Akademik Veri Yönetim Sistemi
ASTRONOMY & ASTROPHYSICS, cilt.693, 2025 (SCI-Expanded, Scopus)
Aims. Measuring the Hubble constant (H-0) is one of the most important missions in astronomy. Nevertheless, recent studies exhibit differences between the employed methods. Methods. Fast radio bursts (FRBs) are coherent radio transients with large dispersion measures (DM) with a duration of milliseconds(D)over dotM(IGM), the free electron column density along a line of sight in the intergalactic medium (IGM), could open a new avenue for probing H-0. However, it has been challenging to separate DM contributions from different components (i.e., the IGM and the host galaxy plasma), and this hampers the accurate measurements of DMIGM and hence H-0. We adopted a method to overcome this problem by using the temporal scattering of the FRB pulses due to the propagation effect through the host galaxy plasma (scattering time). The scattering-inferred DM in a host galaxy improves the estimate of DMIGM, which in turn leads to a better constraint on H-0. In previous studies, a certain value or distribution has conventionally been assumed of the dispersion measure in host galaxies (DMh). We compared this method with ours by generating 100 mock FRBs, and we found that our method reduces the systematic (statistical) error of H-0 by 9.1% (1%) compared to the previous method. Results. We applied our method to 30 localized FRB sources with both scattering and spectroscopic redshift measurements to constrain H-0. Our result is H-0 = 74(-7.2)(+7.5) km s(-1) Mpc(-1), where the central value prefers the value obtained from local measurements over the cosmic microwave background. We also measured DMh with a median value of 103(-48)(+68) pc cm(-3). Conclusions. The DMh had to be assumed in previous works to derive DMIGM. Scattering enables us to measure DMIGM without assuming DMh to constrain H-0. The reduction in systematic error is comparable to the Hubble tension (similar to 10%). Combined with the fact that more localized FRBs will become available, our result indicates that our method can be used to address the Hubble tension using future FRB samples.