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This preliminary data release contains alerts previously presented at the 39th International Cosmic Ray Conference (ICRC 2025), see PoS(ICRC2025)1224. IC-170922A — in spatial coincidence with the blazar TXS 0506+056, representing the first association between a neutrino alert and an astrophysical source. IC-220424A and IC-230416A — in spatial coincidence with NGC 7469. IC-200530A, IC-191119A, and IC-191001A — previously identified in spatial coincidence with several Tidal Disruption Events. In addition to these events, we also include IC-230724A in this preliminary release. Its inclusion is motivated by the fact that it was a promising Gold alert, with an average probability of astrophysical origin of 53%. An issue in the automatic processing pipeline responsible for the offline reconstruction delayed the distribution of its updated position (https://gcn.nasa.gov/circulars/34265). To ensure timely availability at the time, an alternative reconstruction algorithm was applied. Following the update of the reconstruction algorithms for high-energy track alerts in September 2024 (https://roc.icecube.wisc.edu/public/docs/IceCube_Update_Muon_Alert_Reco.pdf), the new position and the alert-related parameters have now been recalculated. In the following months, the full catalog IceCat-2 will be publish, together with a related publication. 

{"Abstract":["Data and plotting scripts for reproducing plots from "Physics potential of the IceCube Upgrade for atmospheric neutrino oscillations". Please refer to the related publication for a detailed explanation of the sample and analysis.\n<br><br>\nContents: \n<ol>\n<li> <code>README.md</code> contains useful information about the contents of this data release.</li>\n<li> <code>example.py</code> Example script demonstrating how to load the csv files, plot the chi squared map, and extract the 90% sensitivity contours shown in Figures 11 and 15.</li>\n<li> <code>modchi2map_nufitwoSK.csv</code> chi2 map used to produce Figure 11 (left), in which the injected truth point is the best fit point from <a href="http://www.nu-fit.org/sites/default/files/v52.tbl-parameters.pdf">NuFit 5.2 w/o SK (upper panel)</a>, sin²(&theta;₂₃)=0.572 and &Delta;m²₃₂=2.43&times;10^-3 eV².</li>\n<li> <code>modchi2map_nufitwSK.csv</code> chi2 map used to produce Figure 11 (right), in which the injected truth point is the best fit point from <a href="http://www.nu-fit.org/sites/default/files/v52.tbl-parameters.pdf">NuFit 5.2 w/ SK (lower panel)</a>, sin²(&theta;₂₃)=0.451 and &Delta;m²₃₂=2.43&times;10^-3 eV².</li>\n<li> <code>modchi2map_icecube.csv</code> chi2 map used to produce Figure 15, in which the injected truth point is the best fit point from the latest published IceCube DeepCore oscillation result <a href="https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.134.091801">Phys. Rev. Lett. 134, 091801 (2025)</a>, sin²(&theta;₂₃)=0.54 and &Delta;m²₃₂=2.40&times;10^-3 eV².</li>\n</ol>\n\nPlease note: The CSV files are available for download through dataverse in either csv or tab format."]} 

{"Abstract":["This sample contains the data used in the Measurement of atmospheric neutrino mixing with improved IceCube DeepCore calibration and data processing, published in Phys. Rev. D 108, 012014 (2023). Please refer to the publication <a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.108.012014">here</a> for a detailed explanation of the sample and analysis."]} 

Data and plotting scripts for reproducing plots from Search for High-Energy Neutrinos From the Sun Using Ten Years of IceCube Data Contents: - paper_plots.h5: Data used to make plots - paper_plots.py: Python script for making plots - paper.mplstyle: Matplotlib style file to set plotting defaults - README.md 

{"Abstract":["Results of the Search for eV-scale sterile neutrinos with the DeepCore "golden" sample in machine readable format. Allows reproduction of Figure 5 of the publication.\n\n<ul>\n<li> The file "wilks_contour_90pct.csv" contains the 90% contour line in CSV format. The columns "U\\mu4_sq" and "U\\tau4_sq" correspond to the _squared_ elements of the 3+1 mixing matrix, |U_{&mu;4}|^2 and |U_{&tau;4}|^2, respectively. The contour was drawn assuming that Wilks' theorem holds with two degrees of freedom. The points are ordered by nearest neighbors. </li>\n<li> The file "expected_sensitivity_90pct.csv" contains the expected sensitivity at 90% CL of the analysis for Asimov data produced at the null hypothesis. The format is identical to that of the result. </li>\n<li> The files "marginalized_umu4_sq.csv" and "marginalized_utau4_sq.csv" contain the marginalized scan of the test statistic over the matrix elements. The column "Metric Difference" refers to the delta chi-square metric used in the analysis. Since this metric is a delta chi-square (rather than a likelihood), it should _not_ be multiplied by two when calculating significances. They allow reproduction of the top and right panels of Figure 5 of the publication. </li>\n<li> The file "real_data_wilks_contours_reprod_mar_2025_best_fit_points.tab" contains the best-fit values of all free nuisance parameters in a |U_{&mu;4}|^2 and |U_{&tau;4}|^2 scan. </li>\n<li> The file "real_data_wilks_contours_reprod_mar_2025_metric_diff.tab" contains the \\chi^2 difference between the scan point and the global best-fit in a |U_{&mu;4}|^2 and |U_{&tau;4}|^2 scan. </li>\n</ul>"]} 

<h1 id="summary">Summary</h1> <p>Title: Data Release for A search for extremely-high-energy neutrinos and first constraints on the ultra-high-energy cosmic-ray proton fraction with IceCube</p> <p>The IceCube observatory analyzed 12.6 years of data in search of extremely-high-energy (EHE) neutrinos above 5 PeV. The resultant limit of the search (Fig 1), and the effective area of the event selection (Fig 7), are provided in this data release.</p> <h1 id="contents">Contents</h1> <ul> <li><p>README file: this file</p> </li> <li><p><code>differential_limit_and_sensitivity.csv</code>: a comma separated value file, giving the observed experimental differential limit, and sensitivity, of the search as a function of neutrino energy. This is the content of Fig 1 in the paper. The first column is the neutrino energy in GeV. The second column is the limit in units of GeV/cm2/s/sr. The third column is the sensitivity in units of GeV/cm2/s/sr.</p> </li> <li><p><code>effective_area.csv</code>: a comma separated value file, giving the effective area of the search as a function of energy. This is the content of Fig 7 in the paper. The first column is the neutrino energy in GeV. The second column is the total effective area of the search, summed across neutrino flavors, and averaged across neutrinos and antineutrinos, in meters-squared. The third column is the effective area of the search for the average of electron neutrino and electron antineutrinos in units of meters-squared. The fourth column is the same as the third, but for muon-flavor neutrinos. The fifth column is the same as the third and fourth, but for tau-flavor neutrinos.</p> </li> <li><p><code>demo.py</code>: a short python script to demonstrate how to read the files. Run like <code>python demo.py</code>. A standard base python installation is sufficient, as the only dependencies are numpy and matplotlib.</p> </li> </ul> <h1 id="contacts">Contacts</h1> <p>For any questions about this data release, please write to analysis@icecube.wisc.edu</p>