WALLABY Pilot Survey: H i in the Host Galaxy of a Fast Radio Burst

Glowacki, Marcin; Lee-Waddell, K.; Deller, Adam T.; Deg, Nathan; Gordon, Alexa C.; Grundy, J. A.; Marnoch, Lachlan; Shen, Ao; Ryder, S. D.; Shannon, R. M.; Wong, O. I.; Dénes, H.; Koribalski, B. S.; Murugeshan, C.; Rhee, J.; Westmeier, T.; Bhandari, Shivani; Bosma, A.; Holwerda, Benne W.; Prochaska, J. Xavier

doi:10.3847/1538-4357/acc1e3

Cited by 6 publications

(7 citation statements)

References 56 publications

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“…At z = 0.0469, FRB 20211127I is a relatively young (≈4 Gyr), nearby spiral galaxy with an age and redshift among the lowest in the sample. This host additionally shows an elevated H I-to-stellar mass ratio and has a slight asymmetry in H I (Glowacki et al 2023). The other notable outlier is the host age of FRB 20210807D.…”

Section: Stellar Population Propertiesmentioning

confidence: 92%

The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors

Gordon,

Fong,

Kilpatrick

et al. 2023

ApJ

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We present a comprehensive catalog of observations and stellar population properties for 23 highly secure host galaxies of fast radio bursts (FRBs). Our sample comprises 6 repeating FRBs and 17 apparent nonrepeaters. We present 82 new photometric and 8 new spectroscopic observations of these hosts. Using stellar population synthesis modeling and employing nonparametric star formation histories (SFHs), we find that FRB hosts have a median stellar mass of ≈109.9 M ⊙, mass-weighted age ≈5.1 Gyr, and ongoing star formation rate ≈1.3 M ⊙ yr−1 but span wide ranges in all properties. Classifying the hosts by degree of star formation, we find that 87% (20 of 23 hosts) are star-forming, two are transitioning, and one is quiescent. The majority trace the star-forming main sequence of galaxies, but at least three FRBs in our sample originate in less-active environments (two nonrepeaters and one repeater). Across all modeled properties, we find no statistically significant distinction between the hosts of repeaters and nonrepeaters. However, the hosts of repeating FRBs generally extend to lower stellar masses, and the hosts of nonrepeaters arise in more optically luminous galaxies. While four of the galaxies with the clearest and most prolonged rises in their SFHs all host repeating FRBs, demonstrating heightened star formation activity in the last ≲100 Myr, one nonrepeating host shows this SFH as well. Our results support progenitor models with short delay channels (i.e., magnetars formed via core-collapse supernova) for most FRBs, but the presence of some FRBs in less-active environments suggests a fraction form through more delayed channels.

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Section: Stellar Population Propertiesmentioning

confidence: 92%

The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors

Gordon,

Fong,

Kilpatrick

et al. 2023

ApJ

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“…Nevertheless, recent H I observations of the host galaxy of the non-repeating FRB 20211127I do not show evidence for any significant asymmetry (Glowacki et al 2023). This particular host galaxy is similar in size and morphology to ESO 601-G036, possibly suggesting that the two bursts could have a common origin mechanism despite their host galaxies having quite different interaction histories.…”

Section: Constraining An Frb Progenitor Modelmentioning

confidence: 76%

“…In these aforementioned systems, all five FRB host galaxies have highly asymmetric emission line spectra, linking FRB progenitors to recent galaxy interaction events. However, recent work by Glowacki et al (2023), finds the H I in the host galaxy of FRB 20211127I to be relatively undisturbed. With only a handful of current examples, detailed analysis of the gas in and around FRB host galaxies is still an emerging topic.…”

Section: Introductionmentioning

confidence: 98%

The host galaxy of FRB 20171020A revisited

Lee-Waddell

James

Ryder

et al. 2023

Publ. Astron. Soc. Aust.

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The putative host galaxy of FRB 20171020A was first identified as ESO 601-G036 in 2018, but as no repeat bursts have been detected, direct confirmation of the host remains elusive. In light of recent developments in the field, we re-examine this host and determine a new association confidence level of 98%. At 37 Mpc, this makes ESO 601-G036 the third closest FRB host galaxy to be identified to date and the closest to host an apparently non-repeating FRB (with an estimated repetition rate limit of $<$ $0.011$ bursts per day above $10^{39}$ erg). Due to its close distance, we are able to perform detailed multi-wavelength analysis on the ESO 601-G036 system. Follow-up observations confirm ESO 601-G036 to be a typical star-forming galaxy with H i and stellar masses of $\log_{10}\!(M_{\rm{H\,{\small I}}} / M_\odot) \sim 9.2$ and $\log_{10}\!(M_\star / M_\odot) = 8.64^{+0.03}_{-0.15}$ , and a star formation rate of $\text{SFR} = 0.09 \pm 0.01\,{\rm M}_\odot\,\text{yr}^{-1}$ . We detect, for the first time, a diffuse gaseous tail ( $\log_{10}\!(M_{\rm{H\,{\small I}}} / M_\odot) \sim 8.3$ ) extending to the south-west that suggests recent interactions, likely with the confirmed nearby companion ESO 601-G037. ESO 601-G037 is a stellar shred located to the south of ESO 601-G036 that has an arc-like morphology, is about an order of magnitude less massive, and has a lower gas metallicity that is indicative of a younger stellar population. The properties of the ESO 601-G036 system indicate an ongoing minor merger event, which is affecting the overall gaseous component of the system and the stars within ESO 601-G037. Such activity is consistent with current FRB progenitor models involving magnetars and the signs of recent interactions in other nearby FRB host galaxies.

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“…Of more benefit will be the Widefield ASKAP Lband Legacy All-sky Blind surveY (WALLABY; Koribalski et al 2020). WALLABY has a spatial resolution of 30″, and is currently ongoing and resulted in the first commensal detection of an FRB and the H I in its host galaxy (Glowacki et al 2023). WALLABY offers an improved angular resolution and depth (z < 0.09) to ALFALFA and HIPASS, and so will enable association of nearby FRBs to hosts without the need for dedicated optical follow-up.…”

Section: Frb Host Galaxy Redshiftsmentioning

confidence: 99%

“…Nonetheless, it remains an avenue to obtain a spectroscopic redshift for FRB host galaxies when optical follow-up is difficult. H I has been detected and studied in five FRB host galaxies to date, where four have shown signs of strong asymmetry in the H I global spectrum and/or disturbed H I intensity maps that were attributed to recent galaxy merger or interaction events (Michałowski 2021;Kaur et al 2022;Lee-Waddell et al 2023), and the fifth with less signs of interaction (Glowacki et al 2023). Thus far, no nondetections of H I have been reported in nearby FRB hosts, in line with the finding by Gordon et al (2023) that FRB host galaxies tend to be in star-forming galaxies.…”

Section: Introductionmentioning

confidence: 99%

H i, FRB, What’s Your z: The First FRB Host Galaxy Redshift from Radio Observations

Glowacki,

Bera,

Lee-Waddell

et al. 2024

ApJL

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Identification and follow-up observations of the host galaxies of fast radio bursts (FRBs) not only help us understand the environments in which the FRB progenitors reside, but also provide a unique way of probing the cosmological parameters using the dispersion measures (DMs) of FRBs and distances to their origin. A fundamental requirement is an accurate distance measurement to the FRB host galaxy, but for some sources viewed through the Galactic plane, optical/near-infrared spectroscopic redshifts are extremely difficult to obtain due to dust extinction. Here we report the first radio-based spectroscopic redshift measurement for an FRB host galaxy, through detection of its neutral hydrogen (H i) 21 cm emission using MeerKAT observations. We obtain an H i–based redshift of z = 0.0357 ± 0.0001 for the host galaxy of FRB 20230718A, an apparently nonrepeating FRB detected in the Commensal Real-time ASKAP Fast Transients survey and localized at a Galactic latitude of –0.°367. Our observations also reveal that the FRB host galaxy is interacting with a nearby companion, which is evident from the detection of an H i bridge connecting the two galaxies. A subsequent optical spectroscopic observation confirmed an FRB host galaxy redshift of 0.0359 ± 0.0004. This result demonstrates the value of H i to obtain redshifts of FRBs at low Galactic latitudes and redshifts. Such nearby FRBs whose DMs are dominated by the Milky Way can be used to characterize these components and thus better calibrate the remaining cosmological contribution to dispersion for more distant FRBs that provide a strong lever arm to examine the Macquart relation between cosmological DM and redshift.

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WALLABY Pilot Survey: H i in the Host Galaxy of a Fast Radio Burst

Cited by 6 publications

References 56 publications

The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors

The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors

The host galaxy of FRB 20171020A revisited

H i, FRB, What’s Your z: The First FRB Host Galaxy Redshift from Radio Observations

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