The Deep and Transient Universe in the SVOM Era: New Challenges and Opportunities - Scientific prospects of the SVOM mission
J. Wei, B. Cordier, S. Antier, P. Antilogus, J.-L. Atteia, A. Bajat,, S. Basa, V. Beckmann, M.G. Bernardini, S. Boissier, L. Bouchet, V. Burwitz,, A. Claret, Z.-G. Dai, F. Daigne, J. Deng, D. Dornic, H. Feng, T. Foglizzo, H., Gao, N. Gehrels, O. Godet, A. Goldwurm, F. Gonzalez

TL;DR
The SVOM mission aims to advance gamma-ray burst research by combining space and ground observations, focusing on distant and faint GRBs, and providing rapid, multi-wavelength data to benefit the broader astronomy community.
Contribution
This paper presents the scientific objectives, instrument design, and potential impact of the SVOM mission for GRB studies and multi-wavelength astronomy.
Findings
SVOM will provide rapid GRB localization and spectral data.
The mission enhances understanding of distant and faint GRBs.
SVOM's multi-wavelength capabilities will benefit various astronomical research areas.
Abstract
To take advantage of the astrophysical potential of Gamma-Ray Bursts (GRBs), Chinese and French astrophysicists have engaged the SVOM mission (Space-based multi-band astronomical Variable Objects Monitor). Major advances in GRB studies resulting from the synergy between space and ground observations, the SVOM mission implements space and ground instrumentation. The scientific objectives of the mission put a special emphasis on two categories of GRBs: very distant GRBs at z5 which constitute exceptional cosmological probes, and faint/soft nearby GRBs which allow probing the nature of the progenitors and the physics at work in the explosion. These goals have a major impact on the design of the mission: the on-board hard X-ray imager is sensitive down to 4 keV and computes on line image and rate triggers, and the follow-up telescopes on the ground are sensitive in the NIR. At the…
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Taxonomy
TopicsGamma-ray bursts and supernovae · Stellar, planetary, and galactic studies · Astronomy and Astrophysical Research
