The GECAM and its payload

Li, Xinqiao; Wen, Xiang-Yang; An, Zhenghua; Xu, Y. B.; Liang, X. H.; Yang, S.; Sun, Xilei; Liu, Xiaojing; Gao, Min; Wang, Jin‐Zhou; Zhang, Dali; Gong, Ke; Liu, YaQing; Zhao, X. F.; Peng, W. X.; Zhu, Yue; Li, Gang; Qiao, Rui; Guo, D. Y.; Liao, J. Y.; Lu, H.; Wang, Hui; Li, Yanguo; Chen, Gang; Zhang, Fan; Xiong, S. L.

doi:10.1360/sspma-2019-0417

Cited by 34 publications

(10 citation statements)

References 8 publications

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“…, the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM,Li et al 2020), the X/Gamma-ray Imaging Spectrometer (XGIS) on board of the Transient High-Energy Sky and Early Universe Surveyor (THESEUS,Amati et al 2018Amati et al , 2021Ciolfi et al ( …”

mentioning

confidence: 99%

Perspectives for multi-messenger astronomy with the next generation of gravitational-wave detectors and high-energy satellites

Ronchini,

Branchesi,

Oganesyan

et al. 2022

Preprint

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The Einstein Telescope (ET) is going to bring a revolution for the future of multi-messenger astrophysics. In order to detect the counterparts of binary neutron star (BNS) mergers at high redshift, the high-energy observations will play a crucial role. Here, we explore the perspectives of ET, as single observatory and in a network of gravitational-wave (GW) detectors, operating in synergy with future γ-ray and X-ray satellites. We predict the high-energy emission of BNS mergers and its detectability in a theoretical framework which is able to reproduce the properties of the current sample of observed short GRBs (SGRB). We estimate the joint GW and high-energy detection rate for both the prompt and afterglow emissions, testing several combinations of instruments and observational strategies. We find that the vast majority of SGRBs detected in γ-rays will have a detectable GW counterpart; the joint detection efficiency approaches 100% considering a network of third generation GW observatories. The probability of identifying the electromagnetic counterpart of BNS mergers is significantly enhanced if the sky localisation provided by GW instruments is observed by wide field X-ray monitors. We emphasize that the role of the future X-ray observatories will be very crucial for the detection of the fainter emission outside the jet core, which will allow us to probe the yet unexplored population of low-luminosity SGRBs in the nearby Universe, as well as to unveil the nature of the jet structure and the connections with the progenitor properties.

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confidence: 99%

Perspectives for multi-messenger astronomy with the next generation of gravitational-wave detectors and high-energy satellites

Ronchini,

Branchesi,

Oganesyan

et al. 2022

Preprint

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“…Limited by the opening angle of GCXT photon output window (about 20 • ), the GCXT is placed at the perpendicular bisector of GECAM-01 and GECAM-02 with about 4 m away from these two satellites to allow X-rays irradiating both of them at the same time. The distance between the two satellites is about 1 m. Some GRDs (#5, #6, #13, #14, #15, #16, #22, #23, #24) [14] facing to the X-ray tube can receive more X-ray photons because they have larger receiving area to the X-ray flux. Considering the maximum photon energy generated by GCXT is about 20 keV, only the high gain channel of the GRD could detect these photons.…”

Section: Grb Simulation Experiments For Gecam On the Groundmentioning

confidence: 99%

“…As in a triode system, the grid cutoff voltage determining the state of negligible tube current is directly related to the anode voltage and so to the maximum X-ray energy. Due to the modulation voltage swing, the energy modulation range is limited to the soft X-ray band (about 1 to 10 keV) [13], which is relatively lower than the observation energy range (about 6 keV to 5 MeV) of GECAM [14]. A newly released highvoltage precision operational amplifier ADHV4702-1 manufactured by Analog Devices Inc. [15] is applied in the GRB simulator to achieve the modulation of X-ray at higher energies (up to about 20 keV).…”

Section: Introductionmentioning

confidence: 99%

Design and test of a portable Gamma-Ray Burst simulator for GECAM

Chen,

Xiao,

Xiong

et al. 2021

Preprint

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The main scientific goal of the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) is to monitor various types of Gamma-Ray Bursts (GRB) originated from merger of binary compact stars, which could also produce gravitational wave, and collapse of massive stars. In order to study the response of GECAM Gamma-Ray Detectors (GRDs) to high-energy bursts and test the in-flight trigger and localization software of GECAM before the launch, a portable GRB simulator device is designed and implemented based on grid controlled X-ray tube (GCXT) and direct digital synthesis (DDS) technologies. The design of this GRB simulator which modulates X-ray flux powered by high voltage up to 20 kV is demonstrated, and the time jitter (FWHM) of the device is about 0.9 µs. Before the launch in December, 2020, both two GECAM satellites were irradiated by different types of GRBs (including short and long bursts in duration) generated by this GRB simulator. The light curves detected with GECAM/GRDs are consistent with the programmed input functions within statistical uncertainties, indicating the good performance of both the GRDs and the GRB simulator.

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“…Over the past decades, there have been many missions or instruments dedicated to the search of rapid X/gammaray transients (e.g., Fishman et al 1993;Boella et al 1997;Kawai et al 1999;Gehrels et al 2004;Meegan et al 2009;Wen et al 2019;Li et al 2020). These instruments all have a wide field of view to increase the probability of catching a transient source from an unknown location.…”

Section: Introductionmentioning

confidence: 99%

Searching for single-frame rapid X-ray transients detected with Chandra

Zhang¹,

Feng²

2022

Preprint

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We propose a new method to identify rapid X-ray transients observed with focusing telescopes. They are statistically significant if three or more photons are detected with Chandra in a single CCD frame within a point-spread-function region. In the Chandra archive, 144 such events are identified after discrimination of cosmic rays and background flares; 16 of them are on top of a weak X-ray source and others emerge out of pure background. Optical counterparts or host galaxies are found for some of them thanks to the superb angular resolution of Chandra. Some events are spatially coincident with normal stars in the Milky Way and are most likely produced by stellar flares. They may represent a new class of stellar flares with short durations (a few seconds), perhaps due to a compact flaring region. Some events may be produced by X-ray binaries, with at least one credible identification. This method would enable identification of quiescent X-ray binaries using Chandra with only three photons. Some events are spatially coincident with distant galaxies and could be produced by the prompt emission of short gamma-ray bursts (GRBs); this method would allow us to detect lowluminosity 170817A-like GRBs at a cosmological distance. Magnetars could also produce rapid X-ray events but no identification can be claimed in this work.

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The GECAM and its payload

Cited by 34 publications

References 8 publications

Perspectives for multi-messenger astronomy with the next generation of gravitational-wave detectors and high-energy satellites

Perspectives for multi-messenger astronomy with the next generation of gravitational-wave detectors and high-energy satellites

Design and test of a portable Gamma-Ray Burst simulator for GECAM

Searching for single-frame rapid X-ray transients detected with Chandra

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