5 research outputs found
Cosmic ray effect on the X-ray Trigger Telescope of UFFO/Lomonosov using YSO scintillation crystal array in space
BDRG and shok instruments for study of GRB prompt emission in michaylo lomonosov space mission
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) (13.0Â Ă—Â 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
Space experiments on-board of lomonosov mission to study gamma-ray bursts and UHECRS
The number of experiments on-board Lomonosov spacecraft are preparing now at SINP MSU in
co-operation with other organisations. The main idea of Lomonosov mission is to study
extreme astrophysical phenomena, such as cosmic gamma-ray bursts and ultra-high energy
cosmic rays. These phenomena connect with processes occurred in very distant astrophysical
objects of the Early Universe and give us information about first stages of Universe
evolution. Thus, the Lomonosov mission scientific equipment includes several instruments
for gamma-ray burst observation in optics, ultra-violet, X-rays and gamma-rays and the
wide aperture telescope for ultra-high energy particle study by detection of ionisation
light along its tracks in the atmosphere. The main parameters and a brief description of
these instruments are presented