{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/detection-and-localisation-of-the-highly","title":"Detection and localisation of the highly active FRB 20240114A with MeerKAT","arxiv_id":"2408.10988","date":"2024-08-20","proceeding":null,"authors":["J. Tian","K. M. Rajwade","I. Pastor-Marazuela","B. W. Stappers","M. C. Bezuidenhout","M. Caleb","F. Jankowski","E. D. Barr","M. Kramer"],"abstract":"We report observations of the highly active FRB 20240114A with MeerKAT using the Ultra-High Frequency (UHF; $544\\text{--}1088$ MHz) and L-band ($856\\text{--}1712$ MHz) receivers. A total of 62 bursts were detected in coherent tied-array beams using the MeerTRAP real-time transient detection pipeline. We measure a structure-optimising dispersion measure of $527.65\\pm0.01\\,\\text{pc}\\,\\text{cm}^{-3}$ using the brightest burst in the sample. We find the bursts of FRB 20240114A are generally detected in part of the broad band of MeerKAT, $\\sim40\\%$ in the UHF and $\\sim30\\%$ in the L-band, indicating the band limited nature. We analyse the fluence distribution of the 44 bursts detected at UHF, constraining the fluence completeness limit to $\\sim1\\,$Jy ms, above which the cumulative burst rate follows a power law $R (>F)\\propto (F/1\\,\\text{Jy}\\,\\text{ms})^\\gamma$ with $\\gamma=-1.8\\pm0.2$. Using channelised telescope data captured in our transient buffer we localise FRB 20240114A in the image domain to RA = 21h27m39.86s, Dec = +04d19m45.01s with an uncertainty of 1.4 arcsec. This localisation allows us to confidently identify the host galaxy of FRB 20240114A. Also using the transient buffer data we perform a polarimetric study and demonstrate that most of the bursts have $\\sim100\\%$ linear polarisation fractions and up to $\\sim20\\%$ circular polarisation fractions. Finally, we predict the flux density of a potential persistent radio source (PRS) associated with FRB 20240114A is $\\backsimeq[0.6\\text{--}60]\\,\\mu\\text{Jy}$ based on the simple relation between the luminosity of the PRS and the rotation measure arising from the FRB local environment.","url_abs":"https://arxiv.org/abs/2408.10988v1","url_pdf":"https://arxiv.org/pdf/2408.10988v1.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"detection-and-localisation-of-the-highly","repo_url":"https://github.com/astrolaura/meerkat_source_matching","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":0,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"syntology_url":null,"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}