Abstract Details
| Name: Param Joshi Affiliation: National Institute of Technology Rourkela Conference ID: ASI2025_12 Title : High Frequency Wideband Study of FRB20240114A with the Allen Telescope Array Authors and Co-Authors : Param Joshi, V. Gajjar, W. Farah, S. Z. Sheikh, A. W. Pollak, A. P. V. Siemion, Alex Medina, Joel T. Earwicker, L. Cruz, J. Hickish, P. Premnath, D. DeBoer, R. Donnachie, G. Singh, R. H. Davis, M. Snodgrass, P. Karn Abstract Type : Poster Abstract Category : High Energy Phenomena, Fundamental Physics and Astronomy Abstract : FRB 20240114A, a bright repeating fast radio burst, was initially reported by the CHIME/FRB collaboration on January 26th 2024. High fluence emissions (> 10 Jy-ms) from this source have been reported by numerous radio telescopes. This FRB was detected at a DM of 527.7 pc cm^-3 and is localized to a host galaxy at redshift Z = 0.42. Previous surveys indicate that the bursts exhibit highly band-limited or narrowband emission characteristics, spanning less than ~100 MHz. In this presentation, I will report on our wideband study of FRB 20240114A using the upgraded Allen Telescope Array (ATA) of the SETI Institute, USA. Our observations cover two independent 672 MHz spectral bands, which were incrementally stepped to uniformly cover the 1 to 7.5 GHz range. We conducted approximately 1200 hours of observations, representing one of the largest follow-up campaigns of repeating FRBs across the widest frequency ranges. Thus far, 42 bursts have been detected in the frequency range of 1 to 3 GHz. Notably, our findings reveal that, in contrast to previous observations, FRB 20240114A exhibits wideband emission, with five bursts covering an unprecedented total bandwidth of approximately 800 MHz. I will also discuss various burst properties such as width, fluence, spectral occupancy, burst rate, etc. This presentation will also address the energy budget of these broadband bursts, which can help scrutinize various emission mechanism models given its distance and host galaxy environment. |