STARE2: Detecting Fast Radio Bursts in the Milky Way

Bochenek, Christopher; McKenna, D.; Belov, K.; Kocz, J.; Kulkarni, S. R.; Lamb, James W.; Ravi, Vikram; Woody, D. P.

doi:10.1088/1538-3873/ab63b3

Cited by 56 publications

(46 citation statements)

References 31 publications

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“…The observational situation changed abruptly with the recent discovery of a luminous millisecond radio burst from the Galactic magnetar SGR 1935+2154 (Bochenek et al 2020c;CHIME/FRB Collaboration et al 2020b). The double-peaked burst, detected independently by CHIME (Bandura et al 2014) and STARE2 (Bochenek et al 2020b), was temporally coincident with an X-ray burst of significantly larger fluence Mereghetti et al 2020a;Ridnaia et al 2020e;Tavani et al 2020). This FRB is still a factor of ∼10 less energetic than the weakest FRB previously detected from any localized cosmological FRB source.…”

Section: Introductionmentioning

confidence: 90%

“…Given the 3.6 sr field of view of STARE2 (Bochenek et al 2020b) and the fact that a single magnetar radio burst has been detected during the ∼300day operating period of the experiment, we estimate the rate of SGR 1935+2154-like magnetar radio bursts (taking the number of active magnetars in the Galaxy to be N = 29; Olausen & Kaspi 2014) to be [ ] l Î´-0.36, 80 10 mag 2 magnetar -1 yr -1 at 95% confidence (assuming Poisson statistics; Gehrels 1986). 11 The radio burst activity (repetition) rate of SGR1935 estimated above is plotted in Figure 3 in comparison to cosmological FRBs.…”

Section: Rates: a Single Magnetar Population?mentioning

confidence: 99%

“…sh and the external density of the upstream baryonic shell at this location, n ext , are given by In the above, we adopt the STARE2 fluence and burst duration (Bochenek et al 2020b) and express the results as a function of the maser efficiency =…”

Section: Baryonic Shellmentioning

confidence: 99%

“…, where we have normalized to a distance of´d 10 kpc 10 and adopted the 1.5 MJy ms fluence and » BW 250 MHz bandwidth of STARE2 (Bochenek et al 2020b(Bochenek et al , 2020c. 8 The radio burst of SGR 1935+2154 is thus within a factor of ∼10 of the lowestenergy burst observed from any cosmological FRB of known distance to date, »5 10 erg 35 (Marcote et al 2020).…”

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confidence: 99%

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Implications of a Fast Radio Burst from a Galactic Magnetar

Margalit

Beniamini

Sridhar

et al. 2020

ApJL

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A luminous radio burst was recently detected in temporal coincidence with a hard X-ray flare from the Galactic magnetar SGR 1935+2154with a time and frequency structure consistent with cosmological fast radio bursts (FRBs) and a fluence within a factor of 10 of the least energetic extragalactic FRB previously detected. Although active magnetars are commonly invoked FRB sources, several distinct mechanisms have been proposed for generating the radio emission that make different predictions for the accompanying higher-frequency radiation. We show that the properties of the coincident radio and X-ray flares from SGR 1935+2154, including their approximate simultaneity and relative fluence~-E E 10 radio X 5 , as well as the duration and spectrum of the X-ray emission, are consistent with extant predictions for the synchrotron maser shock model. Rather than arising from the inner magnetosphere, the X-rays are generated by (incoherent) synchrotron radiation from thermal electrons heated at the same internal shocks that produce the coherent maser emission as ultrarelativistic flare ejecta collides with a slower particle outflow (e.g., as generated by earlier flaring activity) on a radial scale of~10 11 cm. Although the rate of SGR 1935+2154-like bursts in the local universe is not sufficient to contribute appreciably to the extragalactic FRB rate, the inclusion of an additional population of more active magnetars with stronger magnetic fields than the Galactic population can explain both the FRB rate and the repeating fraction, but only if the population of active magnetars are born at a rate that is at least 2 orders of magnitude lower than that of the SGR 1935+2154-like magnetars. This may imply that the more active magnetar sources are not younger magnetars formed in a similar way to the Milky Way population (e.g., via ordinary supernovae) but are instead formed through more exotic channels, such as superluminous supernovae, accretion-induced collapse, or neutron star mergers.

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Section: Introductionmentioning

confidence: 90%

Section: Rates: a Single Magnetar Population?mentioning

confidence: 99%

Section: Baryonic Shellmentioning

confidence: 99%

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confidence: 99%

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Implications of a Fast Radio Burst from a Galactic Magnetar

Margalit

Beniamini

Sridhar

et al. 2020

ApJL

156

123

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“…Although somewhat constraining, GBTrans was not designed with this putative population in mind. Currently, the best limits on Galactic FRB rates come from the STARE2 experiment (Bochenek et al, 2020) with R < 40 FRBs per sky per year.…”

Section: Gbtrans Constraints On Galactic Frbsmentioning

confidence: 99%

Searches for Fast Radio Bursts

Golpayegani¹

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Searches for Fast Radio Bursts Golnoosh Golpayegani Following the discovery of fast radio bursts (FRBs) in 2007, astronomers have entered a new era in astronomy in which understanding the nature of these type of radio transients is one of the most important modern astronomy questions. In this thesis I detail our current state of knowledge in this rapidly evolving field and describe real-time search systems designed to find FRBs using the 20-meter radio telescope at the Green Bank Observatory and the Arecibo L-band Feed Array (ALFA) receiver of the Arecibo 300-meter telescope in Puerto Rico. These experiments are called GBTrans and AL-FABURST, respectively. I give details of the observing systems and report on the non-detection of FRBs for both surveys. GBTrans is sensitive enough to detect approximately half of all currently known FRBs while ALFABURST is sensitive enough to detect almost all of the current FRB population. I estimate that GBTrans survey probed redshifts out to about 0.3 corresponding to an effective survey volume of around 124,000 Mpc 3. Assuming a constant density for sources per unit co-moving volume and considering the possibility of detecting bright FRBs in the sidelobes of the ALFA beams, I estimate ALFABURST probed redshifts out to about 3.5. Based on this, the expected event rate would be at most two FRBs per year at the 99% confidence level. Modeling the FRB rate as a function of fluence, F , as a power law with F −α , I constrain the index α < 2.5 at the 90% confidence level based on the GBTrans results. A number of pulses from previously known pulsars were detected in both the GBTrans and ALFABURST surveys which provided excellent verification on the survey sensitivity used to compute the effective volumes quoted above. One Galactic transient, J1845+00, was found in the ALFABURST survey. This is most likely a member of the rotating radio transient (RRAT) population. It has so far not been seen in follow-up observations. Eight further single-pulse candidates from ALFABURST are also reported. At the time of writing, due to incomplete metadata records, the positions of these sources are not well enough known to allow further follow-up. Future observations with ALFABURST are anticipated in the coming year. Finally, I also describe preliminary observations from an Arecibo survey of gamma-ray burst sources. Dedication To my parents, Minoo Tayebi and Hadi Golpayegani: because I owe it all to you. iii Undertaking this PhD has been truly a life-changing challenge for me and this dissertation would not have been completed without the support and guidance that I received from many people. I would like to pay my deepest gratitude to my dear advisor, Dr. Duncan Lorimer. His never-ending support and encouragement started from day one, when he kindly responded to my very first inquiry email from Iran and since then, he has always been there for me whenever I needed help and patiently kept me motivated. I definitely could never find a better advisor both in immense knowledge and being a wonderful human ...

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