The Host Galaxy of FRB 20190520B and Its Unique Ionized Gas Distribution
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arXiv
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| Auteurs principaux: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866910855750221824 |
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| author | Chen, Xiang-Lei Tsai, Chao-Wei Stern, Daniel Bochenek, Christopher D. Chatterjee, Shami Law, Casey Li, Di Niu, Chenhui Niino, Yuu Feng, Yi Wang, Pei Assef, Roberto J. Li, Guodong Lake, Sean E. Luo, Gan Liao, Mai |
| author_facet | Chen, Xiang-Lei Tsai, Chao-Wei Stern, Daniel Bochenek, Christopher D. Chatterjee, Shami Law, Casey Li, Di Niu, Chenhui Niino, Yuu Feng, Yi Wang, Pei Assef, Roberto J. Li, Guodong Lake, Sean E. Luo, Gan Liao, Mai |
| contents | The properties of host galaxies associated with Fast Radio Bursts (FRBs) provide critical information for inferring the progenitors and radiation mechanisms of these bursts. We report on the host galaxy of the repeating FRB 20190520B, a dwarf galaxy at the spectroscopic redshift $z=0.241$ with a stellar mass of $(6.2 \pm 0.8) \times 10^8 \ M_{\odot}$. The emission line ratios suggest that the ionized gas is powered by star formation. The total H$α$-traced star formation rate (SFR) is $0.70 \pm 0.01 \ {M_{\odot} ~ \rm yr^{-1}}$, and the metallicity is $\rm 12+log_{10} ([O/H]) \geq 7.4 \pm 0.1$. The specific star formation rate (sSFR) is $\rm log \ sSFR/yr^{-1} = -9.0 \pm 0.1$, higher than the upper limit of $-9.4$ observed in nearby dwarf galaxies. The dispersion measure contribution from the host galaxy is estimated to be $\rm DM_{host} \approx 950 \pm 220 \ pc \ cm^{-3}$, based on the H$α$ emission. The FRB and the associated persistent radio source are located at the H$α$ emission peak, offset by $\sim 1.4^{\prime\prime}$ (5.5 kpc) in projection from the stellar continuum. At this position, the lower limit of $\rm \log \ sSFR/yr^{-1}$ is $-8.5 \pm 0.1$, more than three times the galaxy's total sSFR. The H$α$ velocity difference between the stellar continuum and the offset gas is $39.6 \pm 0.4$ km s$^{-1}$, which is sufficient to draw conclusions about the nature of the offset. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_01740 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Host Galaxy of FRB 20190520B and Its Unique Ionized Gas Distribution Chen, Xiang-Lei Tsai, Chao-Wei Stern, Daniel Bochenek, Christopher D. Chatterjee, Shami Law, Casey Li, Di Niu, Chenhui Niino, Yuu Feng, Yi Wang, Pei Assef, Roberto J. Li, Guodong Lake, Sean E. Luo, Gan Liao, Mai Astrophysics of Galaxies The properties of host galaxies associated with Fast Radio Bursts (FRBs) provide critical information for inferring the progenitors and radiation mechanisms of these bursts. We report on the host galaxy of the repeating FRB 20190520B, a dwarf galaxy at the spectroscopic redshift $z=0.241$ with a stellar mass of $(6.2 \pm 0.8) \times 10^8 \ M_{\odot}$. The emission line ratios suggest that the ionized gas is powered by star formation. The total H$α$-traced star formation rate (SFR) is $0.70 \pm 0.01 \ {M_{\odot} ~ \rm yr^{-1}}$, and the metallicity is $\rm 12+log_{10} ([O/H]) \geq 7.4 \pm 0.1$. The specific star formation rate (sSFR) is $\rm log \ sSFR/yr^{-1} = -9.0 \pm 0.1$, higher than the upper limit of $-9.4$ observed in nearby dwarf galaxies. The dispersion measure contribution from the host galaxy is estimated to be $\rm DM_{host} \approx 950 \pm 220 \ pc \ cm^{-3}$, based on the H$α$ emission. The FRB and the associated persistent radio source are located at the H$α$ emission peak, offset by $\sim 1.4^{\prime\prime}$ (5.5 kpc) in projection from the stellar continuum. At this position, the lower limit of $\rm \log \ sSFR/yr^{-1}$ is $-8.5 \pm 0.1$, more than three times the galaxy's total sSFR. The H$α$ velocity difference between the stellar continuum and the offset gas is $39.6 \pm 0.4$ km s$^{-1}$, which is sufficient to draw conclusions about the nature of the offset. |
| title | The Host Galaxy of FRB 20190520B and Its Unique Ionized Gas Distribution |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2503.01740 |