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Peer-reviewedCC BY 4.0The Astrophysical Journal

Fast Radio Bursts Associated with Persistent Radio Sources Prefer Hydrogen-poor Superluminous Supernova Host Environments

  • Fujia Li1
  • Fei Liu1
  • Di Li1
  • Dongzi Li1
  • Ziheng Ding1
  • Ran Gao1
  1. 1Tsinghua University
Open at sourcePDFDOICite

Abstract

A subset of repeating fast radio bursts (FRBs) is associated with compact persistent radio sources (PRSs). The FRB-PRS hosts differ dramatically from the general FRB host population: they do not follow the distribution of localized non-PRS FRB hosts, nor the star formation rate (SFR)-weighted or mass-weighted mock host distributions expected for the general star-forming galaxy population, instead occupying the extreme low-mass, high-specific star formation rate (sSFR), and low-metallicity end of host-galaxy parameter space. We compare these hosts with well-defined samples of hydrogen-poor superluminous supernovae (SLSNe-I), hydrogen-rich superluminous supernovae (SLSNe-II), and Type II core-collapse supernovae (CCSNe). Using cumulative distribution functions (CDFs) and statistical tests, we find that FRB-PRSs tend to reside in dwarf galaxies with high sSFRs and low gas-phase metallicities, even relative to galaxies of similar stellar mass. Their hosts are most similar to those of SLSNe-I, but differ significantly from CCSN hosts, with SLSN-II hosts lying between these populations. These results suggest that FRB-PRSs do not simply trace star formation activity or the general FRB host population, but instead favor SLSN-I-like environments. This preference is consistent with young magnetars formed through low-metallicity massive-star channels, for which SLSN-I-like ejecta imply a characteristic free–free transparency time of ∼29 yr at 600 MHz.

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Cite

BibTeXRIS
BibTeX
@article{li2026fast,
  title = {{Fast Radio Bursts Associated with Persistent Radio Sources Prefer Hydrogen-poor Superluminous Supernova Host Environments}},
  author = {Fujia Li and Fei Liu and Di Li and Dongzi Li and Ziheng Ding and Ran Gao},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = nov,
  doi = {10.3847/1538-4357/aeaa53},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aeaa53},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Fast Radio Bursts Associated with Persistent Radio Sources Prefer Hydrogen-poor Superluminous Supernova Host Environments
AU  - Fujia Li
AU  - Fei Liu
AU  - Di Li
AU  - Dongzi Li
AU  - Ziheng Ding
AU  - Ran Gao
PY  - 2026
DA  - 2026/11/03
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aeaa53
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aeaa53
AB  - A subset of repeating fast radio bursts (FRBs) is associated with compact persistent radio sources (PRSs). The FRB-PRS hosts differ dramatically from the general FRB host population: they do not follow the distribution of localized non-PRS FRB hosts, nor the star formation rate (SFR)-weighted or mass-weighted mock host distributions expected for the general star-forming galaxy population, instead occupying the extreme low-mass, high-specific star formation rate (sSFR), and low-metallicity end of host-galaxy parameter space. We compare these hosts with well-defined samples of hydrogen-poor superluminous supernovae (SLSNe-I), hydrogen-rich superluminous supernovae (SLSNe-II), and Type II core-collapse supernovae (CCSNe). Using cumulative distribution functions (CDFs) and statistical tests, we find that FRB-PRSs tend to reside in dwarf galaxies with high sSFRs and low gas-phase metallicities, even relative to galaxies of similar stellar mass. Their hosts are most similar to those of SLSNe-I, but differ significantly from CCSN hosts, with SLSN-II hosts lying between these populations. These results suggest that FRB-PRSs do not simply trace star formation activity or the general FRB host population, but instead favor SLSN-I-like environments. This preference is consistent with young magnetars formed through low-metallicity massive-star channels, for which SLSN-I-like ejecta imply a characteristic free–free transparency time of ∼29 yr at 600 MHz.
SN  - 1538-4357
SN  - 0004-637X
ER  -