Deep Simultaneous Limits on Optical Emission from FRB 20190520B by 24.4 fps Observations with Tomo-e Gozen

Niino, Yuu; Doi, Mamoru; Sako, Shigeyuki; Ohsawa, Ryou; Arima, Noriaki; Jiang, Ji-an; Tominaga, Nozomu; Tanaka, Masaomi; Li, Di; Niu, Chenhui; Thai, Chao-Wei; Kobayashi, Naoto; Takahashi, H.; Kondo, Sohei; Mori, Yuki; Aoki, Tsutomu; Arimatsu, Ko; Kasuga, Toshihiro; Okumura, Shin-ichiro

doi:10.3847/1538-4357/ac6be8

Cited by 10 publications

(8 citation statements)

References 45 publications

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“…Our nearly simultaneous Binospec limit would be the deepest if it were indeed simultaneous given the aforementioned shutter timing uncertainty. We stress that these fluence ratio limits are lower than the observed values for the Crab and Geminga pulsars (e.g., Danilenko et al 2011;Bühler & Blandford 2014), which may suggest a different emission mechanism (although pulsars with lower fluence ratios have also been observed; see, e.g., Niino et al 2022 for a discussion for FRB 20190520B in this context).…”

Section: Optical-to-radio Flux and Fluence Ratio Limitsmentioning

confidence: 62%

“…We find that these observations have the potential to better constrain optical emission from FRBs compared to the bulk of serendipitous archival observations. In particular, based on the experience and constraining limits from our KeplerCam, LCO, and Binospec observations, as well as previous targeted observations (e.g., Hardy et al 2017;MAGIC Collaboration et al 2018;Kilpatrick et al 2021;Niino et al 2022), we advocate for an approach of simultaneous monitoring of FRBs during CHIME (or other facility) observing windows, especially when repeating FRBs are in a particularly active phase.…”

Section: Discussionmentioning

confidence: 91%

“…On a shorter timescale, several targeted high-speed simultaneous observations-by ULTRASPEC on the 2.4 m Thai National Telescope (TNT; Tulloch & Dhillon 2011;Dhillon et al 2014) for FRB 20121102A (Hardy et al 2017); the central pixel of the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescopes (Lucarelli et al 2008;Hassan et al 2021) for FRB 20121102 (MAGIC Collaboration et al 2018); and Tomo-e Gozen on the Kiso 105 cm Schmidt telescope (Sako et al 2018) for FRB 20190520B (Niino et al 2022)-span a temporal range ∼1-10 ms before/after radio bursts with a luminosity upper limit range of ∼10 45 -10 47 erg s −1 in a single exposure (longer and deeper stacked exposures are also shown in Figure 2). In the ZTF archival search, we also find a simultaneous 30 s r-band observation of FRB 20121102A with a luminosity limit of ∼6 × 10 43 erg s −1 .…”

Section: Optical Luminosity Limitsmentioning

confidence: 99%

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Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts

Hiramatsu

Berger

Metzger

et al. 2023

ApJL

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We present the largest compilation to date of optical observations during and following fast radio bursts (FRBs). The data set includes our dedicated simultaneous and follow-up observations, as well as serendipitous archival survey observations, for a sample of 15 well-localized FRBs: eight repeating and seven one-off sources. Our simultaneous (and nearly simultaneous with a 0.4 s delay) optical observations of 13 (1) bursts from the repeating FRB 20220912A provide the deepest such limits to date for any extragalactic FRB, reaching a luminosity limit of ν L ν ≲ 1042 erg s−1 (≲2 × 1041 erg s−1) with 15–400 s exposures; an optical-flux-to-radio-fluence ratio of f opt/F radio ≲ 10−7 ms−1 (≲10−8 ms−1); and a flux ratio of f opt/f radio ≲ 0.02–≲2 × 10−5 (≲10−6) on millisecond to second timescales. These simultaneous limits provide useful constraints in the context of FRB emission models, such as the pulsar magnetosphere and pulsar nebula models. Interpreting all available optical limits in the context of the synchrotron maser model, we find that they constrain the flare energies to ≲1043–1049 erg (depending on the distances of the various repeating FRBs, with ≲1039 erg for the Galactic SGR 1935+2154). These limits are generally at least an order of magnitude larger than those inferred from the FRBs themselves, although in the case of FRB 20220912A our simultaneous and rapid follow-up observations severely restrict the model parameter space. We conclude by exploring the potential of future simultaneous and rapid-response observations with large optical telescopes.

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Section: Optical-to-radio Flux and Fluence Ratio Limitsmentioning

confidence: 62%

Section: Discussionmentioning

confidence: 91%

Section: Optical Luminosity Limitsmentioning

confidence: 99%

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Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts

Hiramatsu

Berger

Metzger

et al. 2023

ApJL

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“…The unprecedented sensitivity of the Five-hundred-meter Aperture Spherical Telescope enables detailed measurements of burst energy distributions (Li et al 2021), which informs possible progenitor models and emission mechanisms through the determination of minimum and maximum characteristic energies. 1 Despite coordinated efforts, a prompt multiwavelength counterpart to a repeater burst has not been detected (e.g., Hardy et al 2017;Scholz et al 2020;Tavani et al 2020;Niino et al 2022).…”

Section: Introductionmentioning

confidence: 99%

CHIME/FRB Discovery of 25 Repeating Fast Radio Burst Sources

Collaboration¹,

Andersen³

et al. 2023

Preprint

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We present the discovery of 25 new repeating fast radio burst (FRB) sources found among CHIME/FRB events detected between 2019 September 30 and 2021 May 1. The sources were found using a new clustering algorithm that looks for multiple events co-located on the sky having similar dispersion measures (DMs). The new repeaters have DMs ranging from ∼220 pc cm −3 to ∼1700 pc cm −3 , and include sources having exhibited as few as two bursts to as many as twelve. We report a statistically significant difference in both the DM and extragalactic DM (eDM) distributions between repeating and apparently nonrepeating sources, with repeaters having lower mean DM and eDM, and we discuss the implications. We find no clear bimodality between the repetition rates of repeaters and upper limits on repetition from apparently nonrepeating sources after correcting for sensitivity and exposure effects, although some active repeating sources stand out as anomalous. We measure the repeater fraction and find that it tends to an equilibrium of 2.6 +2.9 −2.6 % over our exposure thus far. We also report on 14 more sources which are promising repeating FRB candidates and which merit follow-up observations for confirmation.

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“…For the repeater FRB 20181228, high-time-resolution optical observations have been undertaken, as reported by Hardy et al (2017), with a detection upper limit of 0.33 mJy at an imaging cadence of 70.7 ms. Nino et al (2022) used the Tomo-e-Gozen telescope to observe FRB 20190520B at 24.4 frames per second (40.9 ms frame duration), at times when radio bursts were detected with the FAST radio telescope. They did not detect any bursts at optical wavelengths, placing a best 5σ limit of 0.015 Jy ms.…”

Section: Introductionmentioning

confidence: 99%

A Search of TESS Full-frame Images for an Optical Counterpart of the Repeating FRB 20180916B

Tingay¹

2022

ApJL

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Recently, an association between an optical transient, AT2020hur, and a repeating fast radio burst, FRB 20180916b, has been suggested, based on a strong positional coincidence on the sky and the temporal coincidence with one of the fast radio burst’s activity periods (∼6 days duration every ∼16 days). This suggestion is explored further and tested in this paper, utilizing full-frame images from the Transiting Exoplanet Survey Satellite (TESS) across three of its observing periods in 2019 and 2020 (Sectors 18, 24, and 25). The discovery observations of AT2020hur took place between Sectors 18 and 24, within 5 days of the commencement of Sector 24 observations. The TESS observations cover at least six activity periods for the FRB. Thus, the TESS data provide excellent temporal coverage close in time to the discovery of AT2020hur and at known times of FRB activity and radio detection. From the TESS data, no evidence is found for repeating optical transients with the suspected emission timescale of ⪆1000 s.

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Deep Simultaneous Limits on Optical Emission from FRB 20190520B by 24.4 fps Observations with Tomo-e Gozen

Cited by 10 publications

References 45 publications

Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts

Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts

CHIME/FRB Discovery of 25 Repeating Fast Radio Burst Sources

A Search of TESS Full-frame Images for an Optical Counterpart of the Repeating FRB 20180916B

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