Niu, Jia-Rui and Zhu, Wei-Wei and Zhang, Bing and Yuan, Mao and Zhou, De-Jiang and Zhang, Yong-Kun and Jiang, Jin-Chen and Han, J. L. and Li, Di and Lee, Ke-Jia and Wang, Pei and Feng, Yi and Li, Dong-Zi and Luo, Rui and Wang, Fa-Yin and Dai, Zi-Gao and Miao, Chen-Chen and Niu, Chen-Hui and Xu, Heng and Zhang, Chun-Feng and Wang, Wei-Yang and Wang, Bo-Jun and Xu, Jiang-Wei (2022) FAST Observations of an Extremely Active Episode of FRB 20201124A. IV. Spin Period Search. Research in Astronomy and Astrophysics, 22 (12). Art. No. 124004. ISSN 1674-4527. doi:10.1088/1674-4527/ac995d. https://resolver.caltech.edu/CaltechAUTHORS:20230117-372591200.32
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Abstract
We report the properties of more than 800 bursts detected from the repeating fast radio burst (FRB) source FRB 20201124A with the Five-hundred-meter Aperture Spherical radio Telescope during an extremely active episode on UTC 2021 September 25th-28th in a series of four papers. In this fourth paper of the series, we present a systematic search of the spin period and linear acceleration of the source object from both 996 individual pulse peaks and the dedispersed time series. No credible spin period was found from this data set. We rule out the presence of significant periodicity in the range between 1 ms and 100 s with a pulse duty cycle <0.49 ± 0.08 (when the profile is defined by a von-Mises function, not a boxcar function) and linear acceleration up to 300 m s⁻² in each of the four one-hour observing sessions, and up to 0.6 m s⁻² in all 4 days. These searches contest theoretical scenarios involving a 1 ms–100 s isolated magnetar/pulsar with surface magnetic field <10¹⁵ G and a small duty cycle (such as in a polar-cap emission mode) or a pulsar with a companion star or black hole up to 100 M_⊙ and P_b > 10 hr. We also perform a periodicity search of the fine structures and identify 53 unrelated millisecond-timescale "periods" in multi-components with the highest significance of 3.9σ. The "periods" recovered from the fine structures are neither consistent nor harmonically related. Thus they are not likely to come from a spin period. We caution against claiming spin periodicity with significance below ∼4σ with multi-components from one-off FRBs. We discuss the implications of our results and the possible connections between FRB multi-components and pulsar microstructures.
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Additional Information: | We thank the referee, Scott Ransom, for helpful comments. This work made use of data from the FAST, a Chinese national mega-science facility, built and operated by the National Astronomical Observatories, Chinese Academy of Sciences. This work is supported by the National SKA Program of China (Nos. 2020SKA0120200 and 2020SKA0120100), the National Natural Science Foundation of China (Grant Nos. 12041303, 11873067 and 12041304) the National Key R&D Program of China (Nos. 2017YFA0402600, 2021YFA0718500 and 2017YFA0402602), the CAS-MPG LEGACY project, the Max-Planck Partner Group, and the Key Research Project of Zhejiang Lab (No. 2021PE0AC0). J. L. Han is supported by the National Natural Science Foundation of China (NSFC, Nos. 11988101 and 11833009) and the Key Research Program of the Chinese Academy of Sciences (Grant No. QYZDJ-SSW-SLH021); D. J. Zhou is supported by the Cultivation Project for the FAST scientific Payoff and Research Achievement of CAMS-CAS. | ||||||||||||||||||||||||||||
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Issue or Number: | 12 | ||||||||||||||||||||||||||||
DOI: | 10.1088/1674-4527/ac995d | ||||||||||||||||||||||||||||
Record Number: | CaltechAUTHORS:20230117-372591200.32 | ||||||||||||||||||||||||||||
Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20230117-372591200.32 | ||||||||||||||||||||||||||||
Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||
ID Code: | 118829 | ||||||||||||||||||||||||||||
Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||
Deposited By: | Research Services Depository | ||||||||||||||||||||||||||||
Deposited On: | 10 Feb 2023 20:49 | ||||||||||||||||||||||||||||
Last Modified: | 10 Feb 2023 20:49 |
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