Search for low-energy signals from fast radio bursts with the Borexino detector

The search for neutrino events in correlation with 42 most intense fast radio bursts (FRBs) has been performed using the Borexino dataset from 05/2007 to 06/2021. We have searched for signals with visible energies above 250 keV within a time window of ±1000\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\pm \, 1000$$\end{document} s corresponding to detection time of a particular FRB. We also applied an alternative approach based on searching for specific shapes of neutrino-electron scattering spectra in the full exposure data of the Borexino detector. In particular, two incoming neutrino spectra were considered: the monoenergetic line and the spectrum expected from supernovae. The same spectra were considered for electron antineutrinos detected through inverse beta-decay reaction. No statistically significant excess over the background was observed. As a result, the strongest upper limits on FRB-associated neutrino fluences of all flavors have been obtained in the 0.5–50 MeV neutrino energy range.


Introduction
A fast radio burst (FRB) is a millisecond radio transient observed at extragalactic or cosmological distance. Although FRBs were discovered almost 15 years ago [1], the nature of their source remains unclear. Numerous models with a wide variety of physical processes have been proposed to explain the origin of FRBs (see review articles [2][3][4][5]). The most popular class of models postulates a production mechanism associated with arising activity of magnetars [6,7]. These models have received support from repeating behavior of some FRBs, especially after detection of FRB200428 in temporal and spatial coincidence with X-ray burst from magnetar SGR 1935 + 2154 in the Milky Way galaxy [8,9].
Single-burst FRB models involve processes of supernova evolution, mergers, and collapses of neutron stars [10][11][12][13] with emission of neutrinos [14][15][16][17] (and possibly axions) which could be potentially detected by large-volume Cherenkov or scintillation detectors. The IceCube Neutrino Observatory has searched for spatial and temporal correlation between events with energies above 50 GeV, as well as temporal correlation between MeV events and 28 FRBs. It has set the upper limits on neutrino fluences associated with them [18][19][20]. The ANTARES Neutrino Telescope looked for TeV-PeV high-energy neutrinos spatially and temporally coincident with FRBs detected during 2013-2017, but no coincident neutrino candidate was observed [21].
Since modern radio telescopes have a narrow field of view, they are able to register only a fraction of the overall number of occurring FRBs. Total expected all-sky event rate of FRBs with fluence above ∼ 2 Jy ms is roughly 2 × 10 3 per day [3,30]. 1 Scintillation detectors lack the directional sensitivity to incoming neutrinos and therefore can not be used for temporal analysis in a wide time window due to the high rate of FRBs (in contrast to GRBs or GW events) and a possible delay of low-energy neutrino signal arriving from extragalactic distances.
Here, we have performed the temporal correlation analysis between Borexino events with visible energies above 0.25 MeV and some of the most intensive FRBs assuming the direct connection between radio and neutrino fluences of an FRB. Another approach was based on the search for the characteristic shape of (ν, e)-scattering in the high-statistic Borexino spectrum. Finally, we have taken into account that no events were observed with an energy greater than a certain value in the Borexino spectrum. Two different spectra of incoming neutrinos (ν e,μ,τ andν e,μ,τ ) were used for the analysis: the monoenergetic line and the spectrum expected from supernovae. The sameν e -neutrino spectra were considered for detection with the inverse beta-decay reaction (IBD).

Borexino detector
Borexino is a real-time liquid scintillator detector for solar neutrino spectroscopy. It is located underground at the Gran Sasso Laboratory (Italy) at a depth of 3400 m.w.e. Its main goal is to measure low-energy solar neutrinos via (ν, e) scattering in an ultrapure liquid scintillator.
The inner vessel of the detector (IV) comprises 278 tons of purified organic liquid scintillator confined in a transparent nylon sphere of 4.25 m in radius. The scintillator was produced from petrochemical organics extracted from underground to fulfill high radiopurity requirements. The scintillator compound is based on pseudocumene (PC, C 9 H 12 ) doped with 1.5 g/L of PPO (C 15 H 11 NO). It is surrounded by two concentric PC buffers (323 and 567 tons, respectively) doped with a small amount of light quencher (dimethylphthalate, DMP) intended for light yield reduction. The buffer partitioning is performed in order to reduce the diffusion of radon into the scintillator bulk. The IV and the buffers are contained inside a stainless steel sphere (SSS) with a diameter of 6.75 m fixed in position by a stainless steel support structure. The 1 Jy (Jansky) is a non-SI unit of spectral flux density, 1 Jy = 10 −26 W m −2 Hz −1 . SSS is enclosed in a cylinder with a hemispheric top with a diameter of 18 m and height of 16.9 m.
The water tank (WT) is constructed of stainless steel with high radiopurity and contains 2100 tons of ultrapure water as additional shielding against external γ -rays and neutrons. The WT is equipped with 208 8-in. PMTs and serves as the Cherenkov muon veto (outer detector, OD) for identification of residual muons crossing the detector. The scintillation light is detected by nominally 2212 8-inch PMTs of the inner detector (ID) uniformly distributed on the inner surface of the SSS.
Borexino detects charged particles via scintillation light produced in the liquid scintillator. Each event occurring in the detector is characterized by a number of fired PMTs whose pulse amplitudes and arrival times are recorded. The number of active PMTs has slowly declined over the course of the Borexino data taking. For each FRB event considered in this analysis, the true number of active PMTs was included in the modeling of the detector response and the signal normalized appropriately. These data are used to reconstruct the energy and spatial coordinates of the event and to identify the type of the particle (e, α, μ). Both energy and spatial resolutions of the detector were studied with radioactive sources placed at different positions inside the inner vessel [31]. The energy and position resolutions are σ E ≈ 50 keV and σ X ≈ 10 cm at 1 MeV with 2000 PMTs, respectively; both scaling with the energy of the event as ∼ 1/ √ E at low energies. The Borexino detector is unable to provide sufficient directional information about a single event due to the nearly isotropic emission of scintillation light (see, however, [32]).
A more detailed description of the Borexino detector can be found in the following papers [22][23][24][25].
Neutrinos (ν x , x = e, μ, τ ) and antineutrinos (ν x ) are detected by means of their elastic scattering on electrons: For a given neutrino energy, the maximum electron recoil energy is given by the Compton formula: where E ν is the (anti)neutrino energy and m e is the electron mass. The interaction between the scattered electron and scintillator molecules produces photons which are registered by PMTs.
Electron antineutrinosν e can also be detected via the inverse beta-decay (IBD) reaction with an energy threshold of 1.8 MeV: The visible energy of the positron and two annihilation photons is related to the antineutrino energy as E vis = Eν e − 0.784 MeV. The neutron capture on protons produces a 2.22 MeV γ -ray providing a delayed signal with the mean capture time of ∼ 260 µs [33]. In contrast to the total cross section of (ν e , e)-scattering which is proportional to E ν when E ν m e , the cross section of the IBD is proportional to ∼ E 2 ν e . Borexino was the first experiment to detect and then precisely measure the 7 Be solar neutrino flux [34,35] as well as the 8 B-neutrino flux with 3 MeV threshold [36,37]. It also observed pep-neutrinos for the first time [38] and made the first spectral measurement of pp-neutrinos [25,39,40], and provided the first experimental evidence of solar neutrinos produced in the CNO cycle [41,42]. The Borexino detector also registered antineutrinosν e emitted in the decay of radionuclides naturally occurring in the Earth [43][44][45][46].
Due to its excellent radiopurity, large target mass and low energy threshold, Borexino is perfectly suited for the study of other fundamental problems, as well as searching for rare and exotic processes in particle physics and astrophysics.
The Borexino experiment obtained new data on solar neutrino properties: ruled out any significant day-night asymmetry of the 7Be neutrino interaction rate [47], set new limits on the effective magnetic moment of solar neutrinos [34,48], on the flux ofν e from the Sun [29,49] and on the non-standard solar neutrino interactions [50]. A search for a number of rare low-energy processes has been carried out: possible violation of the Pauli exclusion principle [51], high-energy solar axions [52], heavy sterile neutrino mixing in the 8 B β + -decay [53], decay of an electron into a neutrino and a photon [54]. Additionally, temporal correlations with transient astrophysical sources such as γ -ray bursts [27], gravitational wave events [28], and solar flares [29] have been performed.

Data selection
Since a FRB is a very frequent event that is detected in a few cases, the analysis was conducted via two different approaches: a transient event search in a fixed time window with respect to the FRB detection moment and a generic search for extra neutrino-induced electron recoils or IBD components in the detector energy spectrum.

Transient approach data selection
The first approach does not require a well-described spectral shape due to the limited number of events in the time window and does not need any profound background reduction techniques, although the background is to be kept substantially low. Neutrino-electron elastic scattering events which are of interest in the current analysis lack any characteristic interaction signature. Thus, the background reduction has to be performed in a generic manner so as decrease in the detector count rate per unit of exposure. The background of the Borexino detector includes the following main components: -Short-lived cosmogenic backgrounds (τ ≤ 0.3 s) produced inside the detector fiducial volume, such as 12 B, 8 He, 9 C, 9 Li etc. -Other cosmogenic backgrounds produced inside the detector fiducial volume, such as longer-lived isotopes 11 Be, 10  These backgrounds can be suppressed by using information from the processed detector data, such as ID/OD coincidences as well as the energy and position reconstruction. Cosmogenic backgrounds can be reduced by applying the detector time vetoes after each muon event that can be discriminated through coincidence with the outer veto as well as via pulse-shape discrimination [33,55]. A veto length of 0.3 s following a muon event is applied to suppress 12 B to a statistically insignificant level and reduce 8 He, 9 C, and 9 Li by a factor of 3 with a live time loss of 1 %. Background components contained in the bulk can be reduced by applying a cut on the visible energy. This is important specifically due to the presence of 14 C in the scintillator. The carbon isotope 14 C produces a β-spectrum with an endpoint of 156 keV and has an activity of roughly 110 Bq in the whole inner vessel. The presence of this spectral component sets the lower threshold of the analysis at 250 keV of the visible energy. 2 Background components contained in the nylon of the IV and other detector materials cannot be removed by any kind of purification and therefore are 10 2 -10 3 times higher than within the bulk of the scintillator. The most dangerous components are the 214 Bi and 208 Tl decays. These nuclides undergo β and β +γ decay processes with continuous spectra overlapping with the energy region used in this analysis. The only way to overcome this kind of background is to perform a geometrical cut on events, selecting those within the fiducial volume. In our case the fiducial volume is defined such that all events within 75 cm to the IV are discarded, which corresponds to 3 standard deviations of position reconstruction uncertainty at the lowest energy threshold. The corresponding fiducial volume has a mass of 145 t. The Borexino dataset from May 15, 2007, (corresponding to the detector operation start) to June 21, 2021, was used for the temporal correlation 2 The visible energy spectrum of 14 C is broadened up to this value due to the detector energy resolution and its pile-up. analysis between the Borexino signals and the most intensive FRBs.

Spectral approach data selection
The spectral approach to data selection is more complicated since background components should not only be sufficiently suppressed, but also well described in terms of spectral shapes. Minimization of the number of these spectral components also benefits the final result due to suppression of their spectral correlations fit procedure, even if it comes at the expense of exposure loss. Thus, we modify the data selection procedure of the transient analysis in the following way: -We use the most radiopure dataset acquired from January 01, 2013, (corresponding to the detector stabilization after the water extraction procedure finished at the end of 2011) to November 31, 2020. -We apply an advanced system of the cosmogenic veto based on time and position reconstruction of muons and neutrons in the post-muon gate that strongly reduces cosmogenic backgrounds.
The advanced cosmogenic veto system dedicated to the discrimination of short-lived cosmogenic nuclides is based on the information from the muon trigger and post-muon trigger of the Borexino detector. We organize it in a way, similar to identification of the cosmogenic 11 C background performed in [55], but with different times and radii, namely: -120 s full detector veto after each muon that crossed the ID and has more than 20 neutron-like daughters within the following 1.6 ms trigger gate. -20 s veto on the cylinder with a radius of 0.8 m aligned with the muon track in case the track is reconstructed with OD signals. -120 s spherical veto with a radius of 1.3 m on each reconstructed neutron position in the 1.6 ms post-muon trigger gate. -full detector veto of 4 s after each muon crossing the ID.
This veto system comes at the cost of 15.8% exposure loss that is calculated with toy Monte Carlo (or, in other words by numeric integration with Monte-Carlo method) with fake events produced uniformly within the ID with the constant rate of 100 Hz.
The obtained spectrum is followed by the statistical subtraction of external background based on the radial distribution fit of each energy bin with the function described as: where N 0 (R) is the radial distribution of toy Monte Carlo events within the fiducial volume, λ is a free parameter that describes external gamma-background attenuation, and A and B correspond to the internal and external signal, respectively. Validity of this procedure was tested using the full detector Monte Carlo data [56] and provides reliable separation of external backgrounds which comes at the cost of increased uncertainty in each bin. The spectrum obtained corresponds to 298.4 kt day of exposure and has a significantly reduced background composition that can be described by known background components.

Analysis and results
As mentioned above, two different approaches have been used for studying the neutrino fluence associated with FRBs. First, the excess of the number of Borexino events was searched for in temporal correlation with the most intense FRBs selected from the existing databases. Then, the Borexino energy spectrum with high statistics was analyzed in order to determine the possible additional unaccounted contribution from (ν, e)-scattering and inverse beta-decay reactions.
The temporal correlation method is based on the fact that the radio fluence (which is supposed to be related to the neutrino fluence) from the time window of the most intense FRBs must be greater than the radio fluence from the window of background determination. The expected total radio fluence from the given time window is proportional to its time span Δt and the average radio flux from all FRBs F all . In the windows of the most intense FRBs, the radio fluence will be increased by the average fluence Φ 40 .
In order to calculate the F all and Φ 40 values, we used a power law index α = −1.4 for cumulative fluence distribution and the all-sky FRB rate of N 5 = 818 sky −1 day −1 above the fluence of 5 (Jy ms) obtained in [58]. A small additional contribution to F all from FRBs with the fluence ≤ 5(Jy ms) was made by adding 1200 uniformly distributed fluences in the (0 − 5)(Jy ms) range. As a result, the average flux from all FRBs turned out to be F all = 0.16 (Jy ms)s −1 (or 7.0 (Jy ms) per FRB) while the average fluence of FRBs with the fluence ≥ 40 (Jy ms) amounted to Φ 40 = 74(Jy ms).
Similar results were obtained from the analysis of specific FRBs. According to the CHIME data [58], the average radio fluence of all 536 FRBs is Φ all = 7.0 (Jy ms) per FRB, while for 12 FRBs with the fluence above 40 (Jy ms), the average equals to Φ 40 = 61.3 (Jy ms). Consequently, the average flux should be expressed as where N all is the number of all-sky FRB events per day (T = 24h = 86,400 s).
Thus, the excess of the expected neutrino events corresponding to the most intense FRB time intervals is defined by the factor r = Φ 40 /(Δt F all ). Since in our study we chose the length of the time window Δt = 2000 s, this ratio turns out to be r = 0.2 of the average neutrino flux.
Independently, we analysed the Borexino data in coincidence with FRB 200428 from magnetar SGR 1935+2154 . This event occurred on April 28, 2020 at the intragalactic distance of 9.5 kpc, thus yielding a very high fluence of 1.5×10 6 (Jy ms).
The biggest redshift z = 0.66 was observed for FRB 190523. We have considered the coincidence time window Δt = 2000 s centered at the FRB observation time with a width of ±1000 s covering a possible delay of sub-MeV neutrinos propagating at the sublight speed. For a distance corresponding to the z = 0.66 redshift, the delay should reach 1000 s in case of 0.6 MeV neutrinos with a rest mass of 70 meV, which is the upper limit on the heaviest neutrino mass state from the Planck 2015 data and oscillation mass squared differences [28].
The FRB arrival time could have its own delay associated with propagation through intergalactic plasma. The delay depends on the registered dispersion measure and the frequency ω at which the signal was recorded as ω −2 [1,2,71].
Only the Pushchino telescope [70] operating at a sufficiently low frequency of 109-113 MHz was able to register FRB 160920 with a significantly large delay of 620 s. Among 11 FRBs detected by the Pushchino telescope, only 6 FRBs have a signal delay exceeding 100 s. Higher working frequencies (up to 1 GHz) of all other telescopes result in delays below 100 s. However, these delays were calculated and taken into account in our analysis.
All selected FRBs had the data taking time above 95% of the corresponding time interval Δt.

Neutrino spectra
As noted above, the origin of FRBs is largely unknown. It is not even clear whether all of the observed radio bursts belong to the same type of physical processes. Among many different FRB models, there are several, such as neutron star mergers or supramassive neutron star collapses, which predict collateral neutrino and axion radiation [2,5]. In case of high-energy GeV-PeV neutrinos produced in hadronic processes, one would expect the power law spectrum ∼ E −2 ν . There is no reliable theory of the low-energy part of the FRB neutrino emission spectrum.
We calculated fluence limits on two different kinds of possible neutrino spectra: the monoenergetic line and the SN low-energy continuous spectrum. The latter was assumed as a quasi-thermal spectrum with the mean energy E and deviation from thermal distribution characterized by the pinching parameter α = 3 for all neutrino flavors (ν x ,ν x ) [72][73][74]. The emitted neutrino spectrum S(E ν ) depends on the neutrino energy E ν as: where T = E /(α + 1) is the effective temperature, which was considered to be the same for all neutrino flavors.

Temporal correlations for the most intensive FRBs
The goal of this analysis was to search for an excess of the selected events above the measured background, in coincidence with FRBs in a time window of Δt = 2000 s centered at the FRB arrival time. We calculated the overall number of candidate events above 250 keV in the Δt interval, which met the requirements for selection cuts of the described data. For reference, the Borexino events with an energy above 0.25 MeV produced within ± 5000 s of the most intensive Galactic FRB 200428 detection time are shown in Fig. 1. The closest events, with energies of 1.13 MeV and 1.49 MeV, occurred 105 s before and 539 s after the FRB arrival, respec-  No statistically significant excess of the difference between these spectra for any energy interval was observed.
We calculated the upper limits on fluences Φ ν x ,ν x for monoenergetic (anti)neutrinos with the energy E ν as: where N 90 (E ν , n obs , n bkg ) is the 90% C.L. upper limit for the number of FRB-correlated events in the (E th , E e max ) interval per single FRB, N e is the number of electrons in 145 t of the Borexino scintillator. The factor σ (E th , E e max ) represents the cross section for detected neutrinos (ν x ,ν x ) with the energy E ν without oscillations while recoil electrons are detected in the interval (E th , E e max ) [27]. The recoil electron detection efficiency was taken as 1, with the accuracy corresponding to the precision of the fiducial volume definition ( 1%). The numerator N 90 (E ν , n obs , n bkg ) was calculated taking into account the statistical compatibility between the correlated and uncorrelated FRB spectra and assuming Poisson statistics for the number of detected events in the energy interval (E th , E e max ). Here, n obs and n bkg denote overall numbers of events in the energy interval (E th , E e max ) detected in the time periods N FRB × Δt obs and N FRB × Δt bkg normalized by their respective times. The intervals Δt obs = 2 ks and Δt bkg = 18 ks were taken as ±1000 s and sum of [−10,000 . . . − 1000] s and [1000 . . . 10,000] s, correspondingly. The longer interval for background detection was chosen in order to reduce the error of n bkg that plays an important role in the Feldman-Cousins method. The value n bkg was normalized by the overall time ratio taking into account the actual live time of the detector within these time windows.
The procedure was repeated for neutrino energies E ν from 0.5 to 15 MeV in increments of 0.5 MeV. In order to have the best ratio of the expected effect with respect to the background and taking into account the shape of the spectrum (Fig. 2) in addition to the 0.25 MeV threshold, the 3.0 MeV threshold was used for higher neutrino energies. The upper limits on neutrino and antineutrino fluences of different flavors normalized per single FRB are shown in Fig. 3. The jump in the upper limit at energies above 7 MeV is associated with the inclusion of the above-mentioned 6.8 MeV event in the analysis.
These are the first constraints on the MeV neutrino fluxes obtained from the neutrino-electron scattering reaction. The average radio fluence of the most intensive FRBs and the limits on the neutrino fluence shown in Fig. 3  obtain the limit on the ratio (Φ ν /Φ FRB ) in (ν cm −2 /Jy ms) units.

allow us to
Since there is no reliable model for the low-energy neutrino spectrum for FRBs, we perform calculations of neutrino emission from a supernova collapse [72][73][74]. Assuming quasi-thermal distributions (5) with a mean energy E = 15.6 MeV and the parameter α = 3 and integrating over the analyzed electron recoil energy interval 0.25−15.0 MeV, we get the limits on the total electron neutrino fluence per single FRB: Φ(ν e ) ≤ 3.69 × 10 10 cm −2 (90% C.L.) that is about three times weaker than the limit obtained for monoenergetic neutrinos with the same energy. The values of the limits on other neutrino flavors obtained from the (ν, e)-scattering channel, as well as from the IBD reaction forν e , are given in Table 1.
We also calculated the upper limit on the electron antineutrinos (ν e ) fluence using the IBD reaction from the relation (6) but replacing N e with the number of protons N p , considering cross-section of IBD reaction and using the data acquired between December 2007 and October 2017 [29]. The data period considered includes only 19 FRB events above the threshold 40 (Jy ms). No IBD events were observed in the ±1000 s interval around the selected FRBs and the expected background was almost zero [29,46] that allowed us to use the conservative value of N 90 (E ν , n obs , n bkg ) = 2.44 in the analysis [76]. Since the cross section of IBD reaction is about two orders of magnitude larger than (ν, e)-scattering crosssections at given neutrino energies, and the background level is smaller, the most stringent upper limits have been obtained for the fluence of electron antineutrinos.  1-2 MeV region, and by 8 B solar neutrinos above 2 MeV. The background used in the fit procedure was described with the actual spectral components, such as 210 Po, 85 Kr, solar neutrino recoil electrons, 11 C, and 10 C. External gammas were statistically subtracted and thus were not included in the fit that was performed with the standard χ 2 likelihood function. The detector energy response was described according to [75] with additional empiric consideration of light quenching and Cherenkov radiation emission. The energy scale calibration and light quenching for αand β ± -particles were left as free parameters of the likelihood function [24]. The obtained count rates of all spectral components are in a good statistical agreement with previous publications [24,[40][41][42], but have larger uncertainties caused by the statistical subtraction procedure.
The additional component responsible for the potential FRB signal was added to the background and had a spectral shape of the monoenergetic line with the energy E ν or the supernova spectrum given by (5) with different E values. The limit on the number of events from the additional component was derived using the χ 2 profile as the value that corresponds to increase by (1.64) 2 with respect to the minimal value or the value at zero count rate in cases when the best-fit count rate value turned out to be negative. This limit N 90 (E ν ) corresponds to a confidence level of 90% and could be converted into limit on the FRB fluence as: where N e is the number of electrons in the FV scintillator and σ (E th , E ν ) is the (ν, e)-scattering cross section. The limits on the total fluence (time-integrated neutrino flux) during 2058 days of measurements obtained with this procedure for monoenergetic neutrinos of all flavors are shown in Fig. 5. Assuming an expected all-sky FRBs rate of N all = 2 × 10 3 per day [3,30], the limits per single FRB are 4 × 10 6 times stronger than those shown in Fig. 5. Comparing the limits obtained from the temporal correlation analysis (Fig. 3) and from the spectral fit (Fig. 5), one can see that the latter are about (1-3) ×10 4 times more stringent although they depend on the assumed all-sky FRB count rate N all .
Assuming that the neutrino fluence is proportional to the radio one and taking into account that, as shown in Section 4.1, the average fluence from all flares (7.0 (Jy ms) per FRB) is an order of magnitude less than the average fluence Φ 40 of the most intense ones, the limits on neutrino per radio fluence obtained from spectral analysis are only (1-3) ×10 3 times stronger than those obtained from the temporal analysis.
The same analysis was applied to the neutrino spectrum from a supernova given by Eq. (5). Figure 6 shows the 90% C.L. upper limits on fluences for supernova neutrino spectra with different mean energies E . The correlation of the expected neutrino signal with the components of the Borexino spectrum (Fig. 4) leads to the significant variations in the fluence upper limits observed in Figs. 5, and 6 depending on the neutrino energy E ν and E . For a value of E = 15.6 MeV, the upper limit per total fluence of ν e is Φ ν e ≤ 1.66 × 10 13 cm −2 . Taking into account the number of FRBs expected in 2058 days, the obtained limit turns out to be 9 × 10 3 times more stringent than the one obtained from the temporal analysis (Table 1).

Limits obtained from the absence of the (ν, e)-events above 13.6 MeV
As for the neutrinos with higher energies, the limits on ν e,μ,τ andν e,μ,τ were alternatively obtained using the fact that no events were observed above 13.6 MeV. The right boundary of the interval for the analysis was set to 16.8 MeV in accordance with the verified energy calibration of the data acquisition system. The different values of the monoenergetic neutrino energy E ν and the supernova neutrino mean energy E , the expected spectra of recoil electrons and the number of events N x in the interval 13.6-16.8 MeV were used in the calculations. According to the Feldman-Cousins approach to the case of no observed events with the conservative zero background,   The region of the neutrino energy up to 50 MeV was chosen in accordance with the characteristic energies of neutrinos appearing in the pion decay at rest. A sharp decrease in sensitivity to the neutrino fluence at the energies below 17 MeV occurs when the neutrino energy enters the 13.6-16.8 MeV interval. At higher energies, the limit becomes almost constant since the (ν, e)-scattering cross section is proportional to E ν and the spectrum of recoil electrons weakly depends on the electron energy (Fig. 7). The results of the spectral fit and the case of no observed events are also shown in Table 2 for monoenergetic neutrinos. One can see the validity of using different analysis methods. The spectral fit gives a better sensitivity to lower neutrino energies in the 0.5-14.0 MeV range while the second method allows expanding the neutrino energy range up to 50 MeV.
In case of the supernova neutrino spectrum, the fluence constraints based on the absence of events above 13.6 MeV becomes stronger than the monoenergetic neutrino limit starting from the mean energies above E ≥ 10 MeV. The resulting most stringent limits are given in Table 3. 4.6 Limits on theν e -fluence from the IBD reaction As already mentioned, electron antineutrinos can be also detected in Borexino via the neutron inverse β-decay (IBD) reaction on protons with an energy threshold of 1.8 MeV. The cross section of this process is much higher than the one for (ν e , e) elastic scattering. Additionally, the IBD offers a unique signature given by temporal and spatial coincidence of two correlated events associated with the detection of the positron and the neutron. The prompt positron event with a visible energy of E ν − 0.784 MeV accompanied by γ -rays from neutron capture mostly on protons or carbon nuclei with a small probability. As a result, the rate of the events selected as IBD candidates is much lower with respect to the rate of single electron-like events.
The present study of the electron antineutrino flux associated with FRBs is based on the data acquired between December 2007 and October 2017. The procedure of IBD events selection and the energy spectrum of prompt positron events are described in detail in [29]. After the application of all selection cuts the total live time decreases to 2485 days and the final efficiency of IBD reaction detection turns out to be 0.85 [29]. All electron antineutrino candidates were identified with the main DAQ system as well as the FADC system that provides a linear dynamic range up to ∼ 50 MeV. In this analysis, we used the same 16.8 MeV upper boundary of the antineutrino energy range as in the case of the (ν, e)-scattering analysis.
In order to estimate a limit on theν e fluence, we also exploited the fact that no events were observed with a prompt visible energy exceeding 7.8 MeV. Assuming two different neutrino energy spectra of monoenergetic and supernova neutrinos and no observed events within the 7.8 − 16.8 MeV interval, we obtain the upper limits on theν e fluences presented in Figs. 9, 10, Tables 2 and 3 (sixth column in each  table).
The limits on the fluences of monoenergeticν e with the energies below 7.8 MeV are based on the data from [29] in which the upper limits on theν e flux in the 1.8 − 7.8 MeV range were established for 1 MeV bins. The resulting conservative limits obtained by the Feldman-Cousins procedure with the expected background n bkg (excluding the cosmogenic component [29]) are shown in Fig. 9 and Table 2.
The limits in Figs. 9 and 10 are the limits on the total antineutrino fluence over a period of 2485 days. Since the expected number of FRBs during this time is ∼ 5 × 10 6 , the reduced limits per single FRB will be 5 × 10 6 times stronger.
The fluence upper limits can be converted into upper limits on the total energy radiated in the form of neutrinos. Here, we consider only the energy radiated by monoenergetic 10 MeV electron (anti)neutrinos assuming an isotropic angular distribution. The upper limits on the fluence of ν e ((ν e , e)scattering) andν e (IBD reaction) from the closest flare FRB 200428 lead to restrictions E ≤ 1.3 × 10 53 erg and E ≤ 4.8 × 10 51 erg, correspondingly.
The average of the inverse square of the distance to the registered FRBs corresponds to R = 400 Mpc. The upper limits for the total FRB fluences of 10 MeV ν e andν e obtained from spectral fit through the study of (ν e , e) elastic scattering and IBD reaction ( Table 2) gives weaker limits on the radiated energy E ≤ 4.7 × 10 57 erg/FRB and E ≤ 1.7 × 10 54 erg/FRB, correspondingly. This values can be compared with the energy of solar mass 1.8×10 54 erg. The most stringent restriction on the release of energy in the form of neutrinos obtained by us for FRB 200428 corresponds to The inset shows the Borexino spectrum ofν e -like events [29] 2.7×10 −3 solar mass. Limits on the energy radiated into neutrinos of other flavors can be easily calculated from Tables 1, 2 and 3. Figure 10 shows the IceCube upper limit on theν e fluence of the supernova spectrum with the mean neutrino energy E = 15.6 MeV and pinching the parameter α=3 (shown with a circle) based on a collective increase in the rate of hits in the detector in coincidence with 28 FRBs [20]. The IceCube limit can also be compared with the Borexino limit obtained from the temporal correlation analysis (Table 1, line 6, column 6). Due to different selection approach there are only 4 FRBs in the overlap between the sample of 28 FRBs considered in the IceCube analysis [20] and our dataset of 42 FRBs with fluence exceeding 40 (Jy ms). The Borexino detector is capable of detecting singleν e practically from the threshold of the IBD reaction that leads to significantly higher sensitivity to low energy electron antineutrino fluxes.

Conclusion
We looked for an excess in the number of events detected by Borexino produced by neutrino-electron elastic scattering and the inverse beta-decay on protons correlated to the most intense FRBs between 2007 and 2021. We found no statistically significant increase in the number of events, with the visible energy above 0.25 MeV within time windows of ± 1000 s centered at the time of FRB arrivals. As a result, new limits on the fluence of monochromatic neutrinos of all flavors were set for neutrino energies in the range of 0.5-15 MeV.  [20]. The inset shows the neutrino spectrum for E = 15.6 MeV (1) and expected Borexino spectrum (2). Arrows mark the analysis interval Another approach was based on the search for specific shapes of neutrino-electron scattering in the high statistic Borexino spectrum. The strongest limits on the fluences of monoenergetic neutrinos with energies in the range of 0.5 − 50 MeV and of the supernova neutrino spectrum given by the modified Fermi-Dirac distribution were obtained for different effective neutrino temperatures. Additionally, the inverse beta-decay reaction was considered to set a new limit on the fluence of electron antineutrinos related to FRBs. ons.org/licenses/by/4.0/. Funded by SCOAP 3 .