Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe

Bhandari, Shivani; Heintz, K. E.; Aggarwal, K. K.; Marnoch, Lachlan; Day, Cherie K.; Sydnor, Jessica; Burke-Spolaor, S.; Law, Casey J.; Prochaska, J. Xavier; Tejos, Nicolás; Bannister, K. W.; Butler, B. J.; Deller, Adam; Ekers, R. D.; Flynn, Chris; Fong, W.; James, C. W.; Lazio, T. Joseph W.; Luo, Rui; Mahony, E. K.; Ryder, S. D.; Sadler, E. M.; Shannon, R. M.; Han, J. L.; Lee, Kejia; Zhang, Bing

doi:10.3847/1538-3881/ac3aec

Cited by 136 publications

(125 citation statements)

References 93 publications

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“…The sources of FRBs and their emission mechanisms are still uncertain (see Petroff et al 2021;Lyubarsky 2021, for recent reviews), but growing numbers of FRBs (Amiri et al 2021) and localizations within host galaxies (e.g. Bannister et al 2019;Bhandari et al 2022) recently boosted our understanding of their statistical properties.…”

Section: Introductionmentioning

confidence: 99%

The FRB 20121102A November rain in 2018 observed with the Arecibo Telescope

Spitler¹,

Nimmo²,

Hewitt³

et al. 2022

Preprint

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We present 849 new bursts from FRB 20121102A detected with the 305-m Arecibo Telescope. Observations were conducted as part of our regular campaign to monitor the activity and evolution of burst properties. The 10 reported observations were carried out between 1150 and 1730 MHz and fall in the active period around November 2018. All bursts were dedispersed at the same dispersion measure and are consistent with a single value of (562.4 ± 0.1) pc cm −3 . The burst rate varies between 0 bursts and 218 ± 16 bursts per hour, the highest rate observed to date. The times between consecutive bursts show a bimodal distribution. We find that arrival times with separations > 0.1 s are best described as a Poisson process with varying rate, compared to models with additional parameters. Clustering on time-scales of 22 ms is reflecting a characteristic time-scale of the source and possibly the emission mechanism. We analyse the spectro-temporal structure of the bursts by fitting 2D Gaussians with a temporal drift to each sub-burst in the dynamic spectra. We find a linear relationship between the sub-burst's drift and its duration. At the same time the drifts are consistent with coming from the sad-trombone effect. This has not been predicted by current models. The energy distribution shows an excess of high energy bursts and is insufficiently modeled by a single power-law even within single observations. We find long-term changes in the energy distribution and the average spectrum compared to earlier and later published observations. Finally, despite the large burst rate we find no strict short-term periodicity.

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Section: Introductionmentioning

confidence: 99%

The FRB 20121102A November rain in 2018 observed with the Arecibo Telescope

Spitler¹,

Nimmo²,

Hewitt³

et al. 2022

Preprint

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“…Substantial analysis showed FRB hosts do not track stellar mass or star formation rate (SFR). The population is statistically consistent with hosts of short gamma-ray bursts (SGRBs) and core-collapse supernovae (CCSNe) [11]. Some FRBs have large offsets from galaxy center that consistent with SGRBs, indicating that they might originate from similar events like binary neutron star (NS) mergers [161].…”

Section: Host Galaxy Propertiesmentioning

confidence: 58%

“…Most FRB hosts are moderately star-forming galaxies and lie offset from the star-forming main sequence. Also, a dearth of red galaxies was found [11]. Substantial analysis showed FRB hosts do not track stellar mass or star formation rate (SFR).…”

Section: Host Galaxy Propertiesmentioning

confidence: 99%

Fast Radio Bursts

Xiao¹,

Wang²,

Dai³

2022

Preprint

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The era of fast radio bursts (FRBs) was open in 2007, when a very bright radio pulse of unknown origin was discovered occasionally in the archival data of Parkes Telescope. Over the past fifteen years, this mysterious phenomenon have caught substantial attention among the scientific community and become one of the hottest topic in high-energy astrophysics. The total number of events has a dramatic increase to a few hundred recently, benefiting from new dedicated surveys and improved observational techniques. Our understanding of these bursts has been undergoing a revolutionary growth with observational breakthroughs announced consistently. In this chapter, we will give a comprehensive introduction of FRBs, including the latest progress. Starting from the basics, we will go through population study, inherent physical mechanism, and all the way to the application in cosmology. Plenty of open questions exist right now and there is more surprise to come in this active young field.

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“…Heintz et al 2020), two lie in dwarf galaxies (Chatterjee et al 2017;Niu et al 2021), and one lies in an elliptical or lenticular galaxy (Bannister et al 2019). The relationship between the current sample of known host galaxies and FRB progenitor channels also remains unclear (Heintz et al 2020;Mannings et al 2021;Bhandari et al 2022), although most FRB hosts currently appear to be moderately star-forming (Bhandari et al 2022). As our primary goal is to assess a fiducial amount of scattering that may be expected from host galaxies, we do not examine a variety of progenitor channels or large-scale redshift evolution in the FRB progenitor population.…”

Section: Scattering From a Population Of Host Galaxiesmentioning

confidence: 99%

Radio Scattering Horizons for Galactic and Extragalactic Transients

Ocker,

Cordes,

Chatterjee

et al. 2022

Preprint

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Radio wave scattering can cause severe reductions in detection sensitivity for surveys of Galactic and extragalactic fast (∼ms duration) transients. While Galactic sources like pulsars are subject to scattering in the Milky Way interstellar medium (ISM), extragalactic fast radio bursts (FRBs) can also experience scattering in their host galaxies and other galaxies intervening their lines-of-sight. We assess Galactic and extragalactic scattering horizons for fast radio transients using a combination of NE2001 to model the dispersion measure (DM) and scattering time (τ ) contributed by the Milky Way, and independently constructed electron density models for other galaxies' ISMs and halos that account for different galaxy morphologies, masses, densities, and strengths of turbulence. For FRB source redshifts z s 1, an all-sky, isotropic FRB population has values of τ ranging between ∼ 1 µs and ∼ 2 ms at 1 GHz (observer frame) that are dominated by host galaxies. For a hypothetical, high-redshift (z s ∼ 5) FRB population, τ ranges from ∼ 0.01 − 100s of ms at 1 GHz, and is largely dominated by intervening galaxies. About 20% of these high-redshift FRBs are predicted to have τ > 5 ms at 1 GHz (observer frame), and 40% of FRBs between z s ∼ 0.5 − 5 are predicted to have τ 1 ms for ν ≤ 800 MHz. The percentage of FRBs selected against from scattering may be substantially larger because our scattering predictions are conservative compared to localized FRBs, and if circumgalactic turbulence causes density fluctuations larger than those observed from nearby halos.

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Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe

Cited by 136 publications

References 93 publications

The FRB 20121102A November rain in 2018 observed with the Arecibo Telescope

The FRB 20121102A November rain in 2018 observed with the Arecibo Telescope

Fast Radio Bursts

Radio Scattering Horizons for Galactic and Extragalactic Transients

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