EAS Publications Series
Volume 61, 2013Gamma-ray Bursts: 15 Years of GRB Afterglows – Progenitors, Environments and Host Galaxies from the Nearby to the Early Universe
|Page(s)||553 - 559|
|Section||Chapter XI: Instrumentation & Techniques-II (Lomonosov/UFFO)|
|Published online||22 July 2013|
A.J. Castro-Tirado, J.Gorosabel and I.H. Park (eds)
EAS Publications Series, 61 (2013) 553-559
BDRG and shok instruments for study of GRB prompt emission in michaylo lomonosov space mission
1 D.V. Skobeltsyn Institute of Nuclear
Physics of M.V. Lomonosov Moscow State University, Leninskie Gory, 1/2, 119991
2 P.K. Shternberg Astronomical Institute of M.V. Lomonosov Moscow State University, Universitetskii prosp. 17, 119992 Moscow, Russia
3 Berkeley Center for Cosmological Physics, Berkeley, California, USA
The study of GRB prompt emission (PE) is one of the main goals of the Lomonosov space mission, which is being prepared at Moscow State University. The GRB monitor (BDRG) and the wide-field optical cameras (SHOK) are intended for detection of GRB prompt emission as well as optical counterparts. The BDRG instrument consists of three identical NaI(Tl)/CsI(Tl) (13.0 × 2.0cm ) phoswich detectors, whose axes determine the Cartesian coordinate system. This allows to localize any GRB source on the sky by means of the count rate seen by each detector with an accuracy of ~2 deg. The SHOK instrument consists of two identical wide-field cameras (WFC) directed in such a way that the field of view (FOV) of each WFC overlaps by the corresponding BDRG FOV, which produces a trigger on the WFC in case of a GRB detection. With this setup, the GRB prompt light curve will be obtained in the visible without any delay with respect to gamma-rays, which is crucial for a GRB central engine understanding.
© EAS, EDP Sciences 2013
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