A burst storm from the repeating FRB 20200120E in an M81 globular cluster

Nimmo, K.; Hessels, J. W. T.; Snelders, M. P.; Karuppusamy, R.; Hewitt, D. M.; Kirsten, F.; Marcote, B.; Bach, U.; Bansod, A.; Barr, E. D.; Behrend, J.; Bezrukovs, Vladislavs; Buttaccio, S.; Feiler, R.; Gawroński, M.; Lindqvist, Michael; Orbidans, A.; Puchalska, W; Wang, N; Winchen, T.; Wolak, P.; Wu, J.; Yuan, Jianping

doi:10.1093/mnras/stad269

Cited by 30 publications

(22 citation statements)

References 80 publications

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“…The rate can change from less than one burst per hour to more than 100 bursts per hour, as was observed for FRB 20121102A by Li et al (2021a) in their 60 hr of observations spanning 47 days at 1.2 GHz above a 7σ threshold of 0.015 Jy ms. Gajjar et al (2018) also reported clustered arrival times in their high-frequency (4-8 GHz) study of the same source. Nimmo et al (2023) also observed this behavior from FRB 20200120E, where they detected 53 bursts within 40 minutes, almost 80 bursts per hour. Before this epoch, the observed peak rate from the source was 0.4 0.4 2.0 -+ bursts per hour in their Effelsberg observations at 1.4 GHz above a 7σ threshold of 0.05 Jy ms.…”

Section: Burst Rate Evolutionmentioning

confidence: 55%

A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B

Sand,

Breitman,

Michilli

et al. 2023

ApJ

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FRB 20180916B is a repeating fast radio burst (FRB) with a 16.3 day periodicity in its activity. In this study, we present morphological properties of 60 FRB 20180916B bursts detected by CHIME/FRB between 2018 August and 2021 December. We recorded raw voltage data for 45 of these bursts, enabling microseconds time resolution in some cases. We studied variation of spectro-temporal properties with time and activity phase. We find that the variation in dispersion measure (DM) is ≲1 pc cm−3 and that there is burst-to-burst variation in scattering time estimates ranging from ∼0.16 to over 2 ms, with no discernible trend with activity phase for either property. Furthermore, we find no DM and scattering variability corresponding to the recent change in rotation measure from the source, which has implications for the immediate environment of the source. We find that FRB 20180916B has thus far shown no epochs of heightened activity as have been seen in other active repeaters by CHIME/FRB, with its burst count consistent with originating from a Poissonian process. We also observe no change in the value of the activity period over the duration of our observations and set a 1σ upper limit of 1.5 × 10−4 day day−1 on the absolute period derivative. Finally, we discuss constraints on progenitor models yielded by our results, noting that our upper limits on changes in scattering and DM as a function of phase do not support models invoking a massive binary companion star as the origin of the 16.3 day periodicity.

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Section: Burst Rate Evolutionmentioning

confidence: 55%

A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B

Sand,

Breitman,

Michilli

et al. 2023

ApJ

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“…On timescales of order seconds to hours, bursts from repeaters tend to be clustered (e.g. Gajjar et al 2018;Zhang et al 2021;Nimmo et al 2023), in a process which is often modelled as a Weibull distribution (Oppermann, Yu, & Pen 2018) Thus it should be asked: what effect does this have on the modelling? On sufficiently long timescales, FRBs will become inactive, and new repeating FRBs will be born.…”

Section: Non-poissonian Repetitionmentioning

confidence: 99%

Modelling repetition in zDM: A single population of repeating fast radio bursts can explain CHIME data

James

2023

Publ. Astron. Soc. Aust.

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Regardless of whether or not all fast radio bursts (FRBs) repeat, those that do form a population with a distribution of rates. This work considers a power-law model of this population, with rate distribution Φ r ∼ Rγr between Rmin and Rmax. The zDM code is used to model the probability of detecting this population as either apparently once-off or repeat events as a function of redshift, z, and dispersion measure, DM. I demonstrate that in the nearby Universe, repeating sources can contribute significantly to the total burst rate. This causes an apparent deficit in the total number of observed sources (once-off and repeaters) relative to the distant Universe that will cause a bias in FRB population models. Thus instruments with long exposure times should explicitly take repetition into account when fitting the FRB population. I then fit data from The Canadian Hydrogen Intensity Mapping Experiment (CHIME). The relative number of repeat and apparently once-off FRBs, and their DM, declination, and burst rate distributions, can be well-explained by 50–100% of CHIME single FRBs being due to repeaters, with Rmax > 0.75 day–1 above 1039 erg, and This result is surprisingly consistent with follow-up studies of FRBs detected by the Australian Square Kilometre Array Pathfinder (ASKAP). Thus the evidence suggests that CHIME and ASKAP view the same repeating FRB population, which is responsible not just for repeating FRBs, but the majority of apparently once-off bursts. For greater quantitative accuracy, non-Poissonian arrival times, second-order effects in the CHIME response, and a simultaneous fit to the total FRB population parameters, should be treated in more detail in future studies.

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“…We note that another interesting constraint on the DM excess of the CGM comes from the repeating FRB 20200120E, which was recently localized to a globular cluster in M81 (Kirsten et al 2022;Nimmo et al 2023). Since the sightline does not cross the M81 disk, the DM of this FRB puts a tight upper bound on the Milky Way halo DM and M81 halo DM.…”

Section: Introductionmentioning

confidence: 86%

A Measurement of Circumgalactic Gas around Nearby Galaxies Using Fast Radio Bursts

McQuinn

2023

ApJ

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The distribution of gas in the circumgalactic medium (CGM) of galaxies of all types is poorly constrained. Foreground CGMs contribute an extra amount to the dispersion measure (DM) of fast radio bursts (FRBs). We measure this DM excess for the CGMs of 1011–1013 M ⊙ halos using the CHIME/FRB first data release, a halo mass range that is challenging to probe in any other way. Because of the uncertainty in the FRBs’ angular coordinates, only for nearby galaxies is the localization sufficient to confidently associate them with intersecting any foreground halo. Thus we stack on galaxies within 80 Mpc, optimizing the stacking scheme to approximately minimize the stack’s variance and marginalize over uncertainties in FRB locations. The sample has 20–30 FRBs intersecting halos with masses of 1011–1012 M ⊙ and also of 1012–1013 M ⊙, and these intersections allow a marginal 1σ–2σ detection of the DM excess in both mass bins. The bin of 1011–1012 M ⊙ halos also shows a DM excess at 1–2 virial radii. By comparing data with different models for the CGM gas profile, we find that all models are favored by the data up to 2σ level compared to the null hypothesis of no DM excess. With 3000 more bursts from a future CHIME data release, we project a 4σ detection of the CGM. Distinguishing between viable CGM models by stacking FRBs with CHIME-like localization would require tens of thousands of bursts.

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A burst storm from the repeating FRB 20200120E in an M81 globular cluster

Cited by 30 publications

References 80 publications

A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B

A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B

Modelling repetition in zDM: A single population of repeating fast radio bursts can explain CHIME data

A Measurement of Circumgalactic Gas around Nearby Galaxies Using Fast Radio Bursts

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