PoS(ICRC2021)857 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Cosmic Ray Conference Ray Cosmic ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY https://pos.sissa.it/ ONLINE on behalf of the VERITAS Collaboration ∗ 0, [email protected] International Cosmic Ray Conference (ICRC 2021) Presenter ∗ th Fast radio burst (FRBs) are an excitingThe class recent of development bright, of extragalactic, millisecond large radio field-of-viewthe transients. (FOV) number radio of identified telescopes single has burst and caused repeatingwavelength a FRBs. follow-up to rapid search This for has rise the allowed potential for in counterparts the predicted extensive multi- byobservations theoretical of models. similar radio New transients in Galactic magnetars liketo SGR motivate the 1935+2154 search have for continued rapid optical and very-high-energy (VHE, >1002016 GeV) counterparts. VERITAS has Since engaged in an FRBVHE observing campaign emission to search from for multiple the promptobservations repeating optical, of and FRBs. five repeating sources We including presentby the data these CHIME taken radio new simultaneously telescope. results with bursts from observed VERITAS Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada E-mail: Copyright owned by the author(s) under the terms of the Creative Commons 0 © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 37 July 12th – 23rd, 2021 Online – Berlin, Germany (a complete list of authors can be found at the end of the proceedings) Matthew Lundy Gamma-ray and Optical Observations of RepeatingRadio Fast Bursts with VERITAS PoS(ICRC2021)857 ◦ Matthew Lundy ms duration radio bursts, occurring ∼ [19]. The localization of bursts is of 0 20 − 0 40 bursts were discovered within the first decade 2 80 ∼ in the East/West (due to the significant frequency and mJy - 100 Jy [1]), ◦ 5 50 . 2 − 3 . 1 per day [4], the rapid nature of these transients and the small field-of-view (FOV) of 3 ). CHIME monitors a frequency range from 400 MHz to 800 MHz and the beam width ◦ 10 Multi-wavelength searches are critical for validating the predictions of many theoretical pro- Due to the high bolometric luminosity of these sources, gamma-ray emission has been expected The CHIME radio telescope is located at the Dominion Radio Observatory near Penticton, Fast Radio Bursts (FRBs) are bright ( 11 ∼ FWHM varies as a function of the frequency from declination dependence) [20]. ThisFRB combined with detection CHIME’s instrument geographic will positionof means monitor that the the entire Northern sky every day (above a declination in the North/South direction and genitor models. To date there has beenan no extra-galactic unambiguous FRB. multi-wavelength counterpart An observed for excitinghas recent provided observation some of of the FRB-like first14]. pulses evidence from supporting Although the SGR these class 1935+2154 of shortsource, magnetar FRB-like models were pulses, for 3 measured FRBs orders simultaneously [12, of13, withpulses, magnitude X-ray there more pulses still luminous from remains than the an typical “energyand Soft gap” the Gamma-ray of weakest Repeater approximately FRBs (SGR) 2 [15]. ordersdiscrepancy of It and magnitude is the between multiwavelength still SGRs implications unclear, of in this the difference. magnetar model, whatby accounts some for models and the VHE large neutrino emission hasCherenkov also been Telescopes theorized (IACTs) [16, like].17 VERITAS Imaging are Atmospheric addition uniquely to poised the to high-energy take capabilities,IACTs an advantage ideal the instrument of to rapid this. investigate the photosensors rapidproceedings optical and In emission we large from report these mirror sources on [18]. area the InFRBs. also status these of make We a will parallel optical/VHE presentdiscuss program results the at status of VERITAS of VERITAS investigating the observations 2021 of observations as 5 well repeaters as VERITAS in future the plans. 20202. season and Instrumentation British Columbia, Canada [19]. Thein telescope the is the composed N/S of direction. four 20 A m linear by array 100 of m 256 dishes dual-polarization aligned antennas monitor a FOV of 120 of study [5].the The measured arrival number of of bothfrom large the non-repeating FOV Canadian and Hydrogen radio repeating Intensity survey Mapping FRBsincreasing Experiment telescopes [6]. the (CHIME) known have 535 population In caused bursts by were the a a published, the most factor past massive of recent year four rise catalog due [7]. to in Many CHIMEM81 notable [8], and FRBs a other have periodic also efforts, repeating emerged including in FRBrise an [9], of FRB and CHIME thirteen localized in well to the localized a FRBemerge FRBs globular field that (such cluster were has as in previously also [2, unfeasible allowed10, due for11 ]). to many The the novel multiwavelength rarity opportunities and to sporadic nature of these transients. in extra-galactic environments [2], fromof an the unknown fundamentals class of of progenitor FRBsis [3]. see Petroff, For 2019 a [1]. recenttraditional review Although radio the telescopes estimated meant all-sky that rate only of FRBs VERITAS FRB 1. Introduction PoS(ICRC2021)857 nm. Matthew Lundy 350 ∼ in longitude, if VERITAS ◦ 25 minutes. 3 ∼ pixel field of view, matching the size of the optical point minutes. When VERITAS takes targeted observations of ◦ 30 15 . − 0 5 ∼ minutes past culmination, they will be transiting through the CHIME field of 30 ∼ The VERITAS observatory consists of four 12-meter diameter telescopes located at the Fred The relative geographic location of CHIME and VERITAS allows for a unique monitoring FRB repeaters have been selected for monitoring based on factors that maximize the potential For the 2019 season, FRB repeaters were added to the campaign as they were discovered, Traditionally only the triggered photomultiplier tube (PMT) pulses are saved for shower recon- spread function of the telescope [21].voltage data Attached logger to with these the is ability ation. to commercial sample Changing DATAQ DI-710-ELS the configurations PMT DC can signal improve at thethe a field timing rate of resolution of view of 4,800 being the monitored Hz telescope as atFRB while the 14 observations sacrificing sample use bit rate an resolu- is updated divided configuration amongpixel, where the are two monitored monitored pixels, pixels. on a three central Recent telescopes. pixelfield and The a of final background view, telescope selected monitors four to pixelskHz, isolate that whereas span background the a signals. other wider three Thisare telescopes sensitive telescope sample from at samples approximately a 250 at higher nm a rate to cadence 550 of of nm 2.4 with 1.2 kHz. the The peak sensitivity VERITAS PMTs at Lawrence Whipple Observatory, inobserve Amado, gamma-rays in Arizona, the very-high-energy USA (VHE) regime,, [21 rays between 85 are22]. GeV and measured 30 through Gamma- TeV. VERITAS observationsgamma-ray is of photons designed Cherenkov in to light the produceddetection atmosphere. in of a the The source particle at gamma-ray cascades 10% sensitivity of of the of Crab VERITAS flux allows in for the campaign. Since the sites of the two telescopes are only separated by 8.7 VHE and optical emission. Thea repeaters summary observed up of until the summer30-minute observations 2020 exposures are presented but presented in beginning here1. in Table with observed 2019 observations Observations the were prior source modified to while such"ON" that 2019 it mode, VERITAS were was where only taken transiting the telescope in the FOV is CHIME centered FOV. on These the observations source. werewithout taken any in discrimination.of In observing later a seasons repeaters multiwavelength counterpart. were selected to We optimize sought the to likelihood select a mixture of repeaters with VERITAS FRB a comparable magnitude but theside exact lobe structure contamination. is complicated due to the presence of factors like observes sources repeaters it guarantees simultaneous radio dataother high during energy the follow-up efforts gamma-ray of observations. FRBs,overlap that with In carry the contrast arrival a to time delay, the of gamma-ray the and FRBthe optical detection event. and data also will have several minutes of data surrounding 3. Repeater Observations struction but upgrades in 2016 andin 2018 a subset have allowed of for pixels. VERITAS This tocamera allows monitor while for the optical normal DC photometry gamma-ray to light observations be level areof done underway. 499 with photomultiplier a The tubes portion VERITAS with of camera a the is VERITAS composed view. The duration of an object’sof transit the through source the and can CHIME range FOV from is dependent on the declination PoS(ICRC2021)857 soft ) f Matthew Lundy 4 VERITAS Observation Log for FRB repeaters. The significances are calculated using Equation 17 For runs that lie within 1 hour of a known repeater burst, the events in the ON region are If a repeater has been localized by a smaller field of view telescope then an optical analysis In addition to the previously reported limits from bursts from FRB 121102 [23], VERITAS has An analysis of the gamma-ray data was performed using the Ring Background Method (RBM), FRB NameFRB 121102FRB 180814.J0422+73 1013.22FRB 180916.J0158+65 397.45FRB 181030.J1054+73 Exposure (min) 226.26FRB 1216.64 190116.J1249+27 On Counts 966 45.00 Off Counts 522 Significance( 1681 277 8955 111 4907 14134 2650 -0.62 768 -0.61 -0.06 -0.33 0.83 extracted from the runs and anlogarithmically average spaced background windows rate of is 0.1 extracted s, from 10 theof s, significant RBM 100 emission analysis. s, during Then, and the run 1000 coincident scorrected with are the assessed burst. arrival to time search The of for the arrival evidence barycentric,2.Table times dispersion- No of significant the excess is near-by seen events in foris any FRB shown of in J180916.J0158+65 the1. Figure are windows surrounding shown these in bursts, one of which can be performed at the locationVERITAS means of that the source source. confusion Prior andof large to most non-astrophysical localization, transients backgrounds the ambiguous. leaves large the optical nature pixel size of sources (a spectral index -3.5that to -4.0) was were performed applied was tocumulative the an exposure. data. integrated For search The all for events repeaters,VERITAS emission and were the the around smoothed first results analysis the using are shown the source inFRB2. Figure gamma-ray location position, point the No using significant values spread excess the of was function which foundthe are at of repeaters. shown the in most1, likely Table or within the larger error region of any of also collected data duringfrom three the contemporaneous repeater or FRB 180916.J0158+65. near-contemporaneous The bursts properties with of CHIME these bursts are shown in2. Table 4. Analysis and Preliminary Results where observations were taken in "ON"from mode a and ring backgrounds around are the estimated source using location a [24]. events A taken series of gamma-hadron cuts that optimized for low dispersion measure (the integratedburst electron rates density in which CHIME, acts lowgamma-ray as VERITAS energy a zenith threshold), proxy high angles for CHIME at distance),precise signal-to-noise culmination high localization. ratio (which (a lowers Notable rough the repeaters proxy VERITAS this like for evaluation. fluence), FRB and 121102 were dropped in later seasons based on VERITAS FRB Table 1: in [25] at the best fit position of the FRB. PoS(ICRC2021)857 Matthew Lundy Duration of VERITAS Observation (s) 5 tion (UTC) //www.chime-frb.ca/repeaters Burst analysis time series for the simultaneous FRB. A gray histogram of the number of gamma-ray Fast radio bursts from FRB J180916.J0158+65 with CHIME and VERITAS overlap. All CHIME During the 2020/2021 season we updated our repeater target list based on new available VERITAS begun monitoring VOEvents broadcast by CHIME [26] towards the end of March Time of CHIME FRB (UTC)2019-12-18 04:09:27.633 VERITAS Start of2019-10-30 07:33:56.995676 Observa- 2020-01-20 01:49:14.068 2019-10-30 2019-12-18 07:15:37.69 04:01:59.29 2020-01-20 02:03:01.38 811 900 1800 Figure 1: repeaters from CHIME. AData total were of collected 49.3 on hours181119.J12+65, previous of FRB repeaters data 190303.J1353+48, as FRB was 190212.J18+81, well collected and asfrom as M the the 81. a CHIME addition repeater Coordinates part catalog of were of at taken obtained FRB the this by 190213.J02+20, most a campaign. probable FRB small location FOV if radiopresented no telescope. here precise in localization This a had data future been will publication. be combined Additional bursts with will the also preliminary5.2 be results presented. VOEvents 2021. CHIME releases a realtimetheir stream Comet of event FRB broker. candidates VOEvents inlocalized offer VOEvent repeaters. the format to opportunity subscribers for To of realtime date follow-up the of rate not precisely of FRB-like events has made realtime follow-up of events counts is shown. Burstwindows in are Black shown points in yellow show and the red arrival respectively. time of the gamma-like events. The5. 10 and 100 Discussion s and Future Plans 5.1 2020/2021 Season VERITAS FRB Table 2: information taken from

PoS(ICRC2021)857

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Matthew Lundy color The 190116.J1249+27. FRB e) 181030.J1054+73, FRB d) 180916.J0158+65, FRB c) 180814.J0422+73, FRB b) 121102,

EIA am-a infiac ascnee ntebs tpsto fteFB.TeFB hw r;a FRB a) are; shown FRBs The FRBs. the of position fit best the on centered maps significance gamma-ray VERITAS iue2: Figure 6 impractical. The systemcomparing is the currently live integrated VERITAS pointing asbeen a to a burst the passive whose location error monitora of region with short-duration coincides events campaign a with and of the local sending follow-up, FOV but eventof of an a VERITAS. VERITAS. parser constant alert An A integration assessment if future of of plan events there this into may possibility is the include in GRB underway. pipeline VERITAS FRB PoS(ICRC2021)857 , : . . doi arXiv . arXiv: . arXiv: . 1701.01100 1906 . 05878 arXiv e-prints Matthew Lundy . . arXiv: . arXiv: Science China Physics, 10.1007/s11433- 020- . : doi 2106.04352 [astro-ph.HE] 2001.10275 [astro-ph.HE] 10.1093/mnras/stx3074 : doi 10.3847/2041-8213/ab4a80 . arXiv: 2105.11445 [astro-ph.HE] : doi 1701.01098 [astro-ph.HE] . 7 1904.07947 [astro-ph.HE] . arXiv: 10.3847/2041- 8213/834/2/L7 : doi https://veritas.sao.arizona.edu/ . arXiv: . . 64.4, 249501 (Apr. 2021), p. 249501. 10 . 1146 / annurev - astro - 091918 - 104501 10.1038/s41586-020-2398-2 : : doi doi . . 2101.04907 [astro-ph.HE] 10.1038/nature20797 : doi . arXiv: , arXiv:2106.04352 (June 2021), arXiv:2106.04352. arXiv: [astro-ph.HE] Mechanics, and Astronomy 1661-7 and their follow-up”. 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Acknowledgments For VERITAS acknowledgments see: References VERITAS FRB 5.3 Conclusion Additionally this research was undertaken thanks inExcellence part Fund to through funding the from the Arthur Canada B.tute. First McDonald Research Canadian Thanks Astroparticle should Physics also Research be Insti- given to the whole CHIME FRB team at the McGill Space Institute. PoS(ICRC2021)857 . . : . . . doi . arXiv arXiv . 34th Inter- 0709.4233 2005.10324 1803 . 11235 Matthew Lundy , arXiv:1710.08155 . arXiv: . arXiv: 25.6 (July 2006), pp. 391– . International Cosmic Ray Con- 10.1038/s41550-019-0741- 10.3847/2041-8213/aba2cf 10.1126/science.aaw5903 1702.04728 [astro-ph.IM] : : arXiv e-prints : 2005.05283 [astro-ph.HE] . . 2005.10828 [astro-ph.HE] 1307.4924 [astro-ph.HE] astro-ph/0604119 [astro-ph] doi doi doi . Vol. 36. International Cosmic Ray Con- . arXiv: . arXiv: . arXiv: Astroparticle Physics . . Vol. 34. International Cosmic Ray Conference. 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Kleiner Institute of Physics 18 23 Matthew Lundy , M. Nievas-Rosillo Department of Physics , C. Giuri 21 19 14 , E. Pueschel 15 , D. Kieda 2 , A. J. Chromey 6 Department of Physics, California , D. Nieto , G. H. Sembroski 5 12 19 , R. R. Prado 15 , G. H. Gillanders , , M. Kertzman 13 23 20 , R. Mukherjee , M. Santander 10 , J. L. Christiansen 14 5 15 , A. Gent Physics Department, McGill University, Montreal, QC , M. Pohl 12 , P. Kaaret Department of Astronomy and Astrophysics, 525 Davey 16 15 Department of Physical Sciences, Munster Technological 8 19 Department of Physics and Astronomy, DePauw University, 24 Department of Physics and Astronomy, University of Iowa, 2 20 School of Physics, University College Dublin, Belfield, Dublin , I. Sadeh 9 , P. Moriarty 22 9 , M. Capasso , W. Jin 4 9 1 , A. Furniss , K. Pfrang School of Physics, National University of Ireland Galway, University 11 20 14 Harvard & Smithsonian, Cambridge, MA 02138, USA Department of Physics and Astronomy, Barnard College, Columbia Uni- | 5 , and T. J. Williamson 17 School of Physics and Center for Relativistic Astrophysics, Georgia Institute , J. L. Ryan 13 3 , S. Patel Department of Physics and Astronomy, Purdue University, West Lafayette, IN 15 25 , L. Fortson , C. E McGrath , J. H. Buckley 1 10 15 , T. B. Humensky Institute of Particle and Cosmos Physics, Universidad Complutense de Madrid, 28040 18 21 , E. Roache 1 , D. A. Williams , A. Brill 7 , S. R. Patel 3 , G. Maier 13 16 , B. Hona , G. M. Foote Center for Astrophysics 5 3 10 , D. Ribeiro 24 , W. Benbow , Q. Feng , A. Weinstein , A. N. Otte , M. Lundy Physics Department, California Polytechnic State University, San Luis Obispo, CA 94307, USA 2 9 DESY, Platanenallee 6, 15738 Zeuthen, Germany 6 , J. Holder 22 22 14 15 17 Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 17 Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA 22 , A. Archer 18 1 , R. A. Ong Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, , K. A. Farrell , P. T. Reynolds , M. J. Lang , O. Hervet 16 8 10 16 16 16 , V. V. Vassiliev School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA 15 11 Physics Department, Columbia University, New York, NY 10027, USA and Astronomy, University of Potsdam,University, 14476 Bishopstown, Potsdam-Golm, Cork, Germany T12 P928,47907, USA Ireland Madrid, Spain D. Tak Van Allen Hall, Iowa City, IA 52242, USA versity, NY 10027, USA 95064, USA K. Ragan 1 Physics, Washington University, St. Louis, MO 63130, USA of Physics and Astronomy, IowaLab, State Pennsylvania State University, University, Ames, University Park, IA PA 50011, 16802, USA USA H3A 2T8, Canada and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA Greencastle, IN 46135-0037, USA Road, Galway, Ireland S. O’Brien 4, Ireland USA State University - East Bay, Hayward,of CA Technology, 94542, 837 USA State Street NW, Atlanta, GA 30332-0430 VERITAS FRB Full Authors List: VERITAS Collaboration C. B. Adams A. Falcone D. Hanna S. Kumar