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36 results for “cosmic rays”
The Cosmic-Ray Energy Spectrum
<p>This plot shows a compilation of the cosmic-ray energy spectrum measured by several experiments (after 2000).</p> <p>References are listed in a dedicated GitHub <a href="https://github.com/carmeloevoli/The_CR_Spectrum">repository</a>.</p>
Supporting Information for "An empirical modification of the force field approach to describe the modulation of galactic cosmic rays close to Earth in a broad range of rigidities"
<p>This supporting information provides the Data Set S1 used to produce Fig. 6 in <strong>"An empirical modification of the force field approach to describe the modulation of galactic cosmic rays close to Earth in a broad range of rigidities"</strong> (Gieseler et al., 2017). It can be used to calculate the rigidity-dependent solar modulation potential <span class="math-tex">\(\phi(P)\)</span> for monthly intervals from 1973-2017 following Eq. 10 in Gieseler et al. (2017).</p> <p>If you use this data, please refer to and cite <strong>BOTH</strong> following publications:</p> <ul> <li>Gieseler, J., B. Heber, and K. Herbst, <em>An empirical modification of the force field approach to describe the modulation of galactic cosmic rays close to Earth in a broad range of rigidities</em>, J. Geophys. Res., 2017 (doi:10.1002/2017JA024763).</li> <li>Usoskin, I. G., G. A. Bazilevskaya, and G. A. Kovaltsov, <em>Solar modulation parameter for cosmic rays since 1936 reconstructed from ground-based neutron monitors and ionization chambers</em>, J. Geophys. Res., 2011 (doi:10.1029/2010JA016105).</li> </ul> <p>This data set contains the solar modulation potential values in MV for monthly intervals from 1973-2017 derived from the proton proxies IMP-8 He and ACE/CRIS C (Phi_pp), and from Usoskin et al. (2011) as provided by http://cosmicrays.oulu.fi/phi/phi.html (Phi_Uso11). The uncertainties of Phi_pp are given in column 4, those of Phi_Uso11 are 26 MV for the observed period. The LIS used to calculate the modulation potentials is that from Burger et al. (2000) as given by Usoskin et al. (2005).</p> <p>Column 1: Fractional year (start of interval)<br> Column 2: Month<br> Column 3: Phi_pp /MV<br> Column 4: Uncertainty of Phi_pp /MV<br> Column 5: Phi_Uso11 /MV</p> <p>Data also available at http://www.ieap.uni-kiel.de/et/ag-heber/cosmicrays</p>
Magnetic field data for "Cosmic Rays in Intermittent Magnetic Fields" (magnetic fields produced by the small-scale dynamo)
<p>Magnetic field data for the kinematic dynamo generated magnetic fields (KS) employed in the cosmic ray test particle simulations of Shukurov et al. 2017, <em>ApJL</em>, <strong>839</strong>, L16 [<a href="https://doi.org/10.3847/2041-8213/aa6aa6">https://doi.org/10.3847/2041-8213/aa6aa6</a>]. One dataset was also used in "Relative distribution of cosmic rays and magnetic fields", Seta et al. 2018, <em>MNRAS</em>, <strong>473 </strong>(4), 4544-4557 [<a href="https://doi.org/10.1093/mnras/stx2606">https://doi.org/10.1093/mnras/stx2606</a>]. These studies investigated the effects of magnetic field structure on charged test particle transport and trapping. See the README file for more details.</p> <p> </p>
Diffuse Emission of High-Energy Neutrinos from a Global Fit to Cosmic Rays
<p>Model of diffuse emission of high-energy neutrinos from a global fit of cosmic rays and model of high-energy neutrino emission from unresolved pulsar-powered sources.</p> <p>The maps presented in the form of <em>HEALPix </em>maps (Gorski et al 2005, ApJ, 622, 759) of per-flavor intensity in units of GeV<sup>-1</sup> cm<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup> at 50 logarithmically spaced energies between 10 GeV and 10<sup>8</sup> GeV. We use a value of NSIDE=256 and the RING binning scheme.</p> <p>We here make available our fiducial model, which is calculated assuming the <em>Ferrière 2001</em> cosmic ray source distribution, the <em>AAfrag</em> hadronic production cross sections and the <em>GALPROP</em> gas maps. We calculated the emission from unresolved sources following Vecchiotti et al. 2022, ApJ, 928, 19.</p> <p>In Version 2 of this dataset, we also make available the local cosmic ray fluxes of our fiducial model obtained from a global fit to cosmic ray data together with the corresponding 68% and 95% uncertainty bands. These are shown in figure 6 of <a href="https://arxiv.org/abs/2211.15607">arXiv:2211.15607</a>. The nuclear fluxes are in (GeV/n)<sup>-1</sup> m<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup>, the fluxes of electrons and positrons are in GeV<sup>-1</sup> m<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup> . The fluxes are local interstellar fluxes without solar modulation.</p> <p>In Version 3 of this dataset, we add the fiducial diffuse gamma ray model calculated assuming the <em>Ferrière 2001</em> cosmic ray source distribution, the <em>AAfrag</em> hadronic production cross sections as well as the <em>GALPROP</em> gas maps and ISRF model. We separately make available 3 maps: The hadronic emission on neutral atomic gas, the hadronic emission on molecular gas and the leptonic emission from Inverse Compton Scattering. </p> <p>Similar to the dataset of the fiducial neutrino model, the maps are presented in the form of <em>HEALPix </em>maps (Gorski et al 2005, ApJ, 622, 759) in units of GeV<sup>-1</sup> cm<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup>. We use a value of NSIDE=256 and the RING binning scheme. For the hadronic maps, the intensity is given at 50 logarithmically spaced energies between 10 GeV and 10<sup>8</sup> GeV. For the leptonic maps from Inverse Compton Scattering, the intensity is given at 48 logarithmically spaced energies between 1 GeV and 10<sup>6</sup> GeV.</p> <p>The structure of the files is somewhat different from the file containing the fiducial neutrino model. This is to allow for easy use of the gamma ray maps with the <em>gammapy</em> package (Deil et al. 2017, <a href="https://arxiv.org/abs/1709.01751"> arXiv:1709.01751</a>).</p> <p>Also available in Version 3 are the full spatio-spectral cosmic ray distributions in the Milky Way as predicted by our fiducial model. The nuclear fluxes are given for each species in (GeV/n)<sup>-1</sup> m<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup> at 63 energies between 1 GeV and 10<sup>9</sup> GeV. The leptonic fluxes are given for each species in GeV<sup>-1</sup> m<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup> at 36 energies between 1 GeV and 10<sup>5</sup> GeV. </p> <p>All fluxes are given on a spatial grid at 81 galactocentric radii from 0 kpc to 20 kpc and 61 distances perpendicular to the galactic plane between -6 kpc and 6 kpc.</p> <p>Finally, a word of caution about the extra component of cosmic ray leptons included in our model: This component is contained in the last <em>HDUnit</em> of the <em>fits</em> file containing the leptonic cosmic ray distributions. It is there denoted as a flux of electrons. It must, however, also be added to the flux of positrons to achieve correct results.</p> <p>Please refer to <a href="https://arxiv.org/abs/2211.15607">arXiv:2211.15607</a> for further details.</p> <p>When using these models in your research work, please refer to this Zenodo dataset and the publication.</p>
Buoy-based detection of low-energy cosmic-ray neutrons (Seelhausener See, July 15 to Dec 02, 2014)
<p>Contains two resources used in Schrön & Rasche et al. (2024):</p> <ol> <li><strong>Raw</strong> measurement data files from the buoy detector. Column names are provided in the header of the files. For detailed information about column names and descriptions, see the readme.</li> <li><strong>Processed</strong> measurement data of the buoy detector. Data has been stored as CSV files, the column names are described in `Buoy.csv.readme`. Additional PDF files show the corresponding plots. Two versions of data are provided: <ol> <li><strong>Buoy-1h</strong> contains data aggregated to 1 hour, and</li> <li><strong>Buoy-1h-mavg25</strong> contains the same data but the neutrons underwent a moving average filter with a window size of 25 (1 day).</li> </ol> </li> </ol> <p>Processing has been performed using Corny v0.8.2 (<a title="Corny" href="https://git.ufz.de/CRNS/cornish_pasdy">git.ufz.de/CRNS/cornish_pasdy</a>) with the configuration file <code>Buoy-1h.cfg</code>.</p>
Utilizing cosmic-ray positron and electron observations to probe the averaged properties of Milky Way pulsars
<p>We include here the Milky Way pulsars simulations that were created and used in "Utilizing cosmic-ray positron and electron observations to probe the averaged properties of Milky Way pulsars" of Cholis & Krommydas 2021. We include both the simulations before fitting to the cosmic-ray observations and the simulations whose electron and positron fluxes have been fitted to the AMS, CALET and DAMPE observations. See paper for further details.</p>
Possible counterpart signal of the Fermi bubbles at the cosmic-ray positrons
<p>This contains the files used in "Possible counterpart signal of the Fermi bubbles at the cosmic-ray positrons" paper by same authors to model the cosmic-ray electron and cosmic-ray positron flux for a possible cosmic-ray burst from the center of the galaxy. Please read paper for details. arXiv:2208.07880</p>
Figure 2. - A in High statistics measurement of the positron fraction in primary cosmic rays of 0.5-500 GeV with the alpha magnetic spectrometer on the international space station
Figure 2. - A: Sea lamprey (Petromyzon marinus); B: shad (either Alosa fallax or A. algeriensis). Scale bars = 10 cm. Photographs: M. JácomeFlores and B. Adrados.
Figure 1 in High statistics measurement of the positron fraction in primary cosmic rays of 0.5-500 GeV with the alpha magnetic spectrometer on the international space station
Figure 1. - Map showing previously known records of the sea lamprey (Petromyzon marinus) in north-western Africa (grey squares) and the record from the mouth of Oued Moulouya (black square). References for previous records: 1: Furnestin et al. (1958); 2: Boutellier (1918), adjacent records; 3: Dollfus (1955); 4: Bacha and Amara (2007); 5: records compiled by Renaud (2011).
The cosmic ray spectrum
<p>The cosmic ray spectrum. Compilation of data on charged cosmic rays, gamma-rays and neutrinos. When using the figure, please cite as follows:</p><blockquote><p>Figure by P. Mertsch, 2023; available at <a href="https://doi.org/10.5281/zenodo.10003566">https://doi.org/10.5281/zenodo.10003566</a> under a CC-BY4.0 license.</p></blockquote>
Fragmentation cross-sections for cosmic ray nuclei in the interstellar medium
<p>Table of the cumulative (included ghost nuclei) and direct fragmentation cross sections <strong>on H target</strong> generated with the <a href="https://github.com/carmeloevoli/XS4GCR">XS4GCR</a> code.</p> <p>More than 3800 channels are included from Ni64 to H1.</p> <ul> <li>Tables are saved as txt files with ' ' as delimiter.</li> <li>For each row the first 4 integers represent: fragment Z, fragment A, projectile Z and projectile A</li> <li>The following 160 values are the cross sections (in mbarn) as a function of the projectile kinetic energy per nucleon</li> <li>The first row is identified with 0 0 0 0 as the first 4 values and contains the values of the kinetic energy per nucleon (log spaced between 10 MeV/n and 1 TeV/n) at which the cross sections are computed.</li> </ul>
Cosmic Rays Scientists and Experiments - Outreach and Education Video
<p>How does a cosmic ray detector look like? Discover it in a worldwide journey, in company of scientists working on the detectors!</p> <p>An idea of Elisa Prandini, Michele Doro, Carolin Schwerdt and Sabine Hemmer</p> <p>Video produced for the 10th anniversary of the International Cosmic Day (https://icd.desy.de/).</p> <p>Presenter: Elisa Prandini</p> <p>Direction: Michele Doro</p> <p>Appearing in the movie: Andres Sandoval (HAWC), Ricardo Sato (Pierre Auger Observatory), Alice Donini and Lena Linhoff (MAGIC and LST), Carla Aramo (INFN underground Detector), Alexander Pokharukov (TAIGA), Mingjie Yang (LHAASO), Josh Veitch-Michaelis (IceCube Neutrino Observatory)</p> <p>We also thank the support from: Gabriella Cataldi and the Pierre Auger Observatory Staff, Daniel Mazin, Maximilian Noethe, Stefan Ohm, Madeleine O'Keefe, Flavio Seno, Martin Tluczykont, Simona Toscano, Flavia Violante, Martin Will, Martin Wolf, Cao Zhen, Sylvia Zhu</p> <p>Location: Aula Milla Baldo Ceolin, Physics and Astronomy Department, University of Padova</p>
KRAgamma cosmic-ray diffusion models
<p>These files contain the "KRAgamma" models for the the diffuse gamma-ray maps due to to pi0, Inverse Compton and Bremsstrahlung emission associated to the Galactic cosmic-ray population.</p> <p>The Galactic cosmic-ray sea is propagated in the Galaxy with the DRAGON code, according to the transport setup described in arXiv:1411.7623.</p> <p>The properties of the multi-TeV gamma-ray emission of the KRAgamma models are described in 1504.00227.</p>
Atmospheric Response Matrices (ARMs) computed with AtRIS in: The Atmospheric Influence on Cosmic-Ray-Induced Ionization and Absorbed Dose Rates
<p>Ionization and Dose Atmospheric Response Matrices (ARMs) computed with the Atmspheric Interaction Radiation Simulator (AtRIS) and used in the following publication: <br>The Atmospheric Influence on Cosmic-Ray-Induced Ionization and Absorbed Dose Rates.<br><br>All files are in txt format.<br>Files ending in '_energy_bins.txt', contain the informations about the energy binning of the primary particles used in the AtRIS simulations. <br>Files ending in '_ioni.txt', contain the ionization ARMs computed with the above mentioned energy binning.<br>Files ending in '_dose.txt', contain the ICRU water sphere dose ARMs computed with the above mentioned energy binning.</p>
Galactic cosmic ray fluxes for a number of nearby Sun-like stellar systems
<p>This data set corresponds to the simulation data presented in the article "Charting nearby stellar systems: The intensity of Galactic cosmic rays for a sample of solar-type stars" (Rodgers-Lee, Vidotto & Mesquita, MNRAS, 2021). Details of the stellar wind and cosmic ray model used for the simulations are available in the article.</p> <p>The data consists of the differential intensity of Galactic cosmic rays as a function of cosmic ray kinetic energy at different orbital distances from the star. The data is given for a number of different stellar systems. The first line gives the column headings.</p> <p>File names are formatted as "gcr_data_XXX.dat" where "XXX" corresponds to the name of the star considered. The simulation details can be found in Tables 1 and 2 of the article.</p>
Data in support to the manuscript: Testing a novel sensor design to jointly measure cosmic-ray neutrons, muons and gamma rays for non-invasive soil moisture estimation by Gianessi et al. (2024)
<p>The files contain data presented and discussed in the manuscript: Testing a novel sensor design to jointly measure cosmic-ray neutrons, muons and gamma rays for non-invasive soil moisture estimation by Gianessi et al. (2024).</p> <div> <div>Gianessi, Stefano, Matteo Polo, Luca Stevanato, Marcello Lunardon, Till Francke, Sascha E. Oswald, Hami Said Ahmed, et al. “Testing a Novel Sensor Design to Jointly Measure Cosmic-Ray Neutrons, Muons and Gamma Rays for Non-Invasive Soil Moisture Estimation.” <em>Geoscientific Instrumentation, Methods and Data Systems</em> 13, no. 1 (January 16, 2024): 9–25. <a href="https://doi.org/10.5194/gi-13-9-2024">https://doi.org/10.5194/gi-13-9-2024</a>.</div> </div> <p> </p>
Supporting information for "Incoming Neutron Flux Corrections for Cosmic-ray Soil and Snow Sensors Using the Global Neutron Monitor Network"
<p>This dataset includes 2 files that represent supporting information for McJannet, D and Desilets, D (Submitted 2023)"Incoming Neutron Flux Corrections for Cosmic-ray Soil and Snow Sensors Using the Global Neutron Monitor Network" Water Resources Research.</p> <p>File 1 - Supporting Information 1 - Example calculation: Excel sheet showing demonstration calaculations using the neutron intensity correction described in the paper</p> <p>File 2 - Supporting information 2 - List of neutron moniotr stations used in the paper and acknowledgment of their contribtuion</p>
Spectroscopy of the Cosmic Web: a view beyond collisional ionisation equilibrium with future X-ray telescopes
<p>This is a special seminar I gave at the Goddard Space Flight Center of NASA about my Ph.D. research at the Leiden University and the Netherlands Institute for Space Research SRON. Here you can download the presentation slides as well as the recording of the seminar. </p> <p> </p> <p>Abstract:</p> <p>In this talk I will focus on the X-ray view of the cosmic web filaments, more specifically the warm-hot intergalactic medium (WHIM). Hitomi kick-started an upcoming era of X-ray microcalorimeters which offer an unprecedented spectral resolution of diffuse sources. Many spectral signatures that could not yet have been studied will become feasible for the detection, and my presentation will focus on two of these spectral effects.</p> <p><br> Firstly, I will discuss how galaxy cluster photons alter the ionization state of nearby WHIM and affect the column densities of e.g. O VI, O VII, C V, or Ne VIII. Secondly,<br> I will discuss the feasibility of detecting the circum- and intergalactic medium in X-ray absorption using the extended intracluster medium as a backlight. For this study we used the cosmological hydrodynamical simulations Hydrangea (based on EAGLE) and we reported the feasibility of the detection of cosmic web filaments in OVII and in OVIII absorption with the microcalorimeter arrays onboard Athena and LEM. Last but not least, I will discuss my contribution to updating the cooling curve in the photoionisation model of the plasma code SPEX, and show the comparison to other plasma codes (MEKAL, APEC, Cloudy) and other atomic databases (CHIANTI, ADAS).</p>
Data in support to the paper: Comparison of Soil Water Content from SCATSAR-SWI and Cosmic Ray Neutron Sensing at four agricultural sites in Northern Italy: insights from spatial variability and representativeness by Emamalizadeh et al. (2024)
<p>The study was conducted within the 21GRD08 SoMMet project. The SoMMet project has received funding from the European Partnership on Metrology, co-financed from the European Union’s Horizon Europe Research and Innovation Programme and by the Participating States (funder name European Partnership on Metrology; funder ID 10.13039/100019599; grant no. 21GRD08 SoMMet).</p>
Discover Cosmic Rays - Outreach and Education video
<p>What are cosmic rays? When were they discovered? Where do they come from? How do scientists study them and why?</p> <p>Discover cosmic rays in this short video produced for the 10th anniversary of the International Cosmic Day (<a href="https://icd.desy.de/">https://icd.desy.de/</a>).</p> <p>From an idea of Elisa Prandini, Michele Doro, Carolin Schwerdt, and Sabine Hemmer</p> <p>Presenter: Elisa Prandini</p> <p>Direction: Michele Doro</p> <p>Location: Museum of History of Physics Giovanni Poleni, University of Padova</p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.