The light emitted by the celestial body producing gravitational wave is called gravitational wave electromagnetic counterpart, which is the key to understand the explosion process of gravitational wave celestial body and study the basic physical laws of the universe. The detection and research of gravitational wave gamma ray bursts (i.e., high-energy electromagnetic counterpart of gravitational wave) will be an important milestone in the era of gravitational wave astronomy, which contains huge space for discovery and will produce rich original research results.

The high-energy electromagnetic counterpart of gravitational wave has the characteristics of random occurrence, low event rate (several / year, extremely valuable observation opportunity), and short duration (short storm < 2S). The existing space high-energy telescopes have insufficient field of view coverage for the whole day, which makes it easy to miss the very valuable gravitational wave gamma storm events; the positioning error is large (more than tens of square degrees), so it is difficult to identify the homology of gravitational waves merging with double compact stars; the sensitivity is insufficient to detect the potential high-energy radiation with low current intensity or soft energy spectrum, and the comprehensive detection performance cannot meet the detection requirements.

Based on the importance and scarcity of gravitational wave gamma bursts and the lack of telescope detection capability, the Chinese Academy of Sciences has set up and implemented the gecam project dedicated to the discovery of gravitational wave gamma storms

1. The high-energy electromagnetic correspondents of gravitational wave events are monitored throughout the day, and the largest sample of gravitational wave gamma bursts and new radiation phenomena are found. The dense celestial bodies such as neutron stars and black holes and their merging processes are studied;

2. The possible high-energy radiation of the fast radio storm is monitored all day to reveal its physical origin and radiation mechanism;

3. All kinds of special GRBs and magstar bursts are monitored all the time, and their burst mechanisms are studied in depth.

Special GRBs: full time and all day monitoring of very long bursts, monitoring of low-energy X-ray flashes and X-ray rich bursts, and studying their precursors and physical mechanisms. It is expected that the detection rate of GRBs is about 500 / year.

Magnetostar burst: full time and all day monitoring, discovery of new magnetostar in low energy region, monitoring three complete magnetostar burst cycles every year, studying the radiation properties and explosion mechanism of magnetostar, and studying the structure of magnetostar through QPO.

4. Other scientific objectives

Monitoring hundreds of X-ray / gamma ray sources

Monitoring of solar flare (SFL) wide band radiation

The earth gamma ray flash (TGF) and earth electron beam (TEB) were monitored.