SVOM: A new mission for Gamma-ray burst studies

AIP Conference Proceedings 06/2009; 1133. DOI: 10.1063/1.3155898
Source: arXiv

ABSTRACT We present the SVOM (Space-based multi-band astronomical Variable Object Monitor) mission, that is being developed in cooperation between the Chinese National Space Agency (CNSA), the Chinese Academy of Science (CAS) and the French Space Agency (CNES). Its scientific objectives include the study of the GRB phenomenon, GRB physics and progenitors, cosmology, and fundamental physics. SVOM is designed to detect all known types of Gamma-Ray Bursts (GRBs), to provide fast and reliable GRB positions, to measure the broadband spectral characteristics and temporal properties of the GRB prompt emission. This will be obtained in first place thanks to a set of four space flown instruments. A wide field (~2 sr) coded mask telescope (ECLAIRs), operating in the 4-250 keV energy range, will provide the triggers and localizations, while a gamma-ray non-imaging spectrometer (GRM), sensitive in the 50 keV-5 MeV domain, will extend the prompt emission energy coverage. After a satellite slew, in order to place the GRB direction within field of view of the two narrow field instruments - a soft X-ray (XIAO), and a visible telescope (VT) - the GRB position will be refined and the study of the early phases of the GRB afterglow will be possible. A set of three ground based dedicated instruments, two robotic telescopes (GFTs) and a wide angle optical monitor (GWAC), will complement the space borne instruments. Thanks to the low energy trigger threshold (~4 keV) of the ECLAIRs, SVOM is ideally suited for the detection of soft, hence potentially most distant, GRBs. Its observing strategy is optimized to facilitate follow-up observations from the largest ground based facilities. Comment: Proceedings of the 6th Huntsville Symposium on Gamma-Ray Bursts (October 20-23 2008). Figures in colour with respect to the published version

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Available from: P. Mandrou, Sep 29, 2015
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    • "Rapid follow-up of GRB afterglows in the next decade is predicated on the assumption that there will be a replacement for Swift and Fermi which will be capable of detecting the gamma ray prompt emission and providing alerts. Currently the most promising successor is the joint French-Chinese mission SVOM (Götz et al, 2009). SVOM's scientific payload consists of the ECLAIRs 2D coded mask imager for the detection and localisation of gamma ray transients, and like Swift, optical and X-ray instruments for afterglow follow-up. "
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    Experimental Astronomy 10/2014; 39(1). DOI:10.1007/s10686-015-9447-0 · 1.99 Impact Factor
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    Monthly Notices of the Royal Astronomical Society 12/2009; 406(3). DOI:10.1111/j.1365-2966.2010.16787.x · 5.11 Impact Factor
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    ABSTRACT: Since the launch of Swift satellite, the detections of high-z (z>4) long gamma-ray bursts (LGRBs) have been rapidly growing, even approaching the very early Universe (the record holder currently is z=8.3). The observed high-z LGRB rate shows significant excess over that estimated from the star formation history. We investigate what may be responsible for this high productivity of GRBs at high-z through Monte Carlo simulations, with effective Swif/BAT trigger and redshift detection probabilities based on current Swift/BAT sample and CGRO/BATSE LGRB sample. We compare our simulations to the Swift observations via log N-log P, peak luminosity (L) and redshift distributions. In the case that LGRB rate is purely proportional to the star formation rate (SFR), our simulations poorly reproduce the LGRB rate at z>4, although the simulated log N-log P distribution is in good agreement with the observed one. Assuming that the excess of high-z GRB rate is due to the cosmic metallicity evolution or unknown LGRB rate increase parameterized as (1+z)^delta, we find that although the two scenarios alone can improve the consistency between our simulations and observations, incorporation of them gives much better consistency. We get 0.2<epsilon<0.6 and delta<0.6, where epsilon is the metallicity threshold for the production of LGRBs. The best consistency is obtained with a parameter set (epsilon, delta)=(~0.4, ~0.4), and BAT might trigger a few LGRBs at z~14. With increasing detections of GRBs at z>4 (~15% of GRBs in current Swift LGRB sample based on our simulations), a window for very early Universe is opening by Swift and up-coming SVOM missions. Comment: 9 pages, including 8 figures and 1 table, one more figure added. Accepted for publication in MNRAS
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