Abstract
On behalf of the ARGO-YBJ Collaboration Abstract. We report on the search for Gamma Ray Bursts (GRBs) in the energy range 1 100 GeV in coincidence with the prompt emission detected by satellites, using the Astro- physical Radiation Ground-based Observatory at YangBa- Jing (ARGO-YBJ). With its big active surface ( 6700 m 2 ) and large field of view ( 2 sr) the ARGO-YBJ air shower detector is particularly suitable to detect unpredictable and short duration events such as GRBs. The search has been performed using the single particle technique in time coinci- dence with satellite detections both for single events and for the piling up of all the GRBs in time and in phase. Between November 2004 and June 2010 115 GRBs, de- tected by different satellites (mainly Swift and Fermi), oc- curred within the field of view of ARGO-YBJ. For 94 of these we searched for a counterpart in the ARGO-YBJ data finding no statistically significant emission. Search methods and results are discussed.
Highlights
The study of Gamma Ray Bursts (GRBs) has been carried out mainly from space detecting the primary photons
The search can be performed by means of large area extensive air shower detectors operating at high altitude, measuring the secondary particles generated by the interaction of the primary photons with the Correspondence to: C
A total of 115 GRBs, selected from the GCN Circulars Archive1, was inside the ARGO-YBJ field of view; for 94 of these gamma ray bursts ARGO-YBJ data were available and they have been investigated by searching for a significant excess in the counting rates coincident with the satellite detection
Summary
The ARGO-YBJ experiment is located at 4300 m a.s.l. (vertical atmospheric depth 606 g cm2) at the YangBaJing Cosmic Ray Laboratory (30◦06 38 N 90◦31 56 E, Tibet, P.R. of China). The detector is composed of a single layer of Resistive Plate Chambers (RPCs) operated in streamer mode (Aielli et al, 2006) and grouped in 153 units, called clusters, of area 5.7×7.6 m2 each. In shower mode the arrival time and location of each particle are recorded using the pads allowing the detailed reconstrunction of the shower lateral distribution and the arrival direction. The corresponding measured rates are 40 kHz, 2 kHz, 300 Hz and 120 Hz, respectively This latter technique does not provide information about the energy and arrival direction of the primary cosmic ray, it allows a very low energy threshold of 1 GeV overlapping the highest energy region directly investigated by satellite experiments. Details of this study are widely discussed in Aielli et al (2008), together with the determination of the effective area, upper limit calculation and expected sensitivity
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