2026ApJ...996L..16M

Query : 2026ApJ...996L..16M

2026ApJ...996L..16M - Astrophys. J., 996, L16 (2026/January-1)

A Milliarcsecond Localization Associates FRB 20190417A with a Compact Persistent Radio Source and an Extreme Magnetoionic Environment.

MOROIANU A.M., BHANDARI S., DROUT M.R., HESSELS J.W.T., HEWITT D.M., KIRSTEN F., MARCOTE B., PLEUNIS Z., SNELDERS M.P., SRIDHAR N., BACH U., BEMPONG-MANFUL E.K., BEZRUKOVS V., BLAAUW R., BRAY J.D., BUTTACCIO S., CHATTERJEE S., CORONGIU A., FEILER R., GAENSLER B.M., GAWRONSKI M.P., GIROLETTI M., IBIK A.L., KARUPPUSAMY R., LAZDA M., LEUNG C., LINDQVIST M., MASUI K.W., MICHILLI D., NIMMO K., OULD-BOUKATTINE O.S., PANDHI A., PARAGI Z., PEARLMAN A.B., PUCHALSKA W., SCHOLZ P., SHIN K., SLUMAN J.J., TRUDU M., WILLIAMS-BALDWIN D. and YANG J.

Abstract (from CDS):

We report the milliarcsecond localization of a high (∼1379 pc cm–3) dispersion measure (DM) repeating fast radio burst (FRB), FRB 20190417A. Combining European VLBI Network detections of five repeat bursts, we confirm the FRB's host to be a low-metallicity, star-forming dwarf galaxy at z = 0.12817, similar to the hosts of FRB 20121102A, FRB 20190520B, and FRB 20240114A. We also confirm that it is associated with a previously reported persistent radio source (PRS), which is compact on milliarcsecond scales. Visibility-domain model fitting constrains the transverse physical size of the PRS to <23 pc and yields an integrated flux density of 190 ± 40 μJy at 1.4 GHz. Though we do not find significant evidence for DM evolution, FRB 20190417A exhibits a time-variable rotation measure (RM) ranging between +3958 ± 11 rad m–2 and +5061 ± 24 rad m–2 over a 50-day period. We find no evidence for intervening galaxy clusters in the FRB's line of sight and place a conservative lower limit on the rest-frame host DM contribution of 1228 pc cm–3 (90% confidence)-the largest known for any FRB so far. This system strengthens the emerging picture of a rare subclass of repeating FRBs with large and variable RMs, above-average host DMs, and luminous PRS counterparts in metal-poor dwarf galaxies. Our results suggest that these systems are the result of environmental selection, or a distinct engine for FRB emission.

Abstract Copyright: © 2025. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Radio transient sources - Transient sources - Radio bursts - Very long baseline interferometry - High energy astrophysics - Burst astrophysics

Simbad objects: 18

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Number of rows : 18
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 20180916B rB 01 58 00.750 +65 43 00.30           ~ 457 0
2 PSR J0248+6021 Psr 02 48 18.642 +60 21 34.70           ~ 63 1
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
4 FRB 20201124A rB 05 07 57.600 +26 11 24.00           ~ 307 0
5 FRB 20181119D rB 05 31 58.6980 +33 08 52.588           ~ 933 0
6 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
7 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4725 3
8 FRB 20200120E rB 09 57 56.7 +68 49 32           ~ 219 0
9 FRB 20191106C rB 13 18 +43.0           ~ 22 0
10 FRB 20190520B rB 16 02 04.270 -11 17 17.32           ~ 211 0
11 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
12 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 4970 3
13 PSR J1745-2900 Psr 17 45 40.1640 -29 00 29.818           ~ 358 0
14 NAME Sgr 1935+2154 * 19 34 55.68 +21 53 48.2           ~ 820 1
15 NAME FRB 190417.J1939+59 rB 19 39 04.0 +59 19 55           ~ 37 0
16 FRB 20240619D rB 19 49 29.210 -25 12 49.40           ~ 7 0
17 FRB 20240114A rB 21 27 39.8350 +04 19 45.634           ~ 66 0
18 PSR B2255+58 Psr 22 57 57.744 +59 09 14.83     12.59     ~ 96 0

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