Pos(Integral08)009

PoS(Integral08)009

http://pos.sissa.it ts by other instruments in the IPN. It has also IPN. in the by other instruments ts or two extragalactic giant magnetar flares. magnetar giant extragalactic or two eative Commons Attribution-NonCommercial-ShareAlike Licence. Licence. Commons Attribution-NonCommercial-ShareAlike eative

312, Garching, 85748 Germany 312, Garching, 85748 Germany

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1 Speaker Speaker 1 Copyright ownedCopyright by the author(s) under the terms of the Cr

Max-Planck-Institut für extraterrestrische Physik 1 Giessenbachstrasse Postfach [email protected] E-mail: the below bursts weak certainly almost are which but unconfirmed, are which events 130 over observed include which observations, these of highlights the We review experiments. IPN other the of thresholds one and repeaters, gamma soft bursts, gamma-ray Giselher Lichti Max-Planck-Institut für extraterrestrische Physik 1 Giessenbachstrasse Postfach Andreas von Kienlin the of component essential an been has spectrometer INTEGRAL of the system The anticoincidence as confirmed been have which events 600 about observed has It launch. since network interplanetary gamma ray burs or cosmic gamma repeaters either soft E-mail: [email protected] Arne Rau California Institute of Technology 1200 California Blvd., MS 105-24, Pasadena,91125U.S.A. CA, [email protected] E-mail: [email protected] E-mail: Kevin Hurley ofUniversity CaliforniaSpace Sciences Laboratory Berkeley, 7 Gauss Way, Six Years of Bursts with the SPI-ACS of Bursts with the SPI-ACS Six Years

PoS(Integral08)009 . The SPI- . The 2 Speaker Name Name Speaker tti et al. 2005), and

use they are below the thresholds of the osed as a gamma-ray burst (GRB) detector d byd in the at least one other experiment es, has a maximum effective es, has a area of up to maximum have been detected from the ‘new’ magnetar the ‘new’ magnetar been detected from have rticles. Others, however, are almost certainly so far. The SPI ACS has detected about 45

a single energy which ranges from ~100 channel onfirmed event is GRB071112, with a fluence of with a fluence event is GRB071112, onfirmed 2 on-axis. When triggered, it produces 105 s long on-axis. When triggered, 2 s have been relativelyweak. , and the Fermi Burst Monitor has ~200 cm Burst Monitor the Fermi , and 2 . Its time history is shown in figure 1. The total trigger rate is extremely trigger rate 1. The total . Its time history shown in figure is -2 erg cm at 100 keV, and a thickness of 1.6 to 5 cm. For comparison, a BATSE module had module For comparison, a BATSE to 5 cm. of 1.6 and a thickness keV, at 100 , the Swift BAT has 5240 cm has 5240 Swift BAT , the

2 2 -8 Figure 1. The weakest confirmed cosmic event observed by SPI-ACS. This burst, which resembles many of the weak unconfirmed events, was also detected by Swift. The SPI-ACS has now detected about 550 confirmed cosmic gamma-ray confirmed 550 bursts (1 everyThe SPI-ACS has now detected about cosmic 3 The SPI anticoincidence system was first system prop The SPI anticoincidence 5250 cm 5250 at the 2nd INTEGRAL workshop in St. Malo in 1996 (Hurley 1997). Its BGO shield, which shield, which Its BGO 1997). (Hurley 1996 Malo in INTEGRAL workshop St. at the 2nd in sid and bottom on the spectrometer surrounds the weak gamma-ray bursts which are unconfirmed beca weak gamma-ray which are unconfirmed bursts events No SGR1900+14. from burst one short variable, ranging from one to several hundred triggers per day. of these are one to several Some hundred triggers randomvariable, ranging from fluctuations, while others are due to noise or pa other IPN experiments; 135other IPN experiments; have been detected tar SGR1806-20 (Mereghe the flare from magne one giant short bursts and because the burst SGR0501+4516, probably ACS has a superior response above 100 keV. Its effective area is a function of azimuthal and of azimuthal is a function area keV. Its effective above 100 response ACS has a superior cm drops to about 500 zenithal angles, and Introduction 1.Introduction Short title 4000 cm 4000 days);are events whichthese been observe have GRB time histories with 50 ms resolution in not record energyMeV. It does GRB keV to 10 spectra, nor does it have an independent localization capability. 2. The Score So Far weakest c interplanetary network (IPN). The 10 4.8 x PoS(Integral08)009 , this -2 Speaker Name Name Speaker erg cm -4

dvantage of the excellent statistics and low is evident, which can be fit with a s the later part of the light curve after utrino emission, and very high gamma-ray gamma-ray high very and emission, utrino the ACS. The statistics are excellent: up to rongest bursts, when they are observed with

3 detailed light curve studies which take a detailed light curve high energy sensitivity of the ACS, high energy sensitivity of the Obtaining precise localizations with the burst and searching IPN, for electromagnetic and counterparts, ne radiation, gravitational Searching for emission from bursts, more or less independently of the rapidityand accuracy of the localizations.

Figure 2. The main figure shows the light curve of GRB021206, with the background with the background GRB021206, of curve figure shows the light The main Figure 2. indicated by a dashed line. The inset show background subtraction. A gamma-ray subtraction. background afterg power law of index ~-1.1. power law of index ~-1.1. data falls into three broad categories: SPI-ACS data falls into three The science can be done with the which 1. of 1.6 x 10 a fluence With of GRB021206. the light curve Figure 2 shows 2. 3. We discuss each these in turn. of is one of the most intense events observed by is one of the most are recorded in a single 50 ms time bin. A gamma-ray counts 60,000 is evident in afterglow this these are onlylight curve; detected in the st excellent statistics. Short title 3. Science With The SPI-ACS Data With The SPI-ACS 3. Science 3.1 Light Curve Studies PoS(Integral08)009

Speaker Name Name Speaker DOI: 10.1086/430669 DOI: 10.1086/430669

er), and the Swift BAT, all in low Earth its way to Mercury, and Mars Odyssey, in lines. The configuration of the network is The SPI-ACS light curve of the SGR1806-20 The SPI-ACS light curve of the SGR1806-20 network currently.) Konus-Wind is at about 5 5 about Konus-Wind is at network currently.)

4 Interplanetary Network. rd

Figure 3. From Mereghetti et al. 2005. Figure 3. From Mereghetti et al. The flare itself isgiant flare with evident 50 s binning. starting around 0 seconds. The for about s, and continues 500 peaks around end of the flare, afterglow starts around the of the AAS. permission Reproduced by one hour. Gamma-ray have been observed intense GRBs following afterglows by instruments other The SPI-ACS is one of nine instruments in the IPN. The others are RHESSI, the Suzaku

the outflow from an expanding provide evidence for on giant flares Since radio data Short title prior to GRB021206. However, the observation by the SPI-ACS of a gamma-ray of a the SPI-ACS afterglow by the observation However, GRB021206. prior to phenomenon, This unexpected. was completely SGR1806-20 giant flare from the following which was confirmed extended about one hour, and its spectrum and Konus, lasted by RHESSI in figure 3. The light curve is shown to at least 1 MeV. orbit around Mars, provide the interplanetaryorbit around base WAM, AGILE (Super-AGILE and the mini-calorimet orbit. (The Fermi GBM is being added to the Fermi orbit. (The Earth.light-seconds from Finally, MESSENGER, on 4. shown in figure 3.2 SPI-ACS in the 3 magnetar, the afterglow be related to it. may PoS(Integral08)009

. Because -2 Speaker Name Name Speaker position in the network: it is far enough of view that are unocculted byplanetary of view that d it is in continuous operation, when the duty is in continuous operation, d it vertex for GRB localization. About 200 bursts bursts 200 About for GRB localization. vertex l, they are not the same ones that narrow-field

5 of the Interplanetary Network. , and/or peak fluxes above 0.4 photon cm photon 0.4 above peak fluxes , and/or -2 erg cm -6

Figure 4. The present configuration Figure 4. The present configuration Two interesting events which were detected by are burstsACS on November 3 2005 the The INTEGRAL spacecraft occupies The INTEGRAL spacecraft occupies a unique per year are detected by the IPN, and in genera instruments such as IBIS and the Swift observe. BAT They are the intense events, more with fluences greaterthan 10 from Earth to provide a statistically Earth to provide independent from and February 1 2007. Their light curves are shown in figure 5. are light curves Their 1 2007. and February INTEGRAL, Wind, and MESSENGER have fields INTEGRAL, Wind, and cycles of all its instruments are considered. bodies, the IPN constitutes an all-sky monitor, an constitutes an all-skybodies, the IPN monitor, Short title PoS(Integral08)009

erg,

45 Speaker Name Name Speaker and 1.5 x 10 46 n in figure 6. Because their of overlaps ew a large fraction of the sky, and record e alone is often sufficient to search for more no radiation, and very high energy gamma-ray gamma-ray energy very high and radiation, no 81 and M31 respectively (Frederiks et al. 2007,81 and M31 respectively (Frederiks RB localizations whether to determine an event

es and energy spectra, these bursts are quite likely 6

Figure 5. The SPI-ACS light curves of the November 3 2005 (left) and February 1 2007 February and 1 2007 3 2005 (left) November the SPI-ACS light curves of Figure 5. The (right) events. Figure 6. IPN error boxes for the November 3 2005 (left) and February 1 2007 (right) (right) 1 2007 (left) and February 3 2005 error boxes for the November Figure 6. IPN the overlap but they the left figure, in not visible of M81 are outer contours bursts. The IPN error box. The IPN localizations of these events are show All-skyand experiments which vi experiments,

Mazets et gamma-rayal. their isotropic 2008). If so, energies were 7 x 10 with bright galaxies, as well as their light curv to be extragalactic giant magnetar flares from M Short title respectively. their data, often do not require fast or precise require fast or precise their data, often do not G can be correlated with a GRB. The trigger tim neutri and as gravitational exotic radiation, such 3.3 Searches for Exotic Counterparts PoS(Integral08)009 , in , in Speaker Name Name Speaker , Ap.681, J. On Possibility the of Golenetskii, K. Hurley, A. von K. Hurley, A. Golenetskii, r of fast gamma-ray transients in the al. (2007). So far, they are all upper limits, far, they So all upper limits, are (2007). al. rmined; the redshifts lie in the range 0.105 to range 0.105 to rmined; the redshifts lie in the G. Lichti, G. Weidenspointner, G., and P. Jean, and/or X-ray counterparts, and for 38 events, a X-ray and for 38 events, and/or counterparts,

7 and ssl.berkeley.edu/ipn3/index.html, respectively. Golenetskii, T. Cline, and E. Mazets, Cline, and Golenetskii, T. been issued starting around October 2008. About 90 of the 90 October 2008. About been issued starting around D. Frederiks, J. Goldsten, S. J. Goldsten, D. Frederiks, and above. Using these data, over 175 GCN Circulars have data, over 175 GCN Circulars Using these and above. -2 , Ap. J. 624, L105, 2005 , Astron. 19, 2007 , Astron. Lett. 33(1), A Giant Flare from a Soft Gamma Repeater in the Andromeda Galaxy Galaxy Andromeda in the Repeater Gamma a Soft Flare from A Giant , Ap.2008357, J. 674, The Search for Muon Neutrinos from Northern Hemisphere Gamma-Ray Gamma-Ray Hemisphere Northern from Neutrinos Muon for Search The erg cm -8 ImplicationsObservations070201OriginfromLIGO of GRB for the Milagro Constraints on Very High Energy Emission from Short-Duration Gamma- Short-Duration from Emission Energy High Very on Constraints Milagro , Ap. J. 666, 361, 2007 INTEGRAL as a Gamma-Ray Burst Detector in the Fourth Interplanetary Network Interplanetary Fourth the in Detector Burst as a Gamma-Ray INTEGRAL , Ap. J. 680, 545, 2008 2008 545, 680, J. , Ap.

SPI-ACS is a sensitive monito The INTEGRAL

Guest Observer the U.S. INTEGRAL under support Acknowledgment. KH is grateful for K. Hurley, The Transparent Universe, Proc.2nd INTEGRALWorkshop, Eds. C.Winkler, T. Courvoisier, and Ph. Durouchoux,491,ESA SP 382, p. 1997 S. Mereghetti, D. Gotz, A. von Kienlin, von A. A. Rau, Gotz,S. Mereghetti, D. The First Giant Flare from SGR1806-20: Observations Using the Anticoincidence Shield of the the of Shield Anticoincidence the Using Observations SGR1806-20: from Flare Giant First The INTEGRAL on Spectrometer D. Frederiks, V. Palshin, R. Aptekar, S. V. Palshin, D. Frederiks, IdentifyingShortHard the Burst GRB051103 Gianta withFlare from a Soft Gamma Repeater in of Galaxies Group the M81 E. Mazets, R. Aptekar, T. Cline, Aptekar, E. Mazets, R. et al., A., Achterberg Bursts with AMANDA B. Abbott et al., Kienlin, and V. Palshin, Palshin, V. and Kienlin, (M31) 1419, 2008 Ray Bursts A. Abdo et al., A.

[1] [2] [3] [4] [6] [5] [7] References References fluence range 4.8 x 10 x fluence range 4.8 Short title LIGO, AMANDA,emission. this category.are in Sky, Pi of the These and Milagro nearby), (and presumably of bright a large number from having benefit experiments isotropicallyto study.distributed GRBs Some results of these studies appeared in Abbott have Abdo et et al. (2008), and Achterberg et al. (2008), 4. Summary but the Abbott et al. LIGO result is particularly interesting, since it demonstrates that al. LIGO result is particularlybut the Abbott et it demonstrates interesting, since the merger in M31. been caused by a binary have could not event 070201 program, NASA grant NNX08AC90G. program, been issued, and GCN Notices have been issued, optical, bursts detected by the ACS have radio, been dete redshift has spectroscopic or photometric available at publicly the IPN data, are as well as made curve data, ACS light the Both 3.35. ftp://isdcarc.unige.ch/arc/FTP/ibas/spiacs/