Abstract
This paper presents a catalogue of gamma-ray bursts (GRBs) that were detected by the instruments onboard the Lomonosov space observatory. The Lomonosov mission gave the first experience of not only multi-wavelength (from optical to gamma) observations of GRBs but also multi-messenger observations of extreme phenomena and GRBs. The detailed light curves and energy spectra of the detected GRBs are presented. The results of the prompt, early an afterglow optical observations of several GRBs are discussed.
Highlights
One of the most important and interesting branches of modern physics and astrophysics is the study of extreme processes and phenomena that lead to the most powerful explosions and acceleration of particles to the maximum possible energies. Such phenomena include ultra-high-energy cosmic rays (UHECR) and cosmic gamma-ray bursts (GRBs hereafter), i.e., long-term phenomena that are associated with the collapse of massive stars and short-term, transient phenomena that are due to the merging of relativistic compact objects, which leads to gravitational wave generation
A MASTER robot located near Blagoveshchensk automatically pointed there and discovered that an optical transient [64] appeared at ~70 s from the Swift trigger that was produced at the front of the first peak of the light curve i.e., about 30 s before the BDRG/Lomonosov GRB trigger
The scientific payload on the Lomonosov spacecraft was directly connected to the Internet for the first time in the practice of Russian space instrumentation, and through it, the output data flew into the international gamma-ray burst registration network Gamma-ray Coordinates Network (GCN)
Summary
One of the most important and interesting branches of modern physics and astrophysics is the study of extreme processes and phenomena that lead to the most powerful explosions and acceleration of particles to the maximum possible energies. In the experiments of Fermi/GBM, Swift/BAT and some others, a fast automatic transfer of a message with the coordinates of a gamma-ray burst from space instruments to ground-based telescopes was realised [29] In this case, the possibility of multi-wavelength observations is determined by the speed of pointing the ground telescope to the source. The estimation of GRB positions takes place after the BDRG trigger, and the trigger data, together with the calculated coordinates of the source, are transferred to the Ultrafast Flash Observatory [23] on board the Lomonosov spacecraft and to a ground server via the Global Star transmitter and to several telescopes through the Gamma-ray Coordinates Network (GCN). Computer simulations showed that the accuracy of GRB localisation is up to 2◦ for bright bursts with the fluence of ≥10−5 erg cm−2 measured on the equator and ~5◦ for GRBs with a fluence of ≥10−7 erg cm−2
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