The SVOM mission

2021 ◽  
Author(s):  
J.-L. Atteia ◽  
B. Cordier ◽  
J. Wei
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Space Mission ◽  
Gamma Ray Bursts ◽  
Wide Field ◽  
X Ray ◽  
Ground Segment ◽  
Optical Wavelengths ◽  
Scientific Rationale

The Sino-French space mission SVOM is mainly designed to detect, localize and follow-up Gamma-Ray Bursts and other high-energy transients. The satellite, to be launched mid 2023, embarks two wide-field gamma-ray instruments and two narrow-field telescopes operating at X-ray and optical wavelengths. It is complemented by a dedicated ground segment encompassing a set of wide-field optical cameras and two 1-m class follow-up telescopes. In this contribution, we describe the main characteristics of the mission and discuss its scientific rationale and some original GRB studies that it will enable.

scholarly journals Can we quickly flag ultra-long gamma-ray bursts?

2019 ◽  
Vol 486 (2) ◽  
pp. 2471-2476 ◽  
Author(s):  
B Gendre ◽  
Q T Joyce ◽  
N B Orange ◽  
G Stratta ◽  
J L Atteia ◽  
...  
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
Wide Field ◽  
Exact Nature ◽  
X Ray ◽  
Central Engine ◽  
Long Duration ◽  
Limited Coverage

Abstract Ultra-long gamma-ray bursts are a class of high-energy transients lasting several hours. Their exact nature is still elusive, and several models have been proposed to explain them. Because of the limited coverage of wide-field gamma-ray detectors, the study of their prompt phase with sensitive narrow-field X-ray instruments could help in understanding the origin of ultra-long GRBs. However, the observers face a true problem in rapidly activating follow-up observations, due to the challenging identification of an ultra-long GRB before the end of the prompt phase. We present here a comparison of the prompt properties available after a few tens of minutes of a sample of ultra-long GRBs and normal long GRBs, looking for prior indicators of the long duration. We find that there is no such clear prior indicator of the duration of the burst. We also found that statistically, a burst lasting at least 10 and 20 minutes has respectively $28{{\ \rm per\ cent}}$ and $50{{\ \rm per\ cent}}$ probability to be an ultralong event. These findings point towards a common central engine for normal long and ultra-long GRBs, with the collapsar model privileged.

scholarly journals Imaging in Hard X-ray Astronomy

2003 ◽  
Vol 214 ◽  
pp. 70-83 ◽  
Author(s):  
T. P. Li
Keyword(s):  
Gamma Ray ◽  
Signal To Noise Ratio ◽  
High Energy ◽  
High Signal ◽  
Wide Field ◽  
X Rays ◽  
X Ray ◽  
Energy Gamma ◽  
High Resolution Images ◽  
Energy Processes

The energy range of hard X-rays is a key waveband to the study of high energy processes in celestial objects, but still remains poorly explored. In contrast to direct imaging methods used in the low energy X-ray and high energy gamma-ray bands, currently imaging in the hard X-ray band is mainly achieved through various modulation techniques. A new inversion technique, the direct demodulation method, has been developed since early 90s. with this technique, wide field and high resolution images can be derived from scanning data of a simple collimated detector. The feasibility of this technique has been confirmed by experiment, balloon-borne observation and analyzing simulated and real astronomical data. Based the development of methodology and instrumentation, a high energy astrophysics mission – Hard X-ray Modulation Telescope (HXMT) has been proposed and selected in China for a four-year Phase-A study. The main scientific objectives are a full-sky hard X-ray (20–200 keV) imaging survey and high signal-to-noise ratio timing studies of high energy sources.

Wide field X-ray telescopes: Detecting X-ray transients/afterglows related to gamma ray bursts

1999 ◽  
Vol 69 (1-3) ◽  
pp. 716-719
Author(s):  
René Hudec ◽  
Ladislav Pina ◽  
Adolf Inneman ◽  
Paul Gorenstein ◽  
Tomáš Rezek
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Wide Field ◽  
X Ray

scholarly journals Studying stellar explosions with Athena

2015 ◽  
Vol 11 (A29B) ◽  
pp. 243-243
Author(s):  
P. O'Brien ◽  
P. Jonker
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
Spectral Energy ◽  
Intermediate Mass ◽  
Tidal Disruption ◽  
X Ray ◽  
Cosmic Vision ◽  
Esa Cosmic Vision ◽  
Supernova Explosions

AbstractAthena is the second large mission selected in the ESA Cosmic Vision plan. With its large collecting area, high spectral-energy resolution (X-IFU instrument) and impressive grasp (WFI instrument), Athena will truly revolutionise X-ray astronomy. The most prodigious sources of high-energy photons are often transitory in nature. Athena will provide the sensitivity and spectral resolution coupled with rapid response to enable the study of the dynamic sky. Potential sources include: distant Gamma-Ray Bursts to probe the reionisation epoch and find missing baryons in the cosmic web; tidal disruption events to reveal dormant supermassive and intermediate-mass black holes; and supernova explosions to understand progenitors and their environments. We illustrate Athenas capabilities and show how it will be able to constrain the nature of explosive transients including gas metallicity and dynamics.

Design, Build and Test of the VOEvent Network for the SVOM Chinese Ground Segment

2017 ◽  
Vol 14 (S339) ◽  
pp. 353-353
Author(s):  
M. Zhang ◽  
M. Huang ◽  
C. Wu
Keyword(s):  
Data Reduction ◽  
Gamma Ray ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
Collaborative Project ◽  
Transient Phenomena ◽  
Ground Segment ◽  
Design Build ◽  
Science Centre ◽  
Set Up

AbstractThe Space-based, multi-band, astronomical Variable Object Monitor (SVOM) is a collaborative project between China and France dedicated to the detection, localisation and study of about 60 Gamma Ray Bursts per year, and other high-energy transient phenomena. SVOM is planned to be launched in 2021, with a lifetime of 3–5 years. The poster described our construction and testing of a prototype to set up an interface between our data reduction sub-system, the global VOEvent network, and the French science centre.

scholarly journals GRB 171205A/SN 2017iuk: A local low-luminosity gamma-ray burst

2018 ◽  
Vol 619 ◽  
pp. A66 ◽  
Author(s):  
V. D’Elia ◽  
S. Campana ◽  
A. D’Aì ◽  
M. De Pasquale ◽  
S. W. K. Emery ◽  
...  
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Host Galaxy ◽  
Isotropic Energy ◽  
Optical Telescope ◽  
X Ray ◽  
Hydrogen Column Density ◽  
Peak Energy ◽  
First Time

Context. Gamma-ray bursts (GRBs) occurring in the local Universe constitute an interesting sub-class of the GRB family, since their luminosity is on average lower than that of their cosmological analogs. Attempts to understand in a global way this peculiar behaviour is still not possible, since the sample of low redshift GRBs is small, and the properties of individual objects are too different from each other. In addition, their closeness (and consequently high fluxes) make these sources ideal targets for extensive follow-up even with small telescopes, considering also that these GRBs are conclusively associated with supernova (SN) explosions. Aims. We aim to contribute to the study of local bursts by reporting the case of GRB 171205A. This source was discovered by Swift Burst Alert Telescope (BAT) on 2017, December 5 and soon associated with a low redshift host galaxy (z = 0.037), and an emerging SN (SN 2017iuk). Methods. We analyzed the full Swift dataset, comprising the UV-Optical Telescope (UVOT), X-ray Telescope (XRT) and BAT data. In addition, we employed the Konus-Wind high energy data as a valuable extension at γ-ray energies. Results. The photometric SN signature is clearly visible in the UVOT u, b and ν filters. The maximum emission is reached at ∼13 (rest frame) days, and the whole bump resembles that of SN 2006aj, but lower in magnitude and with a shift in time of +2 d. A prebump in the ν-band is also clearly visible, and this is the first time that such a feature is not observed achromatically in GRB–SNe. Its physical origin cannot be easily explained. The X-ray spectrum shows an intrinsic Hydrogen column density NH,int = 7.4+4.1−3.6 × 1020 cm−2, which is at the low end of the N H, int, even considering just low redshift GRBs. The spectrum also features a thermal component, which is quite common in GRBs associated with SNe, but whose origin is still a matter of debate. Finally, the isotropic energy in the γ-ray band, Eiso = 2.18+0.63−5.0 × 1049 erg, is lower than those of cosmological GRBs. Combining this value with the peak energy in the same band, Ep = 125+141−37 keV, implies that GRB 171205A is an outlier of the Amati relation, as are some other low redshift GRBs, and its emission mechanism should be different from that of canonical, farther away GRBs.

High Energy Transient Ionospheric Monitoring Network

1990 ◽  
Vol 8 (3) ◽  
pp. 263-265
Author(s):  
Paul J. Edwards
Keyword(s):  
Gravity Waves ◽  
Solar Flares ◽  
Gamma Ray ◽  
Monitoring Network ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
Ionospheric Perturbations ◽  
X Ray ◽  
Radio Receivers ◽  
Computer Based

AbstractContinuous, wide sky coverage is essential for the detection and monitoring of infrequent, short-lived events of astrophysical interest such as supernova and nova explosions, variable X-ray sources, gamma ray bursts, gravity waves and stellar and solar flares. We propose to (1) examine past radio propagation records and (2) develop new computer based radio receivers to monitor and log ionospheric perturbations associated with these events.

scholarly journals Abstracts

2011 ◽  
Vol 7 (S279) ◽  
pp. 433-446
Keyword(s):  
Gamma Ray ◽  
Cosmological Parameters ◽  
Supernova Explosion ◽  
Wide Band ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
Core Collapse ◽  
Host Galaxies ◽  
Unique Type ◽  
X Ray

Measuring cosmological parameters with GRBs: status and perspectivesNew interpretation of the Amati relationThe SED Machine - a dedicated transient spectrographPTF10iue - evidence for an internal engine in a unique Type Ic SNDirect evidence for the collapsar model of long gamma-ray burstsOn pair instability supernovae and gamma-ray burstsPan-STARRS1 observations of ultraluminous SNeThe influence of rotation on the critical neutrino luminosity in core-collapse supernovaeGeneral relativistic magnetospheres of slowly rotating and oscillating neutron starsHost galaxies of short GRBsGRB 100418A: a bridge between GRB-associated hypernovae and SNeTwo super-luminous SNe at z ~ 1.5 from the SNLSProspects for very-high-energy gamma-ray bursts with the Cherenkov Telescope ArrayThe dynamics and radiation of relativistic flows from massive starsThe search for light echoes from the supernova explosion of 1181 ADThe proto-magnetar model for gamma-ray burstsStellar black holes at the dawn of the universeMAXI J0158-744: the discovery of a supersoft X-ray transientWide-band spectra of magnetar burst emissionDust formation and evolution in envelope-stripped core-collapse supernovaeThe host galaxies of dark gamma-ray burstsKeck observations of 150 GRB host galaxiesSearch for properties of GRBs at large redshiftThe early emission from SNeSpectral properties of SN shock breakoutMAXI observation of GRBs and short X-ray transientsA three-dimensional view of SN 1987A using light echo spectroscopyX-ray study of the southern extension of the SNR Puppis AAll-sky survey of short X-ray transients by MAXI GSCDevelopment of the CALET gamma-ray burst monitor (CGBM)

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