The SVOM gamma-ray burst mission

Cordier, B.; Wei, J. J.; Atteia, J. L.; Basa, S.; Claret, A.; Daigne, F.; Deng, J.; Dong, Yun; Godet, O.; Goldwurm, A.; Götz, D.; Han, X. H.; Klotz, A.; Lachaud, C.; Osborne, J.; Qiu, Y.; Schanne, S.; Wu, B. B.; Wang, J.; Wu, C. Y.; Xin, L. P.; Zhang, B.; Zhang, S.-N.

doi:10.48550/arxiv.1512.03323

Cited by 18 publications

(14 citation statements)

References 14 publications

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“…However, these missions have all exceeded their nominal mission lifetime. Future missions with triggering capabilities planned to be operating during the lifetime of Athena include the Space Variable Objects Monitor (SVOM; Cordier et al 2015) and the Wide Field Monitor (Hernanz et al 2018) on board the Enhanced X-ray Timing and Polarization mission (eXTP; Zhang et al 2016). A number of proposed missions are currently at concept level, such as the Transient High Energy Sky and Early Universe Surveyor (THESEUS; Amati et al 2018) and the All-Sky Medium Energy Gamma-ray Observatory (AMEGO; McEnery et al 2019), both capable of triggering and localising GRBs.…”

Section: Discussionmentioning

confidence: 99%

Detection capabilities of the Athena X-IFU for the warm-hot intergalactic medium using gamma-ray burst X-ray afterglows

Walsh,

McBreen,

Martin-Carrillo

et al. 2020

Preprint

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At low redshifts, the observed baryonic density falls far short of the total number of baryons predicted. Cosmological simulations suggest that these baryons reside in filamentary gas structures, known as the warm-hot intergalactic medium (WHIM). As a result of the high temperatures of these filaments, the matter is highly ionised such that it absorbs and emits far-UV and soft X-ray photons. Athena, the proposed European Space Agency X-ray observatory, aims to detect the 'missing' baryons in the WHIM up to redshifts of z = 1 through absorption in active galactic nuclei and gamma-ray burst afterglow spectra, allowing for the study of the evolution of these large-scale structures of the Universe. This work simulates WHIM filaments in the spectra of GRB X-ray afterglows with Athena using the SImulation of X-ray TElescopes (SIXTE) framework. We investigate the feasibility of their detection with the X-IFU instrument, through O vii (E = 573 eV) and O viii (E = 674 eV) absorption features, for a range of equivalent widths imprinted onto GRB afterglow spectra of observed starting fluxes ranging between 10 −12 and 10 −10 erg cm −2 s −1 , in the 0.3-10 keV energy band. The analyses of X-IFU spectra by blind line search show that Athena will be able to detect O vii-O viii absorption pairs with EW O vii > 0.13 eV and EW O viii > 0.09 eV for afterglows with F > 2 × 10 −11 erg cm −2 s −1 . This allows for the detection of ≈ 45-137 O vii-O viii absorbers during the four-year mission lifetime. The work shows that to obtain an O vii-O viii detection of high statistical significance, the local hydrogen column density should be limited at N H < 8 × 10 20 cm −2 .

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Section: Discussionmentioning

confidence: 99%

Detection capabilities of the Athena X-IFU for the warm-hot intergalactic medium using gamma-ray burst X-ray afterglows

Walsh,

McBreen,

Martin-Carrillo

et al. 2020

Preprint

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“…mission with comparable capabilities that flies over the next decade or longer (e.g., the Chinese-French satellite SVOM; Cordier et al 2015). Based on the current success rate of redshift determination with Swift, we assume that redshifts will be obtained for a fraction f z = 0.3 of detected SGRBs.…”

Section: Gw and Em Facilitiesmentioning

confidence: 99%

A Program for Multi-Messenger Standard Siren Cosmology in the Era of LIGO A+, Rubin Observatory, and Beyond

Chen,

Cowperthwaite,

Metzger

et al. 2020

Preprint

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The most promising variation of the standard siren technique combines gravitational-wave (GW) data for binary neutron star (BNS) mergers with redshift measurements enabled by their electromagnetic (EM) counterparts, to constrain cosmological parameters such as H 0 , Ω m , and w 0 . Here we evaluate the near-and long-term prospects of multi-messenger cosmology in the era of future GW observatories: Advanced LIGO Plus (A+, 2025), Voyager-like detectors (2030s), and Cosmic Explorer-like detectors (CE, 2035 and beyond). We show that the BNS horizon distance of ≈ 700 Mpc for A+ is well-matched to the sensitivity of the Vera C. Rubin Observatory (VRO) for kilonova detections. We find that one year of joint A+ and VRO observations will constrain the value of H 0 to percent-level precision, given a small investment of VRO time dedicated to targetof-opportunity GW follow-up. In the Voyager era, the BNS-kilonova observations begin to constrain Ω m with an investment of a few percent of VRO time. With the larger BNS horizon distance in the Cosmic Explorer era, on-axis short gamma-ray bursts (SGRBs) and their afterglows (though accompanying only some of the GW-detected mergers) supplant kilonovae as the most promising counterparts for redshift identification. We show that five years of joint observations with Cosmic Explorer-like facilities and a next-generation gammaray satellite with localization capabilities similar to that presently possible with Swift could constrain both Ω m and w 0 to 15 − 20%. We therefore advocate for a robust target-of-opportunity (ToO) program with VRO, and a wide-field gamma-ray satellite with improved sensitivity in the 2030s, to enable standard siren cosmology with next-generation gravitational wave facilities.

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“…The two wide-filed on-board instruments: the soft γ-ray imager ECLAIRs and the Gamma-Ray Monitor (GRM) are designed to observe GRB prompt emission in 4-150 keV and 15-5000 keV energy bands, respectively. With a field-of-view (FoV) of 2sr and a sensitivity of 7.2 × 10 −10 erg s −1 cm −1 (5σ detection level in 1000 s), a total of 60-70 GRBs per year can be triggered by ECLAIRs, and 4-5% of these GRBs are expected to have a redshift 5 (Godet et al 2014b;Cordier et al 2015).…”

Section: Profile and Instruments Of Svommentioning

confidence: 99%

A Pilot Study of Catching High-$z$ GRBs and Exploring Circumburst Environment in the Forthcoming SVOM Era

Wang,

Qiu,

Wei

2020

Preprint

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Rapid spectroscopy of GRB afterglows is an important and hard task. Based on the archival XS-GRB spectral database, we here perform a pilot study on the afterglow's spectroscopy in the forthcoming SVOM era in two aspects. At first, our simulation indicates that the color acquired from the SVOM/VT blue and red channels is effective in discriminating between low-z (z 3) and distant GRB candidates until z ∼ 6. Secondly, by doubling the sample size, we find that the previously proposed global photoionization response of the circumburst gas to the prompt emission (i.e., the CIV/CII-L iso /E 2 peak relationship) is roughly confirmed, although the confirmation is dissatisfactory at the large L iso /E 2 peak end. We believe that this issue can be further addressed in the SVOM era by larger spectroscopy sample, thanks to its capability of rapid identification of optical candidates of afterglow and its anti-solar pointing strategy.

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The SVOM gamma-ray burst mission

Cited by 18 publications

References 14 publications

Detection capabilities of the Athena X-IFU for the warm-hot intergalactic medium using gamma-ray burst X-ray afterglows

Detection capabilities of the Athena X-IFU for the warm-hot intergalactic medium using gamma-ray burst X-ray afterglows

A Program for Multi-Messenger Standard Siren Cosmology in the Era of LIGO A+, Rubin Observatory, and Beyond

A Pilot Study of Catching High-$z$ GRBs and Exploring Circumburst Environment in the Forthcoming SVOM Era

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