satellites themselves and refine the GRB position determination. + +There are two types of messages: +\begin{description} +\item[IPN\_SEG:\xspace] +These Notices use the data from two different spacecrafts. +Triangulation +yields an annulus for possible GRB positions. +The annulii segments are long (2-10deg) and narrow (2-30armin). +%yielding an error box area of 4 sq.arcmin to 5 sq.deg. +%The range of time delays is on average 24 to 48 hours (with the shortest being 11 hours to date). +These message will not be considered further here +because their position uncertainties are too large. +\item[IPN\_POS:\xspace] +For IPN\_POS Notices, the error boxes will be in the several arcmin and above range. +For about 55\% of the Notices there will be only a single error box, +but because 3 sources yield only 2 unique annuli and these 2 annuli cross in 2 locations, +there can be 2 error boxes reports (~25\% of the cases). +Depending on the relative timing of the GRB and the data dumps through the DSN, +the wait can be 1-25 hours (more on the weekends). +In 2002, 22 such messages were sent out with errors in the range of usually +5--30 arcmin. There were no messages before the May 5$^{th}$, however. +\end{description} + +Only one burst would have been announced by an IPN\_POS in less than 12 hours after the burst +(see table~\ref{tab:ipnoverlap}). + +\begin{table}[ht] +\label{tab:ipnoverlap} +\begin{center} +{\small +\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|} +\hline +\hline +GRB & date & UTC & RA & dec. & error & $\theta$ & $\phi$ & flag & comments\\ +name & (dd.mm)& & & & arc. & MA- & MA- & providing & \\ + & & & & & min. & GIC & GIC & position & \\ +\hline +GRB021016 & 16.10. & 10:29:00 & 8.43 & 46.8 & 22 & 61 & 43 & IPN\_POS & +$\theta$ and $\phi$ at 22:06:48 UTC \\ + & & & & & & & & & moon at: \\ + & & & & & & & & & $\theta= 87^\circ, \phi=118^\circ$ \\ +\hline +\hline +\end{tabular} +} +\end{center} +\caption{\ip bursts, which would have been in principle visible from the \ma telescope site at +night. Only bursts which have been announced with less than 12 hours are taken into account. +No burst durations, weather conditions, etc. are displayed. For more +detailed information on single bursts, see~\cite{NICOLAGRB,GCNARCHIVE}.} +\end{table} + +\section{Proposed Observation Strategies} + +{\ldots \it \bf THIS IS TO BE UPDATED !! \ldots \\} +\par +One can see from tables~\ref{tab:heteoverlap},~\ref{tab:hetelongoverlap},~\ref{tab:integraloverlap} +and~\ref{tab:ipnoverlap} that observing GRBs +at moon periods will significantly increase the chance to observe some. +Three out of the seven bursts from table~\ref{tab:heteoverlap} +would have occurred in astronomical twilight +or very close to the start or end of observation +(GRB021113 half an hour after usual closing of the telescope and +GRB020127 and the one on 28.7. each three quarters of an hour after usual +start). If we want to have a realistic chance to observe bursts, it is therefore +important to use all available time {\it including moon periods, periods of astronomical +twilight and putting the telescope as soon as possible in GRB-alert position}. + +\subsection{What to do at alerts without position (yet)} + +{\ldots \it \bf THIS IS TO BE REWRITTEN !! \ldots \\} + +\begin{verbatim} +suggestion email Martin Kestel: \\ +\\ +When you put the telescope in Alt=90 degrees (zenith) and Az=90 degrees east, +you have at most 90 degrees to move in either +axis in order to reach any position on the sky, either in normal tracking mode +or in reverse tracking mode. The actual speed will most probably be different +in the two axes and the elevation will probably be slower, as it has only one +motor attached. Now, the maximum elevation movement from zenith will +correspond to the maximum zenith angle you want your GRB to have, so, +this number will be certainly smaller than 90 degrees. +\end{verbatim} + +\subsection{What to do at alerts with position} + + +\section{Timing considerations} + +{\ldots \it \bf HAS TO BE UPDATED AND COMPLETED!! \ldots \\} +{\it Here, all possible models should go in with reasonning why certain time +or flux estimates are proposed.  We have now only estimates on extrapolations +of the \eg power-laws. Maybe we should include: IC (in many possible combinations), +hadronic emission models (see~\cite{TASC}), Cannonball model. } +\par + +The EGRET~\cite{EGRET} instrument on the CGRO +has detected GeV emission of GRB940217 promptly and 90 sec. after +the burst onset. +\\ +\par +In~\cite{DERMER}, two peaks in the GeV light curve are calculated. An early maximum coincident +with the MeV eak is the high-eneryg extension of the synchrotron component, some seconds +after the burst onset. The second maximum peaking at $\approx$ 1.5 hours is due primarily to +SSC radiation with significant emission of up to $10^5$ sec. ($\approx 25$ hours) after the burst. +\\ +\par +Li, Dai and Lu~\cite{LI} suggest GeV emission after pion production and some thermalization of the +UHE component with radiation maxima of up to one day or even one week (accompanied by long-term +neutrino emission). + +\subsection{Determine a reasonable upper time delay limit for the onset of an observation} +{\ldots \it \bf STILL TO BE WRITTEN \ldots \\} + + +\subsection{Determine a reasonable upper limit on the observation duration} + +{\ldots \it \bf STILL TO BE WRITTEN \ldots \\} +\subsection{Determine a reasonable zenith angle range for observation} +{\ldots \it \bf STILL TO BE WRITTEN \ldots \\} + +\section{Maximizing the duty cycle} + +{\ldots \it \bf STILL TO BE WRITTEN \ldots \\} + +\begin{verbatim} +email Nicola Galante: \\ +\\ +I calculated duty-cycle with a Sun zenith angle greater +than 105 deg, which means that Sun must be at least 15 deg below +horizon, and not with an angle of 115 deg. I tried this calculation also +with a limit of 108 deg, because a lot of people assume that the +astronomical sunset is when the Sun is 18 deg below horizon. Using this +assumption the calculated duty-cycle decreases of about 4\%(from 1.225 to +1.18 srad per year or from 9.75\% to 9.36\% vs 4pi srad per year). Anyway +the definition of astronomical sunset influence the main cut on duty-cycle. +About wind I can say that the data I used were provided by NOT, which is +situated in a place more windy than where MAGIC is growing up. I made +the calculation also with other upper limits to wind's speed then the +usual 10 m/s, and we can gain quite a lot of duty-cycle (even about +1.5\%more vs 4pi srad per year) so it should be interesting to test the +telescope during some windy or foggy days. +\end{verbatim} + +\subsection{Taking OFF data} + +{\ldots \it \bf STILL TO BE WRITTEN \ldots \\} + +\subsection{Observing neutrino events below the horizon} + +{\ldots \it \bf CAN BE MAYBE GO INTO A SEPARATE PROPOSAL \ldots \\} + +\subsection{Observing XRFs} + +{\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 \\} + +\section{Calibration and Tests} + +{\ldots \it \bf STILL TO BE WRITTEN \ldots \\} + +%%% BIBLIOGRAPHY %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% + +%%>>>> Use the following if you are using BibTeX for bibliography +%\theBibliography + +%%>>>> 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 +telescope for Gamma-Astronomy above 10~GeV, March 1998, Version 5 +\bibitem{PETRY} The MAGIC Telescope - Prospects for GRB research +D. Petry for the MAGIC collaboration, Astron. Astrophys. Suppl. Ser. 138, 601, 1999. +\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 +\bibitem{PAZCYNSKI} Pazcy\'{n}ski B., Astrophys. J. 308 L43 (1986) +\bibitem{GOODMAN} Goodman J., Astrophys. J. 308 L47 (1986) +\bibitem{SARI} Sari R., Piran T., Narayan R., Astrophys. J. 497 L17 (1998) +\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, +The Gamma Ray Universe, Les Arcs 9-16 March 2002. +\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} +(see also: http://space.mit.edu/HETE/mission\_status.htm \\ + http://space.mit.edu/HETE/ban.html ) +\bibitem{HETE-SUM} HETE Trigger Summaries +http://space.mit.edu/HETE/Bursts/summaries.html +\bibitem{SWIFT} The SWIFT homepage +http://swift.gsfc.nasa.gov/science/ +\bibitem{SWIFT2} +http://swiftsc.gsfc.nasa.gov/docs/swift/swiftsc.html +\end{thebibliography} + +\end{document} +% +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +%%% Upper-case A B C D E F G H I J K L M N O P Q R S T U V W X Y Z +%%% Lower-case a b c d e f g h i j k l m n o p q r s t u v w x y z +%%% Digits 0 1 2 3 4 5 6 7 8 9 +%%% Exclamation ! 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