Fast radio bursts FRBs are flashes of unknown physical originSUP1SUP. The majority of FRBs have been seen only once although some are known to generate multiple flashesSUP23SUP. Many models invoke magnetically powered neutron stars magnetars as the source of the emissionSUP45SUP. Recently the discoverySUP6SUP of another repeater FRB 20200120E was announced in the direction of the nearby galaxy M81 with four potential counterparts at other wavelengthsSUP6SUP. Here we report observations that localized the FRB to a globular cluster associated with M81 where it is 2 parsecs away from the optical centre of the cluster. Globular clusters host old stellar populations challenging FRB models that invoke young magnetars formed in a corecollapse supernova. We propose instead that FRB 20200120E originates from a highly magnetized neutron star formed either through the accretioninduced collapse of a white dwarf or the merger of compact stars in a binary systemSUP7SUP. Compact binaries are efficiently formed inside globular clusters so a model invoking them could also be responsible for the observed bursts.
['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Cosmology and Nongalactic Astrophysics']
A repeating fast radio burst source in a globular cluster
{'No Header': '26  \n4  \n25', 'A repeating fast radio burst source in a globular cluster': "F. Kirsten 1 , B. Marcote 2 , K. Nimmo 3,4 , J. W. T. Hessels 4,3 , M. Bhardwaj 5,6 , S. P. Tendulkar 7,8 , A. Keimpema 2 , J. Yang 1 , M. P. Snelders 4 , P. Scholz 9 , A. B. Pearlman 5,6,10,11,12 , C. J. Law 13,14 , W. M. Peters 15 , M. Giroletti 16 , Z. Paragi 2 , C. Bassa 3 , D. M. Hewitt 4 , U. Bach 17 , V. Bezrukovs 18 , M. Burgay 19 , S. T. Buttaccio 20 , J. E. Conway 1 , A. Corongiu 19 , R. Feiler 21 , O. Forss'en 1 , M. P. Gawro'nski 21 , R. Karuppusamy 17 , M. A. Kharinov 22 , M. Lindqvist 1 , G. Maccaferri 16 , A. Melnikov 22 , O. S. Ould-Boukattine 4 , A. Possenti 19,23 , G. Surcis 19 , N. Wang 24 , J. Yuan 24 , K. Aggarwal 25,26 , R. Anna-Thomas 25,26 , G. C. Bower 27 , R. Blaauw 3 , S. Burke-Spolaor 25,26,28 , T. Cassanelli 9,29 , T. E. Clarke 15 , E. Fonseca 5,6,25,26 , B. M. Gaensler 9,29 , A. Gopinath 4 , V. M. Kaspi 5,6 , N. Kassim 15 , T. J. W. Lazio 30 , C. Leung 31,32 , D. Z. Li 13 , H. H. Lin 33 , K. W. Masui 31,32 , R. Mckinven 9 , D. Michilli 5,6 , A. Mikhailov 22 , C. Ng 9 , A. Orbidans 18 , U. L. Pen 33,9,28,34 , E. Petro GLYPH<11> 4,5,6,35 , M. Rahman 36 , S. M. Ransom 37 , K. Shin 31,32 , K. M. Smith 34 , I. H. Stairs 38 , and W. Vlemmings 1  \n1 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 439 92, Onsala, Sweden 2 Joint Institute for VLBI ERIC, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands  \n3  \nASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands  \nAnton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH, Amsterdam, The Netherlands  \n5 Department of Physics, McGill University, 3600 rue University, Montr'eal, QC H3A 2T8, Canada  \n6  \nMcGill Space Institute, McGill University, 3550 rue University, Montr'eal, QC H3A 2A7, Canada  \nDepartment of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai, 400005, India  \n8  \nNational Centre for Radio Astrophysics, Post Bag 3, Ganeshkhind, Pune, 411007, India  \n9 Dunlap Institute for Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada 10 Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 11 McGill Space Institute (MSI) Fellow", '12 FRQNT Postdoctoral Fellow': "13 Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1216 E California Boulevard, Pasadena, CA 91125, USA  \n14 Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125, USA  \n15  \nRemote Sensing Division, US Naval Research Laboratory, Washington, DC 20375, USA  \nIstituto Nazionale di Astrofisica, Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna, Italy  \n17  \nMax Planck Institute for Radio Astronomy, Auf dem Heugel 69 53121 Bonn, Germany  \n- 18 Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS), Inzenieru street 101, Ventspils, LV-3601, Latvia\n- 19 Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Cagliari, Via della Scienza 5, I-09047, Selargius, Italy 20 Istituto Nazionale di Astrofisica, Istituto di Radioastronomia Radiotelescopio di Noto, C.da Renna Bassa Loc. Case di Mezzo C.P. 161,\n- 96017, Noto (SR), Italy\n- 21 Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Toru'n, Poland\n- 22 Institute of Applied Astronomy of the Russian Academy of Sciences, Kutuzova Embankment 10, St. Petersburg, 191187, Russia 23 Universit'a di Cagliari, Dipartimento di Fisica, S.P. Monserrato-Sestu Km 0,700 - 09042 Monserrato (CA), Italy  \n24  \nXinjiang Astronomical Observatory, 150 Science 1-Street, Urumqi, Xinjiang 830011, China  \nDepartment of Physics and Astronomy, West Virginia University, P.O. Box 6315, Morgantown, WV 26506, USA  \nCenter for Gravitational Waves and Cosmology, West Virginia University, Chestnut Ridge Research Building, Morgantown, WV 26505,", 'USA': "- 27 Academia Sinica Institute of Astronomy and Astrophysics, 645 N. A'ohoku Place, Hilo, HI 96720, USA 28 Canadian Institute for Advanced Research, CIFAR Azrieli Global Scholar, MaRS Centre West Tower, 661 University Ave. Suite 505, Toronto ON M5G 1M1, Canada\n- 29 David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada 30 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr, Pasadena, CA 91109, USA 31 MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge,\n- MA02139, USA  \n32 Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA 02139, USA 33 Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON, M5S 3H8, Canada 34 Perimeter Institute for Theoretical Physics, 31 Caroline Street North, Waterloo, ON, N2L 2Y5, Canada 35  \n- Veni Fellow  \n36 Sidrat Research, PO Box 73527 RPO Wychwood, Toronto, ON M6C 4A7, Canada  \n37 National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USA  \n38 Dept. of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1  \n7  \n16  \nFast radio bursts (FRBs) are exceptionally luminous flashes of unknown physical origin, reaching us from other galaxies 1 . Most FRBs have only ever been seen once, while others flash repeatedly, though sporadically 2,3 . Many models invoke magnetically powered neutron stars (magnetars) as the engines producing FRB emission 4,5 . Recently, CHIME / FRB announced the discovery 6 of the repeating FRB 20200120E, coming from the direction of the nearby grand design spiral galaxy M81. Four potential counterparts at other observing wavelengths were identified 6 but no definitive association with these sources, or M81, could be made. Here we report an extremely precise localisation of FRB 20200120E, which allows us to associate it with a globular cluster (GC) in the M81 galactic system and to place it GLYPH<25> 2 pc o GLYPH<11> set from optical center of light of the GC. This confirms 6 that FRB 20200120E is 40 times closer than any other known extragalactic FRB. Because such GCs host old stellar populations, this association strongly challenges FRB models that invoke young magnetars formed in a core-collapse supernova as powering FRB emission. We propose, instead, that FRB 20200120E is a highly magnetised neutron star formed via either accretion-induced collapse of a white dwarf or via merger of compact stars in a binary system 7 . Alternative scenarios involving compact binary systems, e GLYPH<14> ciently formed inside globular clusters, could also be responsible for the observed bursts.  \nM81 is one of the most massive nearby galaxies, at 3.6 Mpc 8 . We targeted the previously best-known position 6 of FRB 20200120E several times during February to May 2021 with an array composed of up to eleven radio telescopes that are part of the European Very Long Baseline Interferometry (VLBI) Network (EVN; see Methods). Weobserved at a central radio frequency of GLYPH<24> 1 : 4 GHz and recorded raw voltages from all telescopes. At E GLYPH<11> elsberg and at the Sardinia Radio Telescope (SRT), we collected data in parallel using pulsar data recorders (Methods).  \nIn total we detected five bursts from FRB 20200120E, with dispersion measures close to the previously reported 6 DM = 87 : 8 pc cm GLYPH<0> 3 . Two bursts were detected on 2021 February 20 (called B1 and B2 below), two bursts on 2021 March 7 (B3 and B4), and one burst on 2021 April 28 (B5). Bursts B2-B5 were found by blindly searching both the E GLYPH<11> elsberg voltages and PSRIX 9 data (Methods), while B1 was only detected in the voltage data as it occurred outside the recording times of the PSRIX instrument 10 . In Figure 1 we show the dedispersed dynamic spectra and frequency averaged burst profiles. Burst fluences range from 0 : 13 GLYPH<0> 0 : 71 Jy ms and total burst envelopes span only GLYPH<24> 100 GLYPH<0> 300 µ s (Table 1). A detailed, ultra-high-timeresolution analysis of the burst properties and energetics is presented in a companion paper 10 .  \nCorrelation of the data, in order to produce 'visibilities' for interferometric imaging, was performed at the Joint Institute for VLBI ERIC. To achieve the best-possible sensitivity, we used the coherent-dedispersion mode of the software correlator SFXC 11 , applying DM = 87 : 77 pc cm GLYPH<0> 3 , which we derived from a manual inspection of the bursts (Methods).  \nAfter an initial rough localisation via delay mapping (Methods, accurate to several arcseconds), we individually imaged the five bursts, where each data set spans only the width of each burst in time (Table 1). Given the snapshot nature of the correlations, the rather sparse arrays in each run, and the fact that the bursts only covered a fraction of the observed bandwidth, the images from the individual bursts result in elongated fringe patterns, hindering an individual, unambiguous localisation of each burst at the level of the synthesised beam size (see Figure 2a-d). Therefore, we created a data set that is the combination of the visibilities from all bursts except B1 - as it was too faint to produce a useful image, and we therefore exclude it from the localization analysis. These data allowed us to unambiguously pinpoint the position of FRB 20200120E in the field (see Figure 2e,f). The derived coordinates of FRB 20200120E in the International Celestial Reference Frame (ICRF) 12 are RA (J2000) = 9 h 57 m 54 : 69935 s GLYPH<6> 1 : 2 mas Dec (J2000) = 68 GLYPH<14> 49 0 0 : 8529 00 GLYPH<6> 1 : 3 mas (see Methods). These coordinates coincide with the location of the globular cluster [PR95] 30244 13 , which is part of the M81 globular cluster system 14 .  \nFigure 3a shows the position of FRB 20200120E with respect to [PR95] 30244 in a combined three-colour Subaru image made with i 0 , r 0 , and g 0 filters mapped to red, green, and blue channels, respectively. The galaxy at the bottom-left of [PR95] 30244 is a background SDSS galaxy at redshift z = 0 : 194, i.e. at a z much larger than the maximum possible 6 value ( z < 0 : 03) based on FRB 20200120E's dispersion measure. We performed radial fits to the brightness distribution of [PR95] 30244 using a Mo GLYPH<11> at profile 15 in both RA and Dec for all three bands after fitting and subtracting a bilinearly varying background (to account for the presence of the background galaxy). The average position of the centroid of [PR95] 30244 is RA (J2000) = 9 h 57 m 54 : 7135 s GLYPH<6> 7 mas, Dec (J2000) = 68 GLYPH<14> 49 0 0 : 766 00 GLYPH<6> 4 mas (statistical), well in agreement with previous measurements 13 and the position of the source in the Gaia Early Data Release 3 Catalogue 16,17 (Methods), in which positions are well aligned with the ICRF 17 .  \nThe centre of the FRB localisation is GLYPH<25> 116 mas o GLYPH<11> -set from the optical centre of light of [PR95] 30244 (Figure 3b, corresponding to GLYPH<25> 54% of its e GLYPH<11> ective radius, Methods). Given the astrometric uncertainty of the FRB  \nlocalisation ( GLYPH<25> 1 : 3 mas) and the optical image registration error with respect to the ICRF ( GLYPH<25> 15 mas; see Methods), we conclude that FRB 20200120E is located significantly ( > 7 GLYPH<27> confidence level) o GLYPH<11> set from the optical centre of light of [PR95] 30244. The optical angular size of [PR95] 30244 (0 : 00 77; Methods) in combination with FRB 20200120E's o GLYPH<11> set from M81 (19.6 0 ) and the number of GCs predicted 18 to be part of the galaxy (300 GLYPH<6> 100), allow us to estimate the probability of chance alignment P cc < 1 : 7 GLYPH<2> 10 GLYPH<0> 4 (Methods). From such a very low P cc value, we conclude that the association of FRB 20200120E and [PR95] 30244 is robust.  \nFigure 4a shows a deep continuum map that was created from the combination of the data of all VLBI observations. We find no persistent source at the location of FRB 20200120E above a 5 GLYPH<27> confidence level (rms background noise level of 10 µ Jy beam GLYPH<0> 1 ). Also shown in Figure 4 are continuum images obtained with the Karl G. Jansky Very Large Array (VLA) at 1 : 5 GHz and at 340 MHz between December 2020 to January 2021 (Methods). These maps have noise levels of 6 : 5 µ Jy beam GLYPH<0> 1 and 320 µ Jy beam GLYPH<0> 1 , respectively. Also here, no persistent source is detected at the position of FRB 20200120E in either of the images. For a 1.5 GHz radio flux density limit of 20 µ Jy (3 GLYPH<27> ) and a distance of 3.6 Mpc, we limit the radio luminosity L GLYPH<23> < 3 : 1 GLYPH<2> 10 23 erg s GLYPH<0> 1 Hz GLYPH<0> 1 . This luminosity limit is GLYPH<24> 10 3 times lower than that of any other extragalactic FRB 19 and almost 10 6 times lower than the radio luminosity of the persistent source in the vicinity of FRB 20121102A 20 .  \nWe find no evidence of an X-ray source at the location of FRB 20200120E in archival Chandra observations (Methods). This results in a 0.5-10 keV luminosity upper limit of 2 GLYPH<2> 10 37 erg s GLYPH<0> 1 (3 GLYPH<27> ) at the distance of 3.6 Mpc. A detailed analysis of ongoing X-ray follow-up observations of the region will be presented in Pearlman et al. (in prep.). Similarly, no sources are reported at the location of M81 in any of the Fermi -LAT catalogues 21 . The nearest catalogued source (at a separation of 52 0 ) is 4FGLJ0955.7 + 6940, known to be associated with M82 22 .  \nWithin the context of FRB models that invoke a young, highly magnetized neutron star (NS) powered primarily by the decay of its magnetic field 4,5 , i.e. a magnetar, it is hard to reconcile FRB 20200120E's association with an old globular cluster using the standard core-collapse supernova formation channel of magnetars. Instead, because of their extreme stellar densities, globular clusters are known to form short-orbital-period binaries at a high specific rate 23-25 . We thus propose that FRB 20200120E is a magnetar formed via accretion-induced collapse (AIC) 26 of a white dwarf (WD) or via merger-induced collapse (MIC) of a WD-WD, NS-WD or NS-NS binary 27-29 -systems that are common in globular clusters and, like  \nFRB 20200120E, are found concentrated towards their core 30 (Methods). The lack of a persistent radio or X-ray source at the position of FRB 20200120E is expected in an AIC / MIC scenario, as any emission generated during collapse fades on short time scales ( < 1 yr) 7 .  \nThe globular cluster host of FRB 20200120E also suggests some alternatives to the magnetar class of FRB models. FRB 20200120E could be a compact binary system -such as a tight WD-NS system in a pre-merger phase or a magnetised NS with a planetary companion 31,32 -in which the bodies are interacting magnetically. Similarly, a binary millisecond pulsar with a strong magnetic field formed via AIC and that was subsequently spun-up via accretion 33,34 could act as an FRB engine. Such a system could also be observable as a low mass X-ray binary (LMXB) 35 , as would an accreting black hole (BH). In such an LMXB model, the radio bursts could be generated via magnetic reconnection in a relativistic jet or where the jet shocks with the surrounding medium and creates a synchrotron maser 36 . Except for the most luminous LMXBs (LX GLYPH<25> 10 38 erg s GLYPH<0> 1 ), our observations cannot rule out such systems. However, none of the GLYPH<24> 200 Galactic LMXBs has been seen to generate FRBs. In some cases, ultraluminous X-ray sources (ULXs) 37 have been shown to be NSs accreting at hyper-Eddington rates 38 , though some may be systems with a more massive BH primary 39 . We note that ULXs have been associated with extragalactic globular clusters 40 but such systems are ruled out by our X-ray limit unless their luminosity varies in time by more than two orders of magnitude. Additionally, the association with a globular cluster rules out a high mass X-ray binary origin of FRB 20200120E and the projected o GLYPH<11> set of GLYPH<25> 2 pc from the centre of light of [PR95] 30244 excludes the association of FRB 20200120E with, e.g., a massive ( & 10M GLYPH<12> ) stellar mass BH or a putative intermediate mass black hole at the core of [PR95] 30244.  \nThe association of FRB 20200120E with a globular cluster adds to the diversity of environments in which repeating FRBs have been found. While FRB 20121102A resides in a dwarf galaxy 41 , the host of FRB 20180916B is a spiral galaxy 19 and FRB 20201124A was localised to a massive star forming galaxy 42 . Previously localised repeaters have been associated with nearby star forming regions 43-46 , favouring the core-collapse supernova channel for the formation of a young magnetars, as the rate of AIC and MIC is much lower. The lack of a persistent radio source for all but FRB 20121102A may suggest a range in the possible ages of such magnetars. In a globular cluster environment, however, the recent core-collapse of a massive star is very unlikely. Thus, this suggests a diversity in formation channels for magnetars as FRB engines.  \nFigure 1: Dispersion-corrected time series and dynamic spectra of the five FRB 20200120E bursts Frequencyaveraged time series of the bursts are displayed in panels a-e . The top right corner of each panel shows the burst name used in this work. The blue-coloured bars highlight the GLYPH<6> 2 GLYPH<27> burst width used to measure the burst fluence. The dynamic spectra of each burst are shown in panels f-j . The red marks represent the edges of the subbands. Data that have been removed due to contamination by radio frequency interference have not been plotted. In all panels the data are plotted with 32 µ s and 2 MHz time and frequency resolution, respectively (with the exception of B1 and B5 which are plotted with 4 MHz frequency resolution).  \n<!-- image -->  \nTable 1: Burst properties.  \nFigure 2: Localisation plots for FRB 20200120E. Normalised dirty images of the individual bursts (B2, B3, B4 and B5; a-d ) along with a dirty image of the four bursts combined ( e ), produced by applying a natural weighting to the data. For visualisation purposes we clip the colour scale at zero, i.e. only positive peaks are displayed. The white circles are centred on the location of the globular cluster [PR95] 30244 as derived from the Subaru image in Figure 3. Their size indicates the region that contains 90% of the globular cluster's optical emission. The synthesized beams of each image are displayed as grey ellipses in the bottom left corner of each panel. f : The cleaned image and resulting localisation of FRB 20200120E, as derived from the combined data sets of four bursts. The resulting coordinates of FRB 20200120E (highlighted by the white marker) are RA (J2000) = 9 h 57 m 54 : 69935 s GLYPH<6> 1 : 2 mas, Dec (J2000) = 68 GLYPH<14> 49 0 0 : 8529 00 GLYPH<6> 1 : 3 mas.  \n<!-- image -->  \n68  \n·  \n49  \n'  \n20  \n''  \n10  \n''  \n)  \nJ2000  \n(  \nDec  \n00  \n''  \n48  \n'  \n50  \n''  \nh  \n9  \n57  \na  \nm  \n58  \ns  \ns  \n56  \nRA  \n(  \nJ2000  \n)  \nFigure 3: Optical images of the FRB 20200120E host and surrounding field. Left ( a ): 40 00 GLYPH<2> 40 00 g 0 , r 0 , and i 0 band image of [PR95] 30244 acquired with Hyper Suprime-cam. The small red ellipse is centred at the location of FRB 20200120E. In panel b we show the zoomed-in r 0 band image of [PR95] 30244. The grey circle represents the estimated position of the centre of [PR95] 30244 and its 10 GLYPH<27> uncertainty (dominated by the optical-to-radio reference frame tying). The small red ellipse is the same as in panel a , and also represents the 10 GLYPH<27> positional uncertainty region of FRB 20200120E. Panels c and d show cross-sections of the brightness distribution of the cluster (blue solid lines) with the Mo GLYPH<11> at profile that we fit overlaid in black. Indicated in solid grey lines are the PSFs as measured from stars in the images. Note that scatter in the PSFs is smaller than the linewidth.  \n<!-- image -->  \nFigure 4: Continuum maps of the field around FRB 20200120E. a: 1.4-GHz EVN continuum image after combining the three epochs (EK048B, EK048C, and EK048F); b: 1.5-GHz Realfast , and c: 340-MHz VLITE continuum image. The red circles indicate the 10 GLYPH<27> (for EVN) and 1000 GLYPH<27> (for Realfast , VLITE) positional uncertainty region of FRB 20200120E. Note the very di GLYPH<11> erent scales between the three panels. We clip all values below zero and above 60 µ Jy beam GLYPH<0> 1 (EVN), 50 µ Jy beam GLYPH<0> 1 ( Realfast ) and 3 mJy beam GLYPH<0> 1 (VLITE) for visualisation purposes. The black ellipse in the bottom left corner of each panel indicates the synthesised beam size and position angle.  \n<!-- image -->  \ns  \n54  \ns  \n52", 'VLBI observations': "As part of our ongoing very long baseline interferometry (VLBI) campaign called PRECISE (Pinpointing REpeating ChIme Sources with the EVN), we observed the field centred on the coordinates from the discovery 6 of FRB 20200120E: RA (J2000) = 09 h 57 m 56 : 688 s , Dec (J2000) = 68 GLYPH<14> 49 0 31 : 8 00 . The quoted 90% confidence interval 6 of radius GLYPH<24> 1 : 5 0 is well covered by the field of view of the ad-hoc interferometric array we used to observe, which is comprised of dishes that are also part of the EVN. Weobserved the field 15 times between February and May 2021 (Table 2), with burst detections in the data that were taken on 2021 February 20 UT 17:00-22:00 (project code PR141A), 2021 March 7 UT 15:45-20:45 (PR143A), and 2021 April 28 UT 11:00-22:00 (PR158A). We observed in the 21-cm band ( GLYPH<24> 1 : 4 GHz) with slightly di GLYPH<11> erent array setups in each run. Depending on the capabilities at each station, we recorded either 128 or 256 MHz of total bandwidth, divided into 8 or 16 subbands of 16 MHz each. The participating stations and their respective frequency coverage are summarised in Table 3. We ran regular phasereferencing observations with a cycle time of 7.5 min; that is, 5.5 minutes on target and 2.0 minutes on the phase calibrator (J0955 + 6903, at GLYPH<25> 0 : 32 GLYPH<14> separation). In total, we spent 2.93 hrs on the target field in each of PR141A and PR143A, and 6.73 hrs in PR158A. The calibrator source J1048 + 7143 served as fringe finder and bandpass calibrator and was observed twice for 5 minutes in each run. For verification and single-dish time-domain calibration purposes we observed the pulsar B0355 + 54 for 2 minutes in PR141A and PR143A. In PR158A the pulsar B2255 + 58 was observed for 5 minutes for the same reason.  \nWe recorded raw voltages ('baseband' data, dual circular polarisation, 2-bit sampling) in VDIF 50 or Mark5B 51 format at all stations. At E GLYPH<11> elsberg we also recorded total intensity filterbanks with the PSRIX pulsar backend 9 in parallel to the voltage data. These data span the frequency range of 1255-1505 MHz with a time and frequency resolution of 102.4 µ s and 0.49 MHz, respectively. Similarly, at SRT we also recorded in parallel baseband data and total intensity filterbanks (with the local Digital Filter Bank system, DFB). These DFB-filterbanks have a time and frequency resolution of 128 µ s and 1 MHz, respectively, covering the frequency range of 1140.5-2163.5 MHz out of which we search the usable range of 1210.5-1739.5 MHz.  \nThe data from both E GLYPH<11> elsberg and SRT were searched for bursts in two independent pipelines. The baseband data were processed with the pipeline outlined in Kirsten et al. 52 , which converts the raw voltages to filterbank  \nformat (in this case, total intensity with time resolution 64 µ s and frequency resolution 125 kHz) and searches those with Heimdall within GLYPH<6> 50 pc cm GLYPH<0> 3 of the expected DM = 87 : 818 pc cm GLYPH<0> 3 , as found by Bhardwaj et al. 6 . The burst candidates are classified as either radio frequency interference (RFI) or potential FRBs using the neural network classifier FETCH 53 . The filterbanks as recorded with the respective pulsar backends were searched with a pipeline that uses the PRESTO suite of tools 54,55 and a classifier based on work by Michilli et al. 56 .  \nCorrelation of the data was performed at the Joint Institute for VLBI ERIC (JIVE; in the Netherlands) under proposal EK048 (with codes EK048B for PR141A, EK048C for PR143A, and EK048F for PR158A). In total, we ran three correlator passes using the software correlator SFXC 11 : in the first run we correlate all scans containing the calibrator sources with a standard 2-s time integration and 64 channels per 16-MHz subband. A second correlation pass was performed only on the data containing bursts (their arrival times were determined via the search described above), with a higher frequency resolution (8 192 channels per subband) and time resolution (the correlation gates around the bursts were chosen manually to optimise the signal-to-noise for each burst, Table 1). The strongest bursts allowed a direct fringe fit on their data, which provided a first estimate of their sky position to a level of a few arcseconds: RA (J2000) GLYPH<25> 09 h 57 m 54 : 8 s , Dec (J2000) GLYPH<25> 68 GLYPH<14> 49 0 03 00 . We then used this position to re-correlate the burst data at the same frequency resolution as in the first correlation pass. This allowed us to directly apply the calibration performed on the first pass (containing the calibrator sources) to the data containing bursts.  \nThe full data reduction was performed using the Astronomical Image Processing System AIPS , 57 and D ifmap 58 following standard procedures. A-priori amplitude calibration was performed using the known gain curves and system temperature measurements recorded at each station during the observation. These data were not available for Toru'n and Irbene in EK048B, and for Urumqi in EK048C. We used nominal system equivalent flux density values and flat gain curves to perform the amplitude calibration in these cases. In EK048C, the data from Urumqi were flagged due to the impossibility to properly convert the locally-recorded linear polarizations into circular ones (as in the rest of the antennas). Ionospheric dispersive delays were calculated from maps of total electron content provided by the global positioning system satellites and removed via the TECOR task in AIPS . We first corrected for the instrumental delays and bandpass calibration using the calibrator source J1048 + 7143, and thereafter fringe-fit the data using all calibrator sources. The phase calibrator (J0955 + 6903; displaying a peak brightness of GLYPH<24> 73 mJy beam GLYPH<0> 1 ) was then imaged and self-  \nalibrated to improve the final calibration of the data (for both phases and amplitudes). A common source model for the phase calibrator was used to improve the calibration of both epochs. The obtained solutions were then transferred to the burst data, which were finally imaged.  \nIn the third, and final, correlator pass we processed the entire observation, correlating all scans from the target with the same time and frequency setup as in the first correlator pass, in order to obtain a deep continuum image of the field.", 'VLA': 'Weobserved the field of FRB 20200120E with the Karl G. Jansky Very Large Array (VLA) as part of a program to localise repeating FRBs identified by CHIME / FRB (program 20B-280). The field was observed in five 1-hour blocks from 2020 December 29 through 2021 January 18. Data were recorded in parallel at both 1 : 5 GHz and 340 MHz. The VLA antennas were arranged in the A configuration, which provides baseline lengths up to 30 km and a typical spatial resolution of 1.3 00 and 6.0 00 at 1 : 5 GHz and 340 MHz, respectively. The total on-target integration time amounts to 200 minutes.  \nRealfast Visibility data from the VLA observations were recorded with a sampling time of 3 seconds from 1 to 2 GHz. Simultaneously, a copy of the data with sampling time of 10 ms was streamed into the Realfast system 59 . We used Realfast to search this data stream for FRBs in real time. The typical 1 GLYPH<27> sensitivity of the VLA is 5 mJy beam GLYPH<0> 1 in 10 ms.  \nThe standard (slow) visibility data were analyzed to search for persistent emission associated with the FRB location. We calibrated the data with the VLA calibration pipeline (version 2020.1) using 3C147 as a flux calibrator. Calibrated visibilities for all five epochs were combined and imaged with CASA (version 6.1).  \nWe imaged the data with robust weighting of 0.5 and removed baselines shorter than 100 GLYPH<21> to reduce the e GLYPH<11> ects of RFI. This produced an image with a synthesized beam size of 2 00 by 1 00 with position angle of 126 GLYPH<14> . The sensitivity in the combined image is 6 : 5 µ Jy beam GLYPH<0> 1 , which is consistent with expectations given the usable bandwidth of 400 MHz.  \nVLITE The VLA Low-band Ionosphere and Transient Experiment VLITE; 60,61 is a commensal instrument on the VLA that records and correlates data from a 64-MHz subband at a central frequency of GLYPH<24> 340 MHz. It operates on up to 18 antennas during nearly all regular VLA operations. All VLITE data were processed within the VLITEFast GPU-based real-time system to search the incoming  \nvoltage stream for dispersed transients 62 . For imaging purposes, primary calibration and editing for each day of visibility data were carried out with the automated VLITE processing pipeline. Due to radio interference from satellites at the upper end of the band, the final usable bandwidth was 38.2 MHz centred at 340.85 MHz. The data were subsequently combined, imaged and self-calibrated in amplitude and phase using the Obit task MFImage 63 . In order to reduce artefacts from the bright extended radio galaxy M82 located GLYPH<24> 1 GLYPH<14> northwest of the target position, baselines shorter than 4.0 k GLYPH<21> were removed at this point. The final image was created in WSClean 64 , and corrected for the o GLYPH<11> set primary beam response of VLITE. The image has an rms of 320 µ Jy beam GLYPH<0> 1 , and a beam of 10.1 00 by 3.6 00 at a position angle of 132 GLYPH<14> .', 'Archival optical and high energy data': 'Hyper Suprime-Cam The field around M81 has been well-observed over the years by multiple telescopes. We retrieved archival data from the Hyper Suprime-Cam on the 8.1-m Subaru telescope 65 using the SMOKA interface. We chose images with seeing better than 0 : 00 7. We processed the g 0 , r 0 , and i 0 band images with the hscpipev8.4 pipeline 66 . The pipeline uses the PanSTARRs catalogue PS1; 67 as an astrometric and photometric reference. The typical astrometric residuals were GLYPH<24> 50-60 mas, which is the uncertainty we have assumed to tie the optical and the radio reference frames.  \nGaia [PR95] 30244 also appears in the Gaia Early Data Release 3 Catalogue 16,17 with Source ID 1070264274879949184, and position RA (J2000) = 9 h 57 m 54 : 71402 s GLYPH<6> 1 : 6 mas, Dec (J2000) = 68 GLYPH<14> 49 0 0 : 7775 00 GLYPH<6> 1 : 7 mas. This position is consistent (within < 3 GLYPH<27> confidence level) with the one we have derived from the Hyper Suprime-Cam data. The observed o GLYPH<11> set allowed us to estimate the possible systematic uncertainties in the optical image registration error (15 mas; by adding in quadrature the observed o GLYPH<11> set between the the Gaia position and the one we determined, plus the uncertainties on the positions).  \nChandra X-ray Observatory Several deep archival Xray observations are available for the field around M81 from XMM and Chandra . We selected the archival observation with the longest exposure time that covers the location of FRB 20200120E, a 26 ks Chandra observation Obs. ID 9540, taken with ACIS in FAINT mode, 68 to probe for an X-ray source. The data were reduced using CIAO version 4.12 69 following standard procedures. As the source was located about 14 0 o GLYPH<11> -axis, events were  \nTable 2: Time ranges of PRECISE runs targeting FRB 20200120E between February and May 2021  \na Epoch with detection  \nTable 3: Setups at the di GLYPH<11> erent stations during observations used in the analysis  \nGLYPH<0>  \nextracted in a large 10 00 -radius region centred on the position of FRB 20200120E. We also extract events from a 60 00 -radius region away from the source at a similar o GLYPH<11> -axis angle to estimate the background count rate. The Xray count-rate in the source extraction region, 4 : 4 GLYPH<2> 10 GLYPH<0> 6 counts s GLYPH<0> 1 arcsec GLYPH<0> 2 , is consistent with the background region rate of 3 : 9 GLYPH<2> 10 GLYPH<0> 6 counts s GLYPH<0> 1 arcsec GLYPH<0> 2 . To place a limit on an X-ray source at the location of FRB 20200120E we  \nuse the Bayesian method of Kraft et al. 70 , which results in a 0.5-10 keV source count rate upper limit of 1 GLYPH<2> 10 GLYPH<0> 3 counts s GLYPH<0> 1 (3 GLYPH<27> ). Taking into account the spectral response for the o GLYPH<11> -axis location of the source (via an ancillary response file created by the CIAO tool specextract ), and assuming a photoelectrically absorbed power-law source spectrum with a spectral index of GLYPH<0> = 2 and a hydrogen column density of N H = 10 21 cm GLYPH<0> 2 , this count rate limit  \ncorresponds to a 0.5-10 keV absorbed flux upper limit of 1 GLYPH<2> 10 GLYPH<0> 14 erg cm GLYPH<0> 2 s GLYPH<0> 1 .  \nFermi -LAT The Large Area Telescope (LAT) onboard the Fermi satellite provides a uniform sensitivity survey of the whole sky in the energy range between 100 MeV and 300 GeV. We searched all of the publicly available catalogues for counterparts up to the latest published 71 release, 4FGL-DR2, with null results. However, even the most luminous known Galactic globular cluster (Terzan5), whose luminosity is (42 : 4 GLYPH<6> 1 : 5) GLYPH<2> 10 34 erg s GLYPH<0> 1 in the 0 : 1100 GeV energy range 72 , would have a gamma-ray flux of only (2 : 00 GLYPH<6> 0 : 07) GLYPH<2> 10 GLYPH<0> 16 erg cm GLYPH<0> 2 s GLYPH<0> 1 at the distance of M81. This is nearly three orders of magnitude dimmer than the faintest source detected in the 4FGL-DR2 catalogue.', 'Dispersion measure refinement': 'To refine the DM for further analysis, we maximised the signal to noise ratio (S / N) of a very narrow spike in B3 10 (Figure 1g) and find DM = 87 : 7527 GLYPH<6> 0 : 0003 pc cm GLYPH<0> 3 . This value is comparable to, but formally deviates from DM = 87 : 818 GLYPH<6> 0 : 007 pc cm GLYPH<0> 3 found by Bhardwaj et al. 6 , where a weighted average of three bursts was used. Possible explanations for this discrepancy are the lack of shorttimescale structure in the CHIME / FRB bursts 6 , the potential for non-dispersive time-frequency drifting 73 or a time-variable DM.', 'Milliarcsecond localization of FRB 20200120E': "We imaged both the individual bursts separately, as well as a data set produced by the combination of all individual burst visibilities. Figure 2a-d display the dirty maps (i.e. the inverse Fourier Transform of the visibilities without applying any deconvolution, i.e. 'CLEANing') of the bursts that were detectable in the correlated data, using a natural weighting of the data. B1 was too faint to produce a useful image, and we therefore exclude it from the localisation analysis. B5 was only detected in the lower half of the observed band, where most of the antennas were not recording (see Table 3). We therefore only used data from this part of the band. Figure 2e shows the dirty map of the combined data of the visibilities from all bursts. In this map we obtained an emission pattern consistent with the one expected from the dirty beam (the inverse Fourier Transform of a point-like source), allowing us to unambiguously identify the position of FRB 20200120E. The observed emission reached a 12 GLYPH<27> confidence level, with the secondary sidelobes in the fringe pattern being  \nGLYPH<24> 66% of the peak emission. This provided a robust localization in the map, as it would require a noise fluctuation of & 7 GLYPH<27> to produce such peak emission. We also conducted di GLYPH<11> erent approaches during the imaging of the data: di GLYPH<11> erent weighting schemes, and selecting di GLYPH<11> erent subsets of antennas in the array. The derived position of FRB 20200120E was robust across all these approaches. Figure 2f displays the final, 'CLEANed', image of the combined bursts.  \nThe final coordinates of FRB 20200120E are RA (J2000) = 9 h 57 m 54 : 69935 s GLYPH<6> 1 : 2 mas, Dec (J2000) = 68 GLYPH<14> 49 0 0 : 8529 00 GLYPH<6> 1 : 3 mas. We note that the quoted uncertainties reflect the statistical uncertainties from the measured position of FRB 20200120E (0 : 7 and 0 : 4 mas in RA and DEC, respectively), the uncertainties in the absolute International Celestial Reference Frame position of the phase calibrator (J0955 + 6903; 0.11 mas), and the systematic uncertainty associated with the phase-referencing technique 74 of GLYPH<24> 0 : 9 and 1 : 2 mas, in RA and DEC, respectively.  \nWe combined the continuum VLBI data from the three epochs to produce a deep image of the field around FRB20200120E to search for persistent emission. No significant sources above a 5 GLYPH<27> confidence level (with an rms of 10 µ Jy beam GLYPH<0> 1 ) are detected on milliarcsecond scales (Figure 4a). In the VLA data taken at 1 : 5 GHz (Figure 4b), we did identify two sources with peak brightness of 110 µ Jy beam GLYPH<0> 1 and 73 µ Jy beam GLYPH<0> 1 , and o GLYPH<11> set by 6 00 and 9 00 , respectively. The projected density of radio sources of this brightness is roughly 1 000 to 3 000 per square degree 75 . Therefore, we expect between 13 sources within 1 0 of FRB 20200120E by chance. The closer of the two nearby radio sources is within 0 : 2 00 of a PS1 source with i = 21 : 3 mag. This host galaxy has a photometric redshift in the PS1 STRM catalogue 76 of 0 : 67 GLYPH<6> 0 : 2, so it is most likely a background galaxy. The other identified radio source has no PS1 counterpart. We note that neither of these two sources exhibit significant compact emission on milliarcsecond scales.", '[PR95] 30244 and chance coincidence probability': "We measured the full-width at half maximum (FWHM; 'seeing') of the coadded i 0 , r 0 , and g 0 images of [PR95] 30244 to be 0 : 00 63, 0 : 00 57, and 0 : 00 62, respectively, using profile fits to bright, isolated stars. The brightness distribution of [PR95] 30244 has an FWHM of 0 : 00 77, 0 : 00 70, and 0 : 00 75 in the same three images. Subtracting the FWHMs of the isolated stars in quadrature, we estimate that the intrinsic FWHM of [PR95] 30244 is about 0 : 00 42, corresponding to about 7.4 pc at a distance of 3.63 Mpc.  \nTo estimate the probability of chance coincidence 77 for an M81 globular cluster in the FRB localisation region,  \nwe use a circular localisation region with a radius ( R ) = max f 2 R e GLYPH<11> of [PR95] 30244, maximum seeing-limited size of [PR95] 30244 in the Hyper Suprime-images g = 0 : 00 77. Perelmuter & Racine 14 parameterized the projected areal number density ( GLYPH<26> GC = arcmin 2 ) of the M81 globular clusters as a function of their angular o GLYPH<11> set from M81 ( r , in arcmin) as, log 10 ( GLYPH<26> GC) = GLYPH<0> 2 : 07 GLYPH<2> log 10 ( r ) + 0 : 82 GLYPH<6> 0 : 05, for 0 GLYPH<20> log 10 ( r ) GLYPH<20> 1 : 4. At the o GLYPH<11> set of FRB 20200120E from M81 (19 : 6 0 ), GLYPH<26> GC = 0 : 014 arcmin GLYPH<0> 2 GLYPH<25> 3 : 8 GLYPH<2> 10 GLYPH<0> 6 arcsec GLYPH<0> 2 . Assuming a Poisson distribution of M81 globular clusters at r = 19 : 6 0 , the probability of finding at least one globular cluster by chance within a radius R is given by P cc = 1 GLYPH<0> exp( GLYPH<0> GLYPH<25> R 2 GLYPH<26> GC) GLYPH<25> 7 GLYPH<2> 10 GLYPH<0> 6 . A more conservative estimate of P cc can be derived by assuming that all the predicted 300 GLYPH<6> 100 M81 globular clusters 18 are uniformly distributed within the angular area of radius = 19 : 6 0 so that GLYPH<26> GC = 4 : 6-9 : 2 GLYPH<2> 10 GLYPH<0> 5 , and consequently P cc = 0.85 GLYPH<0> 1 : 7 GLYPH<2> 10 GLYPH<0> 4 . From such a very low P cc value, we conclude that the association of FRB 20200120E and [PR95] 30244 is robust.", 'Modelling of [PR95] 30244': "To estimate important physical properties of [PR95] 30244, such as its stellar mass, metallicity, stellar population age and V-band extinction, we used the Prospector code 78,79 for stellar population inference. We modelled the SDSS photometry (Table 5, from the SDSS DR12 catalogue 80 ) of [PR95] 30244 and fit a five-parameter (Table 6) 'delayed-tau' model for the star formation rate SFR( t ) / t exp( GLYPH<0> t =GLYPH<28> ), where t is the time since the formation epoch of the galaxy, and GLYPH<28> is the characteristic decay time of the star-formation history of [PR95] 30244 81,82 . As we are modelling a globular cluster, we did not include nebular line emission but only enabled a dust emission model 83 in our fitting. The best-fit spectral energy distribution (SED) profile of [PR95] 30244 is shown in Figure 6. Prospector also enables Markov Chain Monte Carlo (MCMC) sampling of the posterior to estimate uncertainty in the best-fit values of the physical properties of [PR95] 30244. We show the corner plot of the MCMC-analysis in Figure 7 and list the results in Table 4. Using the relation 84 , [Fe / H] = 1.024 GLYPH<2> log(Z / Z GLYPH<12> ), we estimate the [Fe / H] of [PR95] 30244 = GLYPH<0> 1 : 83 + 0 : 86 GLYPH<0> 0 : 87 , which is in good agreement with earlier estimates 13,85 . We can get an estimate of the velocity dispersion ( GLYPH<27> r) of [PR95] 30244 using the virial theorem: GLYPH<27> r GLYPH<24> p 2GM = 3Re GLYPH<11> , where G is the gravitational constant. Using the M and Re GLYPH<11> values of [PR95] 30244 from Table 4, we estimate GLYPH<27> r GLYPH<24> 22 km s GLYPH<0> 1 .", 'Possible MIC-models for the formation FRB 20200120E': 'of  \nThe most likely of the MIC-models is that of a merging WD-WD system as those dominate the cores of globular clusters 86 , while a NS-NS progenitor system is less probable 87 . A typical globular cluster with a total mass of GLYPH<24> 2 GLYPH<2> 10 5 M GLYPH<12> can host 10 GLYPH<0> 20 MSPs formed via AIC or MIC 34 . At birth, such NSs would be extreme objects with high rotation rates and strong magnetic fields, potentially capable or generating FRBs. We note that the metallicity limit (log[Fe = H] > GLYPH<0> 0 : 6) set for the formation of young NSs in globular clusters 88 is much higher than the metallicity that we estimate for [PR95] 30244 (log[Fe = H] = GLYPH<0> 1 : 83, Table 4). Nevertheless, non-recycled pulsars have been found towards some globular clusters 88-90 . These young pulsars are formed at a comparable rate to MSPs in globular clusters, but they have much shorter active lifetimes (Myr versus Gyr).', 'Constraints on the Galactic halo DM and RM': 'Since FRB 20200120E is extragalactic, its dispersive delay is probing the full extent of the Milky Way ISM (DM MW ISM ) and halo (DM MW Halo ) along this line of sight. There are also extragalactic contributions from the intergalactic medium DMIGM and the host galaxy (DMM81), leading to the total observed DM = DM MW ISM + DM MW Halo + DMIGM + DMM81. The intergalactic medium between the Milky Way and M81 contributes on the order 91 of DMIGM GLYPH<24> 1 pc cm GLYPH<0> 3 . To estimate DMM81, we only consider the contribution from the halo of M81, as both the M81 disk and the globular cluster make negligible contributions to the measured DM. The M81 halo DM contribution is estimated 6 to be GLYPH<24> 15-50 pc cm GLYPH<0> 3 depending on the choice of a halo density profile and baryon fraction in the M81 halo. For the Galactic contribution, models of the Milky Way ISM predict DM MW ISM = 30-40 pc cm GLYPH<0> 3 in this direction 92,93 (with a shallow spacial gradient in the region, Figure 5). Using these estimates, we limit the Milky Way halo contribution to the FRB sight-line, which is poorly constrained by current observations 94 , to DM MW Halo = DM GLYPH<0> DM MW ISM GLYPH<0> DMIGM GLYPH<0> DMM81 . 3242pc cm GLYPH<0> 3 . This is well in line with the models of Yamasaki & Totani 95 , which predict DM MW Halo = 1030 pc cm GLYPH<0> 3 , but lower than predicted in some other models 96 .  \nSimilar considerations are also applicable for the rotation measure 6 RM = GLYPH<0> 36 : 9 rad m GLYPH<0> 2 as determined in the companion paper by Nimmo et al. (submitted). The Galactic contribution 97 along the line of sight to FRB 20200120E is RM = GLYPH<0> 17 GLYPH<6> 4 rad m GLYPH<0> 2 (Figure 5). The contribution of the IGM is most likely minor, leav-  \ning only the MW halo, the M81 halo and the local environment of FRB 20200120E as contributing sources. The RMs of the MW- and M81-halo are likely small ( j RM j < 20 rad m GLYPH<0> 2 ), constraining RMLocal to the range [ + 20 ; GLYPH<0> 60] rad m GLYPH<0> 2 . This is comparable to earlier results 98 for FRB 20180916B (RM = GLYPH<0> 115 rad m GLYPH<0> 2 ) but three orders of magnitude lower than the (highly variable) RM of FRB 20121102A 99 . This indicates that models of FRB sources do not necessarily require extreme magneto-ionic environments, unless the magnetic fields along the line of sight to both FRB 20200120E and FRB 20180916B are strongly tangled, such that they result in a low net RM. More likely though, FRB 20121102A resides in a very different environment giving rise to its observed properties.', 'Data availability': 'The datasets generated from the EVN observations and analysed in this study are available at the Public EVN Data Archive under the experiment codes EK048B, EK048C, and EK048F.', 'Code availability': 'The codes used to analyse the data are available at the following sites: AIPS ( http: //www.aips.nrao.edu/index.shtml ), CASA ( https://casa.nrao.edu ), Difmap ( ftp://ftp. astro.caltech.edu/pub/difmap/difmap.html ), DSPSR ( http://dspsr.sourceforge.net/ ), FETCH ( http://dspsr.sourceforge.net/ ), Heimdall ( https://sourceforge.net/projects/ heimdall-astro/ ), IRAF ( http://ast. noao.edu/data/software ), PRESTO ( https: //github.com/scottransom/presto ), PSRCHIVE ( http://psrchive.sourceforge.net ), and SpS ( https://github.com/danielemichilli/SpS ).', 'References': "- [1] Petro GLYPH<11> , E., Hessels, J. W. T. & Lorimer, D. R. Fast radio bursts. 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(submitted) for details).  \n<!-- image -->  \nTable 4: Notable properties of [PR95] 30244.  \nTable 5: Broadband SDSS filters used to model the SED of [PR95] 30244.  \n- [18] Harris, W. E., Harris, G. L. H. & Alessi, M. A Catalog of Globular Cluster Systems: What Determines the Size of a Galaxy's Globular Cluster Population? Astrophys. J. 772, 82 (2013).\n- [19] Marcote, B. et al. A repeating fast radio burst source localized to a nearby spiral galaxy. Nature 577, 190-194 (2020).\n- [20] Marcote, B. et al. The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales. Astrophys. J. Lett. 834, L8 (2017).\n- [21] Ajello, M. et al. The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope. Astrophys. J. 892, 105 (2020).\n- [22] Abdo, A. A. et al. Detection of Gamma-Ray Emission from the Starburst Galaxies M82 and NGC 253 with the Large Area Telescope on Fermi. Astrophys. J. 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Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds. Astrophys. J. 500, 525-553 (1998).", 'Acknowledgements': "Figure 7: MCMCsimulation corner plot , where the posterior probability distributions are shown for each of the five model parameters along the diagonal panels, and the correlations between model parameter posteriors are shown along the columns. Above each probability distribution, the median of the parameter posterior is printed, along with the oneGLYPH<27> error bars.  \n<!-- image -->  \nWe would like to thank the directors and sta GLYPH<11> at the various participating stations for allowing us to use their facilities and running the observations. The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. Scientific results from data presented in this publication are derived from the following EVN project code: EK048. This work was also based on simultaneous EVN and PSRIX data recording observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at E GLYPH<11> elsberg, and we thank the local sta GLYPH<11> for this arrangement. We would like to express our gratitude to Willem van Straten for modifying the DSPSR software package to fit our needs. We appreciate helpful discussions about magnetar formation scenarios in a globular cluster environment with E. P. J. van den Heuvel. A.B.P is a McGill Space Institute (MSI) Fellow and a Fonds de Recherche du Quebec - Nature et Technologies (FRQNT) postdoctoral fellow. B.M. acknowledges support from the Spanish Ministerio de Econom'ıa y Competitividad (MINECO) under grant AYA2016-76012-C3-1-P and from the Spanish Ministerio de Ciencia e Innovaci'on under grants PID2019-105510GB-C31 and CEX2019000918-M of ICCUB (Unidad de Excelencia 'Mar'ıa de Maeztu' 2020-2023). Basic research in radio astronomy at NRL is funded by 6.1 Base funding. Construction and installation of VLITE was supported by the NRL Sustainment Restoration and Maintenance fund. C.J.L. acknowledges support from the National Science Foundation Grant 2022546. C.L. was supported by the U.S. Department of Defense (DoD) through the National Defense Science & Engineering Graduate Fellowship (NDSEG) Program. D.M. is a Banting Fellow. E.P. acknowledges funding from an NWO Veni Fellowship. F.K. acknowledges support from the Swedish Research Council via Grant No. 2014-05713. FRB research at UBC is supported by an NSERC Discovery Grant and by the Canadian Institute for Advanced Research. J.P.Y. is supported by the National Program on Key Research and Development Project (2017YFA0402602). K.S. is supported by the NSF Graduate Research Fellowship Program. K.W.M. is supported by an NSF Grant (2008031). M.B. is supported by an FRQNT Doctoral Research Award. N.W. acknowledges support from the National Natural Science Foundation of China (Grant 12041304 and 11873080) P.S. is a Dunlap Fellow and an NSERC Postdoctoral Fellow. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The NANOGrav project receives support from National Science Foundation (NSF)  \nPhysics Frontiers Center award number 1430284. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. B.M.G. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC) through grant RGPIN-2015-05948, and of the Canada Research Chairs program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. SMR is a CIFAR Fellow and is supported by the NSF Physics Frontiers Center award 1430284. This work is based in part on observations carried out using the 32-m radio telescope operated by the Institute of Astronomy of the Nicolaus Copernicus University in Toru'n (Poland) and supported by a Polish Ministry of Science and Higher Education SpUB grant. V.B. acknowledges support from the Engineering Research Institute Ventspils International Radio Astronomy Centre (VIRAC). V.M.K. holds the Lorne Trottier Chair in Astrophysics & Cosmology and a Distinguished James McGill Professorship and receives support from an NSERC Discovery Grant and Herzberg Award, from an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), and from the FRQNT Centre de Recherche en Astrophysique du Quebec We receive support from Ontario Research Fund-research Excellence Program (ORF-RE), Natural Sciences and Engineering Research Council of Canada (NSERC) [funding reference number RGPIN-2019-067, CRD523638-201, 555585-20], Canadian Institute for Advanced Research (CIFAR), Canadian Foundation for Innovation (CFI), the National Science Foundation of China (Grants No. 11929301), Simons Foundation, Thoth Technology Inc, and Alexander von Humboldt Foundation. Computations were performed on the SOSCIP Consortium's [Blue Gene / Q, Cloud Data Analytics, Agile and / or Large Memory System] computing platform(s). SOSCIP is funded by the Federal Economic Development Agency of Southern Ontario, the Province of Ontario, IBM Canada Ltd., Ontario Centres of Excellence, Mitacs and 15 Ontario academic member institutions. Based [in part] on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. AIPS is a software package produced and maintained by the National Radio Astronomy Observatory (NRAO).  \nAuthor contributions F.K. is the Principal Investigator of the PRECISE team, he organised the observations, found the five bursts in the raw voltages and coordinated writing of the manuscript. B.M. lead the analysis of the correlated data, performed the localisation and wrote parts of the manuscript. K.N. lead the time-domain analysis of the bursts. J.W.T.H. lead the interpretation of the results and wrote parts of the manuscript. M.B. lead and performed the modelling of [PR95] 30244. S.P.T. performed the data reduction and analysis of the Subaru data. A.K. wrote and modified the software correlator SFXC to allow for the highest time resolution data. J.Y. assisted with the data reduction, analysis and interpretation of the correlated data. M.P.S. helped with the manuscript and created Fig. 5. P.S. and A.B.P. reduced and analyzed the archival Chandra data. C.J.L. reduced and analysed the Realfast data. W.M.P. reduced and analysed the VLITE data. M.G. searched the Fermi catalogues. Z.P. assisted with the reduction and analysis of the correlated data. C.B. assessed the optical registration errors of the Subaru images. D.M.H. searched the PSRIX and DFB data for bursts. U.B. coordinated and performed the observations at E GLYPH<11> elsberg. V.B. coordinated and performed the observations at Irbene. M.B. helped commissioning the dual recording mode at SRT. S.T.B coordinated and performed the observations at Noto. J.E.C. supported the observations at Onsala. A.C. implemented the dual recording mode at SRT and performed some of the observations. R.F. supports the observations at Toru'n. O.F. wrote observing schedules. M.P.G. coordinated and performed the observations at Toru'n. R.K. assisted with the dual recording at E GLYPH<11> elsberg. M.A.K. supports the observations at Badary, Svetloe and Zelenchukskaya. M.L. supported the observations at Onsala and assisted with the manuscript. G.M. coordinated and performed the observations at Medicina. A.M. coordinated and performed the observations at Badary, Svetloe and Zelenchukskaya. O.S.O-B wrote observing schedules. A.P. supported the observations at SRT. G.S. ran most of the observations at SRT. N.W. and J.Y. coordinated and performed the observations at Urumqi. V.M.K. played a significant coordination role that enabled these results. All other co-authors contributed to the CHIME / FRB discovery of the source or the interpretation of the analysis results and the final version of the manuscript.  \nCompeting interests The authors declare no competing interests.  \nAdditional information  \nCorrespondence and requests for materials should be addressed to F.K."}