2020/05/31 by Sunil Simha, Joseph N. Burchett, J. Xavier Prochaska +12
Physics and Astronomy · #Astrophysical Phenomena and Observations #COSMIC cancer database #Cosmic background radiation #Cosmic microwave background #Dark matter #Fast radio burst #Galaxy #Gamma-ray bursts and supernovae #Halo #Measure (data warehouse) #Monte Carlo method #Pulsars and Gravitational Waves Research #Sky #astro-ph.GA
paper · pdf · doi:10.3847/1538-4357/abafc3
14 pages, 9 figures, 3 tables. The full version of Table 1 is available as a LaTeX file. Only the first 10 entries are present in the print version. Submitted to ApJ
openalex created_date 2020/06/05 · openalex publication_date 2020/09/30 · arxiv created 2020/12/21 · arxiv updated 2020/12/24 · openalex updated_date 2026/08/06
Abstract Fast radio burst (FRB) 190608 was detected by the Australian Square Kilometre Array Pathfinder (ASKAP) and localized to a spiral galaxy at in the Sloan Digital Sky Survey (SDSS) footprint. The burst has a large dispersion measure ( ) compared to the expected cosmic average at its redshift. It also has a large rotation measure ( ) and scattering timescale ( τ = 3.3 ms at 1.28 GHz). Chittidi et al. perform a detailed analysis of the ultraviolet and optical emission of the host galaxy and estimate the host DM contribution to be . This work complements theirs and reports the analysis of the optical data of galaxies in the foreground of FRB 190608 in order to explore their contributions to the FRB signal. Together, the two studies delineate an observationally driven, end-to-end study of matter distribution along an FRB sightline, the first study of its kind. Combining our Keck Cosmic Web Imager (KCWI) observations and public SDSS data, we estimate the expected cosmic dispersion measure along the sightline to FRB 190608. We first estimate the contribution of hot, ionized gas in intervening virialized halos ( ). Then, using the Monte Carlo Physarum Machine methodology, we produce a 3D map of ionized gas in cosmic web filaments and compute the DM contribution from matter outside halos ( ). This implies that a greater fraction of ionized gas along this sightline is extant outside virialized halos. We also investigate whether the intervening halos can account for the large FRB rotation measure and pulse width and conclude that it is implausible. Both the pulse broadening and the large Faraday rotation likely arise from the progenitor environment or the host galaxy.