2025A&A...693A..85Y

Query : 2025A&A...693A..85Y

2025A&A...693A..85Y - Astronomy and Astrophysics, volume 693A85 (2025/1-1)

Constraining the Hubble constant with scattering in host galaxies of fast radio bursts.

YANG T.-C., HASHIMOTO T., HSU T.-Y., GOTO T., LING C.-T., HO S.C.-C., CHEN A.Y.-A. and KILERCI E.

Abstract (from CDS):

Aims. Measuring the Hubble constant (H0) 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 millisecondsḊMIGM, the free electron column density along a line of sight in the intergalactic medium (IGM), could open a new avenue for probing H0. 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 H0. 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 H0. 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 H0 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 H0. Our result is H0 = 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^{+68}_{-48} $ 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 H0. The reduction in systematic error is comparable to the Hubble tension (∼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.

Abstract Copyright: © The Authors 2025

Journal keyword(s): scattering - intergalactic medium - cosmological parameters

Simbad objects: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 FRB 20210603A rB 00 41 05.774 +21 13 34.57           ~ 17 0
2 FRB 20180916B rB 01 58 00.750 +65 43 00.30           ~ 457 0
3 FRB 20220319D rB 02 08 42.700 +71 02 06.94           ~ 39 0
4 FRB 20180924A rB 02 21 50.4000 +37 31 12.000           ~ 10 0
5 FRB 20190614D rB 04 20 18.13 +73 42 24.3           ~ 37 0
6 FRB 20201124A rB 05 07 57.600 +26 11 24.00           ~ 307 0
7 FRB 20181119D rB 05 31 58.6980 +33 08 52.588           ~ 933 0
8 FRB 180301 rB 06 12 43.40 +04 33 44.8           ~ 125 0
9 FRB 20220310F rB 08 58 52.920 +73 29 27.00           ~ 25 0
10 FRB 20200120E rB 09 57 56.7 +68 49 32           ~ 219 0
11 NAME FRB 181030.J1054+73 rB 10 33 24.0000 +73 47 24.000           ~ 79 0
12 FRB 190714 rB 12 15 55.1 -13 01 16           ~ 64 0
13 FRB 210320 rB 13 37 16.800 -15 24 37.30           ~ 29 0
14 FRB 190523 rB 13 48 15.6 +72 28 11           ~ 109 0
15 FRB 20220418A rB 14 36 25.340 +70 05 45.40           ~ 24 0
16 FRB 200430 rB 15 18 49.54 +12 22 36.8           ~ 59 0
17 FRB 20220920A rB 16 01 01.700 +70 55 07.68           ~ 28 0
18 FRB 20190520B rB 16 02 04.270 -11 17 17.32           ~ 211 0
19 FRB 20210405I rB 17 01 21.50 -49 32 42.8           ~ 17 0
20 FRB 20221012A rB 18 43 11.690 +70 31 27.15           ~ 25 0
21 FRB 20220914A rB 18 48 13.630 +73 20 12.89           ~ 31 0
22 FRB 20220509G rB 18 50 40.800 +70 14 37.80           ~ 37 0
23 FRB 20220207C rB 20 40 47.890 +72 52 56.38           ~ 29 0
24 FRB 20220825A rB 20 47 55.550 +72 35 05.89           ~ 25 0
25 FRB 20220506D rB 21 12 10.760 +72 49 38.20           ~ 24 0
26 FRB 190611 rB 21 22 58.91 -79 23 51.3           ~ 82 0
27 FRB 190102 rB 21 29 39.76 -79 28 32.5           ~ 83 0
28 FRB 191001 rB 21 33 24.373 -54 44 51.40           ~ 64 0
29 FRB 20210410D rB 21 44 20.70 -79 19 05.5           ~ 23 0
30 FRB 181112 rB 21 49 23.630 -52 58 15.39           ~ 131 0
31 FRB 20190711A rB 21 57 40.7 -80 21 29           ~ 114 0
32 FRB 190608 rB 22 16 04.74 -07 53 53.6           ~ 102 0
33 FRB 20210117A rB 22 39 55.015 -16 09 05.45           ~ 49 0
34 FRB 191228 rB 22 57 43.30 -29 35 38.7           ~ 37 0
35 FRB 20220912A rB 23 09 04.9 +48 42 25           ~ 126 0
36 FRB 20220307B rB 23 23 29.880 +72 11 32.59           ~ 26 0
37 FRB 20220610A rB 23 24 17.569 -33 30 49.37           ~ 31 0

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