X-ray and gamma-ray timing of GRB 180720B, GRB 181222B, GRB 211211A, and GRB 220910A observed with Fermi and ASIM

We present a timing study of the gamma and X-ray observations and analysis of a sample of bright gamma-ray bursts (GRBs; i.e. GRB 180720B, GRB 181222B, GRB 211211A, and GRB 220910A), including the very bright and long GRB 211211A (a.k.a. kilonova candidate). They have been detected and observed by t...

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Detalles Bibliográficos
Autores: Caballero-García, María Dolores, Göǧüş, E., Navarro-González, J., Atapin, K. E., Sonbas, E., Uzuner, M., Castro-Tirado, Alberto J., Pandey, Shashi Bhushan, Gupta, Rahul, Ror, Amit Kumar, Hu, Y. D., Wu, Si-Yu, Sánchez Ramírez, Rubén, Guziy, Sergey, Christiansen, F., Connell, P. H., Neubert, Torsten, Østgaard, Nikolai, Adsuara, J. E., Gordillo Vázquez, Francisco J., Fernández-García, E., Pérez-García, I., Reglero, V.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2025
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/384209
Acceso en línea:http://hdl.handle.net/10261/384209
Access Level:acceso abierto
Palabra clave:Methods: data analysis
Gamma-ray burst: general
Gamma-ray burst: individual: GRB 180720B, GRB 181222B, GRB 211211A, and GRB 220910A.
Descripción
Sumario:We present a timing study of the gamma and X-ray observations and analysis of a sample of bright gamma-ray bursts (GRBs; i.e. GRB 180720B, GRB 181222B, GRB 211211A, and GRB 220910A), including the very bright and long GRB 211211A (a.k.a. kilonova candidate). They have been detected and observed by the Atmosphere–Space Interactions Monitor (ASIM) installed on the International Space Station (ISS) and the Gamma-ray Burst Monitor (GBM) onboard the Fermi mission. The early (T − T0≈ s) and high-energy (0.3–20 MeV) ASIM High Energy Detector (HED) and (150 keV–30 MeV) Fermi (BGO) light curves show well-defined peaks with a low quasi-periodic oscillation (QPO) frequency between 2.5 and 3.5 Hz that could be identified with the spin of the neutron star (NS) in the binary mergers originating these GRBs. These QPOs consist on the first detection of low-frequency QPOs (≤10 Hz) detected in magnetars so far. We also detect a strong QPO at 21.8 − 22 Hz in GRB 181222B together with its (less significant) harmonics. The low-frequency QPO would correspond to the signal of the orbiting NS previous to the final coalescence giving rise to the gravitational wave (GW) signal. © 2025 The Author(s).

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