Table 1.
Sample of 14 FRBs analysed in this work.
| FRB ID | RA | Dec | Redshift | DMobsb | RMobsc | RMMWd | Source of Narrow-field Data |
|---|---|---|---|---|---|---|---|
| deg | deg | pc cm−3 | rad m−2 | rad m−2 | |||
| FRB 20211127Ia | 199.8087 | −18.8380 | 0.0469 | 234.8 | −67.0 ± 1.0 | −2.9 ± 6.2 | 2dF-AAOmega, 6dF |
| FRB 20211212Aa | 157.3507 | +01.3605 | 0.0707 | 206.0 | +21.0 ± 7.0 | +6.0 ± 5.7 | 2dF-AAOmega |
| FRB 20190608Ba | 334.0199 | −07.8983 | 0.1178 | 338.7 | +353.0 ± 1.0 | −24.4 ± 13.3 | SDSS, KCWI, MUSE |
| FRB 20200430Aa | 229.7064 | +12.3768 | 0.1610 | 380.0 | −195.3 ± 0.7 | +14.5 ± 7.0 | LRIS, DEIMOS, MUSE |
| FRB 20210117A | 339.9795 | −16.1515 | 0.2145 | 729.2 | −45.8 ± 0.7 | +3.3 ± 9.2 | MUSE |
| FRB 20191001Aa | 323.3513 | −54.7477 | 0.2340 | 506.9 | +51.1 ± 0.4 | +23.5 ± 4.3 | 2dF-AAOmega, MUSE |
| FRB 20210320C | 204.4608 | −16.1227 | 0.2797 | 384.6 | +288.8 ± 0.2 | −2.8 ± 5.7 | MUSE |
| FRB 20190102C | 322.4157 | −79.4757 | 0.2912 | 363.6 | −106.1 ± 0.9 | +26.6 ± 7.7 | MUSE |
| FRB 20180924Ba | 326.1052 | −40.9000 | 0.3212 | 362.2 | +17.3 ± 0.8 | +16.5 ± 5.0 | 2dF-AAOmega, MUSE |
| FRB 20211203C | 204.5624 | −31.3803 | 0.3439 | 635.0 | +34.3 ± 1.2 | −29.2 ± 9.1 | MUSE |
| FRB 20200906Aa | 53.4962 | −14.0832 | 0.3688 | 577.8 | +75.4 ± 0.1 | +30.3 ± 19.8 | LRIS, DEIMOS, MUSE |
| FRB 20190611B | 320.7456 | −79.3976 | 0.3778 | 321.4 | +17.0 ± 3.0 | +29.0 ± 10.8 | MUSE |
| FRB 20181112A | 327.3485 | −52.9709 | 0.4755 | 589.3 | +10.5 ± 0.4 | +16.2 ± 5.9 | MUSE |
| FRB 20190711A | 329.4192 | −80.3580 | 0.5220 | 591.6 | +4.0 ± 1.0 | +19.4 ± 6.5 | MUSE |
Notes. From left to right, columns show full FRB name in TNS standard, right ascension, declination, FRB redshift, observed dispersion and rotation measures, total contribution to the rotation measure from the Milky Way (halo and ISM), and instrument or survey used to collect narrow-field spectroscopic information of foreground galaxies.
Part of the FLIMFLAM DR1 (Khrykin et al. 2024b; Huang et al. 2025).
DM measurements adopted from Bannister et al. (2019), Macquart et al. (2020), Heintz et al. (2020), Bhandari et al. (2020).
RM measurements adopted from Scott et al. (2025).
Milky Way RM contributions adopted from Hutschenreuter et al. (2022).
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