Energy response of GECAM gamma-ray detector based on LaBr3:Ce and SiPM array

Zhang, Dali; Li, Xinqiao; Xiong, S. L.; Li, Yanguo; Sun, Xilei; An, Zhu; Xu, Y. B.; Zhu, Yong; Peng, Wen-Xi; Wang, Huan‐Yu; Zhang, Fan

doi:10.1016/j.nima.2018.12.032

Cited by 73 publications

(33 citation statements)

References 16 publications

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“…3.1 探测原理和物理设计 GRD主要功能是实现8 keV-2 MeV伽马射线探测, 测量伽马暴的光变和能谱, 对伽马暴进行定位 [21] . The positioning accuracy distribution obtained by using three typical energy spectra of soft, medium and hard GRB as input is shown in eq.…”

Section: 伽马射线探测器mentioning

confidence: 99%

The GECAM and its payload

Li¹,

Wen²,

An³

et al. 2020

Sci. Sin.-Phys. Mech. Astron.

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Section: 伽马射线探测器mentioning

confidence: 99%

The GECAM and its payload

Li¹,

Wen²,

An³

et al. 2020

Sci. Sin.-Phys. Mech. Astron.

Self Cite

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“…The GECAM (Gravitational Wave Electromagnetic Counterpart All-sky Monitor) mission is the planned Chinese space telescope to monitor the GRBs coincident with GW events, which will launch in late 2020. It has a FOV of 100% all-sky and it has lower detection threshold than Fermi-GBM, about the same as Swift (Zhang et al 2019;Zheng 2019). Our calculation shows that the peak luminosity is about 6×10 46 erg s −1 and 4.0×10 48 erg s −1 at luminosity distance of 200 Mpc and 1 Gpc, respectively, and the number of sGRBs that can be detected by GECAM are 1.04−35.96 yr −1 and 16.97−593.91 yr −1 within 200 Mpc and 1Gpc, respectively, which is about five times larger than that can be detected by Fermi-GBM.…”

Section: Discussionmentioning

confidence: 99%

The Luminosity Distribution of Short Gamma-Ray Bursts under a Structured Jet Scenario

Guo¹,

Wei²,

Wang³

2020

ApJ

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The joint detection of gravitational wave (GW) and electromagnetic radiation from the binary neutron star merger event GW170817 marks a breakthrough in the field of multi-messenger astronomy. The short gamma-ray burst (sGRB) GRB 170817A, associated with this binary neutron star merger event, has an isotropic-equivalent gammaray radiation luminosity of 1.6×10 47 erg s −1 , which is much lower than that of other sGRBs. The measurement of the superluminal movement of the radio afterglow emission confirms the presence of the relativistic jet, and the emission features can be well explained by the structured jet model. In this paper, we calculate the luminosity distribution of sGRBs and its evolution with redshift based on the structured (Gaussian) jet model, and find that the typical luminosity increase with redshift, for nearby sGRBs (such as for luminosity distance less than 200 Mpc) the typical gamma-ray luminosity is just around 10 47 -10 48 erg s −1 , which naturally explains the very low radiation luminosity of GRB 170817A. We derived the detection probability of sGRBs by Fermi-GBM and found that the expected detection rate of sGRBs is only about 1 yr −1 within the distance of several hundred Mpc. We explored the effect of the power-law index α of the merger time distribution on the observed characteristics and found that it had little effect on the observed luminosity and viewing-angle distributions. However, it is very interesting that, for different values of α, the distributions of the number of observed sGRBs are quite different, so it is possible to determine the value of α through observed distributions of the number of sGRBs. We used the Bayesian method to make a quantitative analysis and found that the value of α may be identified when the number of observed sGRBs with known redshifts is more than 200. Finally, we compare our results of gamma-ray luminosity distribution with sGRBs with known redshifts, and found that our results are consistent with the observation, which implies that our simulation results can reproduce the observed luminosity distribution well.Unified Astronomy Thesaurus concepts: Gamma-ray bursts (629); Gamma-ray astronomy (628); Astronomical methods (1043)

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“…Thus we adopt D > 100 Mpc. For sensitivity, we use the gravitational wave high-energy electromagnetic counterpart all-sky monitor (GECAM) as an example, which has S ≈ 2 × 10 −8 erg cm −2 s −1 in 8 − 2000 keV [68]. The corresponding lower limit on luminosity is then L 2.4 × 10 46 erg s −1 .…”

Section: Precursor Modelsmentioning

confidence: 99%

Electromagnetic Precursors of Short Gamma-Ray Bursts as Counterparts of Gravitational Waves

Wang

Liu

2021

Galaxies

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Precursor emissions are found in some short gamma-ray bursts (SGRBs). In this paper, we review the theories and observations of the SGRB precursor and discuss its prospect as an electromagnetic counterpart of the gravitational wave event produced by neutron star (NS) mergers. The observed luminosity, spectrum, and duration of precursors are explained by the magnetospheric interaction model during the inspiral or the cocoon/jet shock breakout model during the jet propagation. In general, these two models predict that the precursor will be weaker than the main GRB, but will be of a larger opening angle, which makes it an advantageous gamma-ray counterpart for NS mergers in the local Universe, especially for NS - black hole mergers with very low mass ratios, in which the main GRBs are not expected. The joint observation of the precursor, SGRB, and gravitational wave will help to reveal the jet launch mechanism and post-merger remnant.

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Energy response of GECAM gamma-ray detector based on LaBr3:Ce and SiPM array

Cited by 73 publications

References 16 publications

The GECAM and its payload

The GECAM and its payload

The Luminosity Distribution of Short Gamma-Ray Bursts under a Structured Jet Scenario

Electromagnetic Precursors of Short Gamma-Ray Bursts as Counterparts of Gravitational Waves

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