The 60 pc Environment of FRB 20180916B

Tendulkar, Shriharsh P.; Paz, A. Gil de; Kirichenko, A.; Hessels, J. W. T.; Bhardwaj, Mohit; Avila, Fernando Bastos De; Bassa, Cees; Chawla, Pragya; Fonseca, Emmanuel; Kaspi, V. M.; Keimpema, A.; Kirsten, F.; Lazio, T. Joseph W.; Marcote, B.; Masui, Kiyoshi; Nimmo, K.; Paragi, Zsolt; Rahman, Mubdi; Paya, D.; Scholz, Paul; Stairs, I. H.

doi:10.3847/2041-8213/abdb38

Cited by 103 publications

(114 citation statements)

References 98 publications

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“…This distance makes FRB 20180916B by far the closest known FRB source with a precise localization; in fact, it is also the most precisely localized FRB to date. The 2.3 mas localization provided by the European VLBI Network (EVN; Marcote et al 2020), coupled with 60-90 mas imaging from the Hubble Space Telescope (HST), demonstrates that FRB 20180916B is close to but still offset by ∼250 pc from the nearest knot of star formation in the host galaxy (Tendulkar et al 2021). This suggests that FRB 20180916B may be too old (100 kyr-10 Myr) to host an active magnetar.…”

Section: Introductionmentioning

confidence: 99%

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LOFAR Detection of 110–188 MHz Emission and Frequency-dependent Activity from FRB 20180916B

Pleunis

Michilli

Bassa

et al. 2021

ApJL

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The object FRB 20180916B is a well-studied repeating fast radio burst source. Its proximity (∼150 Mpc), along with detailed studies of the bursts, has revealed many clues about its nature, including a 16.3 day periodicity in its activity. Here we report on the detection of 18 bursts using LOFAR at 110-188 MHz, by far the lowest-frequency detections of any FRB to date. Some bursts are seen down to the lowest observed frequency of 110 MHz, suggesting that their spectra extend even lower. These observations provide an order-of-magnitude stronger constraint on the optical depth due to free-free absorption in the source's local environment. The absence of circular polarization and nearly flat polarization angle curves are consistent with burst properties seen at 300-1700 MHz. Compared with higher frequencies, the larger burst widths (∼40-160 ms at 150 MHz) and lower linear polarization fractions are likely due to scattering. We find ∼2-3 rad m −2 variations in the Faraday rotation measure that may be correlated with the activity cycle of the source. We compare the LOFAR burst arrival times to those of 38 previously published and 22 newly detected bursts from the uGMRT (200-450 MHz) and CHIME/ FRB (400-800 MHz). Simultaneous observations show five CHIME/FRB bursts when no emission is detected by LOFAR. We find that the burst activity is systematically delayed toward lower frequencies by about 3 days from 600 to 150 MHz. We discuss these results in the context of a model in which FRB 20180916B is an interacting binary system featuring a neutron star and high-mass stellar companion.

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Section: Introductionmentioning

confidence: 99%

“…This suggests that FRB 20180916B may be too old (100 kyr-10 Myr) to host an active magnetar. Rather, Tendulkar et al (2021) argued that FRB 20180916B may be a high-mass X-ray binary (HMXB), where interaction between the companion wind and neutron star magnetosphere produces FRBs.…”

Section: Introductionmentioning

confidence: 99%

LOFAR Detection of 110–188 MHz Emission and Frequency-dependent Activity from FRB 20180916B

Pleunis

Michilli

Bassa

et al. 2021

ApJL

Self Cite

159

146

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“…Multiwavelength follow-ups of this source provide constraints on the FRB progenitor and the local environment, and also introduce additional puzzles. Imaging from the Hubble Space Telescope shows that the location of FRB 180916 is offset by ∼250 pc from the nearest knot of star formation in the host galaxy (Tendulkar et al 2021), while young magnetars are expected to born in a star-forming region. For bursts detected in the L band, the change of linear polarization position angle (PA) is constrained to be 10°-20°across the bursts of the same phase (Nimmo et al 2020), and  50°across the L-band active phases (Pastor-Marazuela et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Emission Properties of Periodic Fast Radio Bursts from the Motion of Magnetars: Testing Dynamical Models

Zanazzi

2021

ApJL

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Recent observations of the periodic fast radio burst source 180916.J0158+65 (FRB 180916) find small linear polarization position angle swings during and between bursts, with a burst activity window that becomes both narrower and earlier at higher frequencies. Although the observed chromatic activity window disfavors models of periodicity in FRB 180916 driven solely by the occultation of a neutron star by the optically thick wind from a stellar companion, the connection to theories where periodicity arises from the motion of a bursting magnetar remains unclear. In this Letter, we show how altitude-dependent radio emission from a magnetar, with bursts emitted from regions that are asymmetric with respect to the magnetic dipole axis, can lead to burst activity windows and polarization consistent with the recent observations. In particular, the fact that bursts arrive systematically earlier at higher frequencies disfavors theories where the FRB periodicity arises from forced precession of a magnetar by a companion or fallback disk, but is consistent with theories where periodicity originates from a slowly rotating or freely precessing magnetar. Several observational tests are proposed to verify/ differentiate between the remaining theories, and pin down which theory explains the periodicity in FRB 180916.

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“…Only one other repeating FRB (FRB 180916.J0158+65) has been localized (Marcote et al 2020) to a star-forming region in a massive spiral galaxy. Similar to FRB 121102, FRB 180916.J0158 + 65 is offset from this knot of the star-forming region (Bassa et al 2017;Tendulkar et al 2021). No persistent radio emission has been detected in any of these other localized FRBs.…”

Section: Introductionmentioning

confidence: 76%

Multiwavelength Follow-up of FRB180309

Aggarwal

Burke-Spolaor

Tejos

et al. 2021

ApJ

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We report on the results of multiwavelength follow-up observations with Gemini, Very Large Array (VLA), and Australia Telescope Compact Array to search for a host galaxy and any persistent radio emission associated with FRB 180309. This FRB is among the most luminous FRB detections to date, with a luminosity of >8.7 × 10 32 erg Hz −1 at the dispersion-based redshift upper limit of 0.32. We used the high-significance detection of FRB 180309 with the Parkes Telescope and a beam model of the Parkes Multibeam Receiver to improve the localization of the FRB to a region spanning approximately 2 2 ¢´¢. We aimed to seek bright galaxies within this region to determine the strongest candidates as the originator of this highly luminous FRB. We identified optical sources within the localization region above our r-band magnitude limit of 24.27, 14 of which have photometric redshifts whose fitted mean is consistent with the redshift upper limit (z < 0.32) of our FRB. Two of these galaxies are coincident with marginally detected "persistent" radio sources of flux density 24.3 μJy beam −1 and 22.1 μJy beam −1 , respectively. Our redshift-dependent limit on the luminosity of any associated persistent radio source is comparable to the luminosity limits for other localized FRBs. We analyze several properties of the candidate hosts we identified, including chance association probability, redshift, and presence of radio emission; however, it remains possible that any of these galaxies could be the host of this FRB. Follow-up spectroscopy on these objects to explore their Hα emission and ionization contents, as well as to obtain more precisely measured redshifts, may be able to isolate a single host for this luminous FRB.

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The 60 pc Environment of FRB 20180916B

Cited by 103 publications

References 98 publications

LOFAR Detection of 110–188 MHz Emission and Frequency-dependent Activity from FRB 20180916B

LOFAR Detection of 110–188 MHz Emission and Frequency-dependent Activity from FRB 20180916B

Emission Properties of Periodic Fast Radio Bursts from the Motion of Magnetars: Testing Dynamical Models

Multiwavelength Follow-up of FRB180309

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