dataesr/scientific-paragraphs-categorization huggingface dataset:
Dark showers Exotic scenarios are discussed in Section 2. 10. The most likely dark shower (Section 2. 10. 3) signatures in kaon decays are K → πj and K → πj j , where j denotes a lepton jet consisting of e + e -pairs, photons and potentially missing energy. Depending on the mediator and final dark sector particle masses and lifetimes, the experimental signature can deform continuously from the prompt lepton jet signal in the case of short lifetimes all the way to just missing energy in case the lifetimes are sufficient for the dark sector particles to traverse the detector. A search for prompt lepton jets can be performed using the NA62 di-electron dataset (Section 3. 1). In case of pure missing energy signal, the results of the K → πX searches with X invisible (Section 4. 1) can be reinterpreted in terms of constraints on the parameters of the more complex dark sector.
Complementary probes in rare hyperon decays Authors: Dettori, Fornal, Geng, Kupsc, Martin Camalich, Martinez Santos, Shi, Wang Hyperons are the strange baryonic siblings of the nucleons and can lead to strangeness-changing decay signatures complementary to those of the kaons. Their lifetimes are O(10 - 10  ) s, significantly shorter than the K + and K L lifetimes O(10 -8 ) s  [255]. If kaonic and hyperonic amplitudes for the s → dX transition are of similar size (X are "dark sector" particles), we can expect the rare hyperondecay to be about two orders of magnitude less sensitive for a given dataset, due to the shorter lifetimes. On the other hand, hyperons do carry nonzero spin and baryon number, and are as such sensitive to the new physics interactions that are difficult or impossible to search for using kaons  [406].
Status and prospects at LHCb The LHCb experiment has reported the first evidence for the Σ + → pµ + µ -decay with Run 1 dataset, measuring the branching fraction to be  [416]  B(Σ + → pµ + µ -) = 2. 2 +1. 8 -1. 3 × 10 -8. This result is inconsistent with the HyperCP anomaly  [417]  and excludes the central HyperCP branching fraction value, while being consistent with the SM expectation. A yield of O(  10 3 ) candidates per year is envisaged in the LHCb upgrade, thanks to a more efficient trigger chain  [387]. This would lead to a sensitivity to the decay rate at a few percent level, and allow for a differential and forward-backward asymmetry measurements. In addition, CP violation can be studied by measuring the difference between the Σ + → pµ + µ -and Σ -→ pµ + µ -rates, and a full angular analysis probing the Lorentz structure in the s → dµµ currents is foreseen.
Flagship measurements The following searches for light dark sectors in kaon and hyperon decays would bring major improvements. Many of these searches can be performed with existing datasets. -Searches for the K + → π + X inv decay (performed with NA62 Run 1 dataset, Section 4. 1) should be extended into the mass range m X > 260 MeV, and pursued with future datasets. Also desirable would be the improvement of signal acceptance for m X = 0, which is currently limited at NA62 by the definition of the K + → π + ν ν signal and control regions. These measurements represent a unique probe into the Higgs mixed dark scalar (Section 2. 1) and ALP (Section 2. 2) phase space, and other models in which X particle does not decay preferentially to visible states. In particular, for the Higgs mixed scalar an improvement on B(K + → π + X inv ) by two orders of magnitude would close the gap to the BBN excluded region up to m ϕ = 200 MeV (Fig.
1 ). A similar improvement would also close the low mass range of the ALP parameter space, with the caveat that a comprehensive study of the BBN bounds for different ALP couplings is still missing. Searches for the K L → π 0 X inv decay (performed by KOTO, Section 4. 1) should be pursued with future datasets: they are complementary to the K + → π + X inv for m X in the vicinity of the π 0 mass. -Searches for resonances in the m spectra of K + → π + + -decays (Section 4. 6) , and the m γγ spectrum of the K + → π + γγ decays (Section 4. 5), including scans in the lifetime of the intermediate particle, should be pursued with the world's largest samples of these decays collected by NA62 to advance the study of the ALP phase space. Searches at future experiments would benefit from the development of dedicated trigger lines.
Studies of the K L → π 0 γγ decays (Section 4. 5) should be pursued with the KOTO dataset and future K L datasets. Improvement in sensitivity to resonance production by two orders of magnitude would close the gap to the constraints from beam dump searches for a significant ALP mass range (Figs. 9, 11), thus making K → πX inv the only phenomenologically viable ALP signature. -Improvement in sensitivity to the two-body K + → + X inv branching ratios by two orders of magnitude would start probing the seesaw neutrino mass models with O(100 MeV) sterile neutrinos (Fig. 14 ). Improvement in sensitivity to the three-body K + → µ + νX inv branching ratio by an order of magnitude would probe fully the preferred region for self-interacting neutrinos that may alleviate the Hubble tension (Fig. 18 ). Progress can be achieved with the future NA62 datasets (Section 4.
14). -First direct searches for the leptonic force mediator (Section 2. 5) in the K + → µ + νX decays, with X → µ + µ -and X → γγ should be performed with the available NA62 dataset (Sections 4. 15, 4. 16). These channels can probe a region of parameter space where these mediators can explain the muon g -2 anomaly. Searches at future experiments would benefit from the development of dedicated trigger lines. -Searches for emission of multiple dark sector mediators in kaon decays such as the K + → π + 2(e + e -) should be performed with the NA62 dataset (Section 4. 8) as they would be the first probes of a simple Higgsed U (1) d model for a dark photon in a particular region of parameter space (Section 2. 8). -The K → ππX inv (Section 4. 2) and B 1 → B 2 X inv (Section 5. 2. 2) decays of kaons and hyperons probe different couplings to those involved in the K → πX inv transitions, such as the CP violating couplings in the Higgs-mixed scalar model (Section 2.
1) and the axial couplings of the ALP (Sections 2. 2 and 5). The missing energy signature due to the ALP escaping the detector can also be replaced by the signatures due to a promptly decaying ALP, a → γγ or a → + -. Kaon measurements should be pursued with the available NA62 and KOTO datasets, and hyperon measurements with the BESIII and LHCb datasets.
Conclusions Rare kaon decays are among the most sensitive probes of both heavy and light new physics, as a combined consequence of both experimental and theoretical considerations. On one hand, large datasets are available in the current and future kaon experiments, two to three orders of magnitude larger than the usable B and D meson datasets at Belle, BaBar and LHCb. At the same time the kaon decay width is power suppressed, Γ K ∝ m 5 K /m 4 W , compared to the B and D mesons, Γ B,D ∝ m 5 B,D /m 4 W. For example, the total K + decay width is almost four orders of magnitude smaller than for the B + meson, Γ B + /Γ K + 7. 5 × 10 3. The small total decay width enhances the sensitivity to NP decay channels, B(K → X NP ) = Γ(K → X NP )/Γ K , so that the sensitivity to the same branching ratio value in reality corresponds to a sensitivity to a smaller NP partial decay width for rare kaon decays.
For instance, with two to three orders of magnitude larger datasets one could close the gap for Higgs-mixed scalar all the way to the BBN floor (Fig. 1 ). The searches for promptly decaying ALPs in K → πa decays, in either the a → γγ or the a → e + e -channel, could be improved such that the gap to constraints from beam dump searches would be closed (Figs. 9, 11). This would either lead to a discovery of the ALP, or leave K → πa inv , where a inv is and ALP that escapes the detector, as the only remaining phenomenologically viable possibility. An improvement in sensitivity to B(K + → + N ) by two orders of magnitude would start probing the minimal (vanilla) seesaw neutrino mass models for sterile neutrino masses in the O(100 MeV) regime (Fig. 14 ). An order of magnitude improvement on B(K + → µ + νX inv ) would probe fully the preferred region for self-interacting neutrinos that may alleviate the Hubble tension (Fig.
Acknowledgements We are grateful to  Brigitte Bloch-Devaux  for sharing tabulated NA48/2 results on rare kaon decay spectra, and for the discussion of the analysis. BD acknowledges support through  ERC-2018-StG-802836  ( AxScale  project). The work of BS is supported by the  US NSF  under Grant  PHY-1820770  and by the  Research Corporation for Science Advancement  through a  Cottrell Scholar Award. DSMA acknowledges support from  Los Alamos National Laboratory's Science Program Office , and from the  DOE Office of Science High Energy Physics  under contract number  DE-AC52-06NA25396. DW is supported by  Joint Large-Scale Scientific Facility Funds of the NSFC and CAS  under Contract No. U1832207 , and  National Key Research and Development Program of China  under Contract No. 2020YFA0406400.
KT is supported in part by the  US Department of Energy  grant  DE-SC0010102  and by  JSPS   KAKENHI 21H01086. The work of ME is supported by a Fellowship of the  Alexander von Humboldt Foundation. MT acknowledges the financial support from the  Slovenian Research Agency  (research core funding No. P1-0035 ). RXS acknowledges support from the  National Natural Science Foundation of China  under Grants No. 12147145 and Project funded by  China Postdoctoral Science Foundation  No. 2021M700343. RZ acknowledges support from the  European Union 's  Horizon 2020 research and innovation programme  under the  Marie Skłodowska-Curie  grant agreement No 860881-HIDDeN SH is supported in part by the  DOE  Grant  DE-SC0013607 , and in part by the  Alfred P. Sloan Foundation  Grant No. G-2019-12504. SS is supported by a  Stephen Hawking Fellowship  from  UKRI  under reference  EP/T01623X/1  and the  Lancaster-Manchester-Sheffield Consortium for Fundamental Physics , under  STFC  research grant  ST/T001038/1.
Data Analysis OTDR traces were recorded before, during and after irradiation. Data analysis consisted of calculating the slope of the trace over the FUT length. The reference trace was subtracted from the measured slope over time to overcome the intrinsic attenuation of the fiber and to follow the evolution of the RIA during both the irradiation and the recovery phases. The evolution of the Brillouin Gain Spectrum (BGS) was recorded using the BOTDA interrogator. Data post treatment consist of a Lorentzian fit of each BGS signature providing its Brillouin frequency and peak amplitude over time during and after the irradiation. In addition, thermocouples provide the temperature measurement (near the sample), which helps in correcting the measured BFS by the temperature-induced frequency shift in order to extract the RI-BFS (Radiation-Induced BFS) from the measured BFS response, which can be affected by temperature variations (~1 • C) in the irradiation chamber.
Formal Models. Sîrbu et al. [SPGK18]  use a model that updates probabilistically to investigate the effects of algorithmic bias on polarization by counting the number of opinion clusters, interpreting a single opinion cluster as consensus. Leskovec et al. [GG16]  simulate social networks and observe group formation over time. The Degroot models developed in  [DeG74]  and used in  [GJ10]  are closest to ours. Rather than examining polarization and opinions, this work is concerned with the network topology conditions under which agents with noisy data about an objective fact converge to an accurate consensus, close to the true state of the world. As already discussed the basic DeGroot models do not include confirmation bias, however [SSVL20, MBA20, MF15, HK02, CVCL + 20] all generalize DeGroot-like models to include functions that can be thought of as modelling confirmation bias in different ways, but with either no measure of polarization or a simpler measure than the one we use.
e. there are no voxel-to-voxel correspondences. We therefore exploit this potential to build a dataset of MRI, CT pairs. The training procedure is done first by gathering a curated dataset and then training the cycle GAN, usually for about two weeks of time, to ensure that during the training procedure, the GAN reaches an equilibrium, where the discriminator and the generator are on par. The developed AI model is then used for the generation of pseudo-CTs from TrueFisp images of the MR-Linac on 4 Nvidia gtx 2080ti GPUS in parallel. The training time was 131h with a maximum GPU usage of 18721MB.
The training procedure is shown in Figure1. A two-step process was used, meaning that the cycle GANs that generate the synthetic CTs are trained twice. The first training is performed between the 350 pairs of weakly aligned data from the pelvic planning CTs and the TrueFisp (0. 35T) MRIs. After this first step, the MR images used for training are converted to CT scans and aligned with the input CT scans based on deformable registration. The result of this registration is a new dataset of MR-CT pairs, where the pairs are much better aligned. Finally, a new cycle GAN is trained on this new dataset. This is the second training phase of our training procedure.
00(2) at any order n [see the orange squares in Fig. 1(c)] , confirming that the deviations in the (nonrandomized) experimental data are significant. The randomization method also yields a Poisson statistics when applied to the Mott insulator data set. Note that the results of the randomization method validate the algorithm used to compute the n-body correlations and provide a means to test the accuracy of the measured statistics  [47]. As discussed previously, deviations to a perfectly coherent state are expected in the presence of quantum and/or thermal depletion of the condensate. Here, we probe Bose superfluids with both a quantum and a thermal depletion as our experiment is performed with interacting bosons at finite temperature. In addition, both the BEC and its depletion contribute to the mode k = 0 since atoms are released from a harmonic trap.
We thank  S. Butera ,  A. Browaeys ,  I. Carusotto ,  T. Lahaye ,  T. Roscilde , and the members of the  Quantum Gas group at Institut d'Optique  for insightful discussions. We acknowledge financial support from the  Région Ile-de-France  in the framework of the DIM SIRTEQ, the  "Fondation d'entreprise iXcore pour la Recherche ," the  Agence Nationale pour la Recherche  (Grants No. ANR-17-CE30-0020-01  and No  ANR-22-PETQ-0004 ). D. C. acknowledges support from the  Institut Universitaire de France. A. A. acknowledges support from the  Simons Foundation  and from  Nokia-Bell Labs.
IV. STACK COMPARISON Across all four stacks, 27 devices in total were measured at 10K and their figures of merit are extracted and compared between different samples. Figure  4a  shows the dependence of H c normalized with temperature, which gives us the blocking temperature for devices of different stacks; Py: 45K, Ru:150K, Mg:230K and Ref:300K. These values will change within a range of ≈ 50 to 100K depending on the thickness of the storage layer and its area, but only Py based pillars showed T b < 50K. Fig. 4b  shows the dependence of FOM 1 with diameter, which increases for smaller pillar diameters. Assuming that the STT critical current density is constant, the current required for switching would decrease as 1/D 2 , which is in general agreement with the limited data set presented here.
X-Ray Observations IXPE observed 4U 1820-303 in two different periods: on 2022 October 11 from 13:53 to 22:55 UTC for a total exposure of ;16 ks per detector unit (DU) and from 2023 April 15 01:33 to April 16 23:17 UTC for a total exposure of ;86 ks per DU. During these periods, other observatories performed simultaneous observations. To determine the state of 4U 1820-303 during the IXPE observations, we analyzed the daily count rates in the 2-20 keV energy band from MAXI telescope 63     From this analysis, we can confirm that the HR values fluctuate around an average HR band as shown in Figure  4 ,thus, the source has not changed its state; only the data from observation ID (ObsID) 00014980055 (on April 15 since 00:41) show a slightly harder spectrum, but this hardening corresponds to a slightly higher counting rate, and it can be explained as due to pile-up  (Romano et al.
Polarimetric Analysis IXPE observed 4U 1820-303 twice, both times during its lower banana state; this suggests that the two observations have the same spectral properties, allowing us to merge them. From the point of view of the polarization, due to the lack of significant measurements before IXPE, this is something that we need to confirm by comparing the polarization in the first and in the second observation. At this aim, we used the IXPEOBSSIM software  (Baldini et al. 2022)  with the PCUBE algorithm to have a preliminary estimate of polarization. In the IXPE data, the background is negligible (roughly 2 orders of magnitude below the source in the whole energy band); thus, the prescription reported in Di  Marco et al. (2023)  for bright sources have been applied. IXPE in its nominal energy band reports an average polarization that is not significant in the first observation and has a low significance in the second.
Also combining the two data sets, we obtain a polarization below the 99% CL. The polarimetric analysis was performed using two energy bins: 2-4 and 4-8 keV, as reported in Figures  5(a ) and (b). The contour regions resulting from the two IXPE observations in both the energy bins are compatible allowing to combine the two data sets. We performed a study of the polarization using the combined data from the two IXPE observations by using the PCUBE analysis to measure the normalized Stokes parameters as a function of the energy with bins of 1 keV; the results are shown in Figure  6 , and reported in Table  1. We obtain that only the energy bin 7-8 keV has a highly significant polarization at 99. 99% CL. On the other hand, taking into account each energy bin as an independent data set, the statistical significance of this observation in any one bin has been evaluated; then, the CL for the polarization detection was tested assuming the ensemble of bins against the null hypothesis (i.
Spectral Analysis Using the data from NICER (in 0. 7-12 keV) and NuSTAR (in 3-30 keV)-see Appendix for details about data extraction -and IXPE (in 2-8 keV) weighted spectra (Di  Marco et al. 2022a ) and on the basis of the spectral models present in the literature  (Tarana et al. 2007; Titarchuk et al. 2013) , we applied the model tbabs * (diskbb+comptb) in XSPEC v. 12. 13. 0c  (Arnaud 1996). To estimate the absorption from the interstellar medium, we set the abundances at the wilm values  (Wilms et al. 2000). The NuSTAR residuals show an excess, as reported in Figure  7 , compatible with the presence of a broad iron line, such an excess is not appreciable in the IXPE and NICER data. Because of the excess in the NuSTAR residuals, we included in the model a Gaussian line: tbabs * (diskbb+comptb +Gauss).
9 -56 ± 10 -1. 1 ± 0. 9 -2. 5 ± 0. 9 6-7 1. 3 ± 1. 3 -57 ± 29 -0. 6 ± 1. 3 -1. 2 ± 1. 3 7-8 10. 3 ± 2. 4 -67 ± 7 -7. 1 ± 2. 4 -7. 5 ± 2. 4 2-4 0. 75 ± 0. 30 30 ± 11 0. 37 ± 0. 30 0. 66 ± 0. 30 4-7 2. 0 ± 0. 5 -55 ± 7 -0. 7 ± 0. 5 -1. 9 ± 0. 5 Note. Errors are reported at 68% CL. This model has been applied to fit a broadband spectrum of the combined simultaneous data set by NICER, NuSTAR, and IXPE. We also used the energy-independent cross-normalization factors. The best-fit parameters are summarized in Table  2. The EF E spectrum and its residuals are reported in Figure  8. To take into account NuSTAR calibration uncertainties  (Madsen et al. 2022) , we assumed a gain offset free in the fit, obtaining -(0. 085 ± 0. 009) keV and -(0. 068 ± 0. 008) keV for the focal plane modules Aand B(FPMA and FPMB), respectively; similarly for IXPE calibration uncertainties (Di Marco et al.
Radio Observation 4U 1820-303 was observed with the ATCA on 2021 April 15 from 12:49:40 and 21:51:20 UT (under project code CX530). During this observation, ATCA was in a relatively compact H214 configuration. The data were recorded simultaneously at two central frequencies, 5. 5 and 9 GHz, with 2 GHz of bandwidth at each frequency. We used the unpolarized PKS B1934-638 for primary calibration and to solve for antenna leakages. The nearby calibrator B1817-254 was used for gain calibration. Calibration and imaging followed standard procedures using the Common Astronomy Software Applications for radio astronomy (CASA, version 5. 1. 2; CASA Team et al. 2022). The polarization calibration used the CASA task atcapolhelpers. py and qufromgain routine. 65  The imaging used a Briggs robust parameter of 2 to maximize the image sensitivity.
Future studies of this source with a longer exposure could help to disentangle the polarization of each spectral component. Monitoring the source along its superorbital period or when it moves along the banana and island states could help to better understand the polarization variations and, thanks to this, verify possible geometry variations as a function of the mass accretion rate. NuSTAR performed coordinated observations, one (ObsID: 90802327002) from 2022 October 12 at 14:31 UTC to October 13 at 2:41 UTC with a total exposure of ;16. 9 ks and the other two on 2023 April 15 and 16 (ObsIDs: 90902308002 and 90902308004) with a total exposure of ;16. 8 and ;15. 2 ks, respectively. The NuSTAR data were processed with the standard Data Analysis Software (nustardas 16Feb22 v2. 1. 2) provided under HEASOFT v6.
Acknowledgments The Imaging X-ray Polarimetry Explorer (IXPE) is a joint US and Italian mission. The US contribution is supported by the  National Aeronautics and Space Administration (NASA)  and led and managed by its  Marshall Space Flight Center (MSFC) , with industry partner  Ball Aerospace  (contract  NNM15AA18C ). The Italian contribution is supported by the  Italian Space Agency (Agenzia Spaziale Italiana, ASI)  through contract  ASI-OHBI-2017-12-I. 0 , agreements  ASI-INAF-2017-12-H0  and  ASI-INFN-2017. 13-H0 , and its  Space Science Data Center (SSDC)  with agreements  ASI-INAF-2022-14-HH. 0  and  ASI-INFN 2021-43-HH. 0 , and by the  Istituto Nazionale di Astrofisica (INAF)  and the  Istituto Nazionale di Fisica Nucleare (INFN) in Italy. This research used data products provided by the  IXPE Team (MSFC ,  SSDC ,  INAF , and  INFN)  and distributed with additional software tools by the  High-Energy Astrophysics Science Archive Research Center (HEA-SARC) , at  NASA Goddard Space Flight Center (GSFC).
Overlap estimation To investigate how analyses can be combined to provide the most stringent constraints on a BSM model point, we choose the selection of analyses available both in SMOD-ELS and MADANALYSIS 5 as our database. At the time of writing this includes 18 analyses: ATLAS-SUSY-2013-02  [8] , ATLAS-SUSY-2013-04  [9] , ATLAS-SUSY-2013-05  [10] , ATLAS-SUSY-2013-11  [11] , ATLAS-SUSY-2013-21  [12] , ATLAS-SUSY-2015-06  [13] , ATLAS-SUSY-2016-07  [14] , ATLAS-SUSY-2018-04  [15] , ATLAS-SUSY-2018-06  [16] , ATLAS-SUSY-2018-31  [17] , ATLAS-SUSY-2018-32  [18] , ATLAS-SUSY-2019-08  [19] ; CMS-SUS-13-011  [20] , CMS-SUS-13-012  [21] , CMS-SUS-16-033  [22] , CMS-SUS-16-039  [23] , CMS-SUS-16-048  [24]. CMS-SUS-17-001  [25] , and CMS-SUS-19-006  [26]. The cascade decays, or topologies, covered by these analyses are simplified so that they focus on the production of two massive BSM states that each decay to at most 2-3 finalstate particles.