A repeating fast radio burst source localized to a nearby spiral galaxy

Marcote, B.; Nimmo, K.; Hessels, J. W. T.; Tendulkar, Shriharsh P.; Bassa, C. G.; Paragi, Z.; Keimpema, A.; Bhardwaj, Mohit; Karuppusamy, R.; Kaspi, V. M.; Law, Casey J.; Michilli, D.; Aggarwal, K. K.; Andersen, Bridget C.; Archibald, Anne M.; Bandura, Kevin; Bower, Geoffrey C.; Boyle, P. J.; Brar, Charanjot; Burke-Spolaor, S.; Butler, B. J.; Cassanelli, Tomas; Chawla, Pragya; Demorest, Paul; Dobbs, M.; Fonseca, Emmanuel; Giri, Utkarsh; Good, Deborah C.; Gourdji, K.; Josephy, Alexander; Kirichenko, A.; Kirsten, F.; Landecker, T. L.; Lang, Dustin; Lazio, T. Joseph W.; Li, D. Z.; Lin, H.; Linford, Justin D.; Masui, Kiyoshi; Mena-Parra, Juan; Naidu, Arun; Ng, Cherry; Patel, C.; Pen, Ue-Li; Pleunis, Ziggy; Rafiei-Ravandi, Masoud; Rahman, Mubdi; Rénard, A.; Scholz, Paul; Siegel, Seth R.; Smith, Kendrick M.; Stairs, I. H.; Vanderlinde, K.; Zwaniga, A. V.

doi:10.1038/s41586-019-1866-z

Cited by 401 publications

(460 citation statements)

References 76 publications

(112 reference statements)

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“…Following (Marcote et al 2020), we remark that the radio position of FRB 180916 is positionally coincident with a remarkable "cusp" of star formation in its host galaxy. If this is not a coincidence, the apparent cusp can actually be a "wake" of stars caused by the presence of a BH of a mass sufficiently large to influence an otherwise ordered flow.…”

Section: The Black Hole Hypothesismentioning

confidence: 79%

Gamma-Ray and X-Ray Observations of the Periodic-repeater FRB 180916 during Active Phases

Tavani

Verrecchia

Casentini

et al. 2020

ApJL

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FRB 180916 is a most intriguing source capable of producing repeating fast radio bursts with a periodic 16.3 day temporal pattern. The source is well positioned in a star forming region in the outskirts of a nearby galaxy at 150 Mpc distance. In this paper we report on the X-ray and γ-ray observations of FRB 180916 obtained by AGILE and Swift. We focused especially on the recurrent 5-day time intervals of enhanced radio bursting. In particular, we report on the results obtained in the time intervals Feb. 3 -8;Feb. 25; Mar. 5 -10; Mar. 22 -28, 2020 during a multiwavelength campaign involving high-energy and radio observations of FRB 180916. We also searched for temporal coincidences at millisecond timescales between the 32 known radio bursts of FRB 180916 and X-ray and MeV events detectable by AGILE. We do not detect any simultaneous event or any extended X-ray and γ-ray emission on timescales of hours/days/weeks.Our cumulative X-ray (0.3-10 keV) flux upper limit of 5 × 10 −14 erg cm −2 s −1 (obtained during 5-day active intervals from several 1-2 ks integrations) translates into an isotropic luminosity upper limit of L X,U L ∼ 1.5× 10 41 erg s −1 . Deep γ-ray observations above 100MeV over a many-year timescale provide an average luminosity upper limit one order of magnitude larger. These results provide the so-far most stringent upper limits on highenergy emission from the FRB 180916 source. Our results constrain the dissipation of

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Section: The Black Hole Hypothesismentioning

confidence: 79%

Gamma-Ray and X-Ray Observations of the Periodic-repeater FRB 180916 during Active Phases

Tavani

Verrecchia

Casentini

et al. 2020

ApJL

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“…The young active NSs are born in core-collapse explosions. Recently, a second repeating FRB 180916.J0158+65 was localized to a star-forming region in a nearby massive spiral galaxy (Marcote et al 2020). Two coherent mechanisms are often considered in current FRB models: curvature radiation by bunches (Katz 2014(Katz , 2018aKumar et al 2017;Ghisellini & Locatelli 2018;Yang & Zhang 2018) and the maser mechanisms (Lyubarsky 2014;Beloborodov 2017;Ghisellini 2017;Waxman 2017;Lu & Kumar 2018;Metzger et al 2019;Beloborodov 2019).…”

Section: Introductionmentioning

confidence: 99%

Fast Radio Bursts from Activity of Neutron Stars Newborn in BNS Mergers: Offset, Birth Rate, and Observational Properties

Wang

Yang

et al. 2020

ApJ

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Young neutron stars (NSs) born in core-collapse explosions are promising candidates for the central engines of fast radio bursts (FRBs), since the first localized repeating burst FRB 121102 happens in a star forming dwarf galaxy, which is similar to the host galaxies of superluminous supernovae (SLSNe) and long gamma-ray bursts (LGRBs). However, FRB 180924 and FRB 190523 are localized to massive galaxies with low rates of star formation, compared with the host of FRB 121102. Meanwhile, the offsets between the bursts and host centers are about 4 kpc and 29 kpc for FRB 180924 and FRB 190523, respectively. These properties of hosts are similar to short gamma-ray bursts (SGRBs), which are produced by mergers of binary neutron star (BNS) or neutron star-black hole (NS-BH). Therefore, the NSs powering FRBs may be formed in BNS mergers. In this paper, we study the BNS merger rates, merger times, and predict their most likely merger locations for different types of host galaxies using population synthesis method. We find that the BNS merger channel is consistent with the recently reported offsets of FRB 180924 and FRB 190523. The offset distribution of short GRBs is well reproduced by population synthesis using galaxy model which is similar to GRB hosts. The event rate of FRBs (including non-repeating and repeating), is larger than those of BNS merger and short GRBs, which requires a large fraction of observed FRBs emitting several bursts. Using curvature radiation by bunches in NS magnetospheres, we also predict the observational properties of FRBs from BNS mergers, including the dispersion measure, and rotation measure. At late times (t ≥ 1yr), the contribution to dispersion measure and rotation measure from BNS merger ejecta could be neglected.

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“…In such cases, we adopt the reported duration as an intrinsic duration, w int , instead of our calculation. The spec-z flag is for four FRBs with spectroscopic redshift measured from the host galaxies (FRB 121102, 180916.J0158+65, 180924, and 190523;Tendulkar et al 2017;Marcote et al 2020;Bannister et al 2019;. For these four FRBs we use the spectroscopic redshifts instead of the redshift estimated from the dispersion measure.…”

Section: Samplementioning

confidence: 99%

“…As a conservative estimate, we adopted the highest uncertainty of DM IGM (z), δDM IGM (z), among simulations with different resolutions (Zhu et al 2018). We used spectroscopic redshift instead of DM-derived redshift if available (i.e., FRB121102, 180916.J0158+65, 180924, and 190523: Tendulkar et al 2017;Marcote et al 2020;Bannister et al 2019;). We calculated time-integrated luminosities of FRBs at rest-frame 1.83 GHz by using Eq.…”

Section: Time-integrated Luminositymentioning

confidence: 99%

Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts

Hashimoto

Goto

Wang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Fast radio bursts (FRBs) are mysterious radio bursts with a time scale of approximately milliseconds. Two populations of FRB, namely repeating and non-repeating FRBs, are observationally identified. However, the differences between these two and their origins are still cloaked in mystery. Here we show the time-integrated luminosityduration (L ν -w int,rest ) relations and luminosity functions (LFs) of repeating and nonrepeating FRBs in the FRB Catalogue project. These two populations are obviously separated in the L ν -w int,rest plane with distinct LFs, i.e., repeating FRBs have relatively fainter L ν and longer w int,rest with a much lower LF. In contrast with non-repeating FRBs, repeating FRBs do not show any clear correlation between L ν and w int,rest . These results suggest essentially different physical origins of the two. The faint ends of the LFs of repeating and non-repeating FRBs are higher than volumetric occurrence rates of neutron-star mergers and accretion-induced collapse (AIC) of white dwarfs, and are consistent with those of soft gamma-ray repeaters (SGRs), type Ia supernovae, magnetars, and white-dwarf mergers. This indicates two possibilities: either (i) faint non-repeating FRBs originate in neutron-star mergers or AIC and are actually repeating during the lifetime of the progenitor, or (ii) faint non-repeating FRBs originate in any of SGRs, type Ia supernovae, magnetars, and white-dwarf mergers. The bright ends of LFs of repeating and non-repeating FRBs are lower than any candidates of progenitors, suggesting that bright FRBs are produced from a very small fraction of the progenitors regardless of the repetition. Otherwise, they might originate in unknown progenitors.

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A repeating fast radio burst source localized to a nearby spiral galaxy

Cited by 401 publications

References 76 publications

Gamma-Ray and X-Ray Observations of the Periodic-repeater FRB 180916 during Active Phases

Gamma-Ray and X-Ray Observations of the Periodic-repeater FRB 180916 during Active Phases

Fast Radio Bursts from Activity of Neutron Stars Newborn in BNS Mergers: Offset, Birth Rate, and Observational Properties

Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts

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