A Search for the Host Galaxy of FRB 171020

Mahony, E. K.; Ekers, R. D.; Macquart, Jean–Pierre; Sadler, E. M.; Bannister, K. W.; Bhandari, Shivani; Flynn, Chris; Koribalski, B. S.; Prochaska, J. Xavier; Ryder, S. D.; Shannon, R. M.; Tejos, Nicolás; Whiting, M. T.; Wong, O. I.

doi:10.3847/2041-8213/aae7cb

Cited by 58 publications

(48 citation statements)

References 39 publications

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“…In the era of ASKAP and CHIME, through detecting and localizing hundreds or thousands of FRBs in short periods of time, one might expect that far brighter and/or nearby FRBs could be detected. Potentially the closest FRB yet detected is the lowest DM detection by ASKAP, FRB171020, most likely identified with the galaxy ESO 601−G036 at a redshift of 0.00867 (∼37 Mpc) (Mahony et al 2018). If FRB181228 occured in ESO 601−G36, its radio flux density would be approximately 1900 times higher, or approximately 35.5 kJy.…”

Section: Discussionmentioning

confidence: 98%

A Search of TESS Full-frame Images for a Simultaneous Optical Counterpart to FRB 181228

Tingay

Yang

2019

ApJ

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FRB181228 was detected by the Molonglo Synthesis Radio Telescope (MOST) at a position and time coincident with Transiting Exoplanet Survey Satellite (TESS) observations, representing the first simultaneous multi-wavelength data collection for a Fast Radio Burst (FRB). The large imaged field-ofview of TESS allows a search over the uncertainty region produced by MOST. However, the TESS pixel scale of 21 and the Full Frame Image (FFI) cadence of 30 minutes is not optimal for the detection of an FOB with a possible millisecond duration. We search the TESS FFIs and find no events with a limiting TESS magnitude of 16, assuming a 30 minute event duration, corresponding to an optical flux density upper limit of approximately 2000 Jy for a ∼ 1 ms signal duration, assuming no signal loss. In addition, the cosmic ray mitigation method for TESS significantly reduces its sensitivity to short timescale transients, which we quantify. We compare our results to the predictions of Yang et al. (2019) and find that the upper limit is a factor of two thousand higher than the predicted maximum optical flux density. However, we find that if FRB181228 had occurred in the galaxy thought to host the nearest FRB detection to date (37 Mpc), an FOB may have been detectable by TESS. In the near future, when CHIME and ASKAP will detect hundreds to thousands of FRBs, TESS may be able to detect FOBs from those rare bright and nearby FRBs within this large population (if more sophisticated cosmic ray excision can be implemented).

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Section: Discussionmentioning

confidence: 98%

A Search of TESS Full-frame Images for a Simultaneous Optical Counterpart to FRB 181228

Tingay

Yang

2019

ApJ

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“…However, once FRBs are more routinely localized to host galaxies, the types of galaxies and the specific regions thereof in which they reside may provide some of the most important clues for identifying sub-populations. The repeating FRB 121102 resides in a low-metalicity dwarf galaxy, and searches for galaxies of similar type have been done for other FRBs (Mahony et al, 2018). If some FRBs are found to reside in larger galaxies, or at different radii from their host galaxy centers, such as for GRBs (Kulkarni, 2018), this may provide a valuable tool for distinguishing between types of FRB sources.…”

Section: Sub-populations Emerging?mentioning

confidence: 99%

Fast radio bursts

Petroff

Hessels

Lorimer

2019

Astron Astrophys Rev

622

471

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The discovery of radio pulsars over a half century ago was a seminal moment in astronomy. It demonstrated the existence of neutron stars, gave a powerful observational tool to study them, and has allowed us to probe strong gravity, dense matter, and the interstellar medium. More recently, pulsar surveys have led to the serendipitous discovery of fast radio bursts (FRBs). While FRBs appear similar to the individual pulses from pulsars, their large dispersive delays suggest that they originate from far outside the Milky Way and hence are many ordersof-magnitude more luminous. While most FRBs appear to be one-off, perhaps cataclysmic events, two sources are now known to repeat and thus clearly have a longer-lived central engine. Beyond understanding how they are created, there is also the prospect of using FRBs -as with pulsars -to probe the extremes of the Universe as well as the otherwise invisible intervening medium. Such studies will be aided by the high implied all-sky event rate: there is a detectable FRB roughly once every minute occurring somewhere on the sky. The fact that less than a hundred FRB sources have been discovered in the last decade is largely due to the small fields-of-view of current radio telescopes. A new generation of wide-field instruments is now coming online, however, and these will be capable of detecting multiple FRBs per day. We are thus on the brink of further breakthroughs in the short-duration radio transient phase space, which will be critical for differentiating between the many proposed theories for the origin of FRBs. In this review, we give an observational and theoretical introduction at a level that is accessible to astronomers entering the field.

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“…Plasma and gravitational lensing. Refraction and especially lensing from discrete structures causes multiple imaging from the Crab pulsar (Graham Smith et al 2011), strong enhancements of pulse amplitudes from the bow shock produced by a millisecond pulsar (Main et al 2018), fringes in the dynamic spectra of pulsars (Wolszczan & Cordes 1987), and events in the radio light curves of AGNs (Fiedler et al 1987;Bannister et al 2016). The strongly episodic burst detections from the repeating FRB 121102 may be explained most easily from plasma lensing and the overall detection rate could also be affected.…”

Section: Scintillation Source Size Requirementsmentioning

confidence: 99%