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36 results for “cosmic rays”
Data for '3D Radio Frequency Mapping and Polarization Observations Show Lightning is Ignited by Cosmic-ray Shower' by Shao et al., 2024
<p>Data for manuscript "<a name="_Hlk177653706"></a><strong><span>3D Radio Frequency Mapping and Polarization Observations Show Lightning is Ignited by Cosmic-ray Shower" <br></span></strong></p>
Thunderstorm charge distribution determination using cosmic rays induced air showers and lightning imaging at LOFAR
Open the record for dataset details and reuse information.
The cosmic web of X-ray active galactic nuclei seen through the eROSITA Final Equatorial Depth Survey (eFEDS)
<p>Which galaxies in the general population turn into active galactic nuclei (AGN) is a keystone of galaxy formation and evolution.</p> <p>Thanks to SRG/eROSITA’s contiguous 140 square degrees pilot survey field, we constructed a large, complete, and unbiased soft<br> X-ray flux-limited AGN sample at low redshift 0.05 < z < 0.55. Two summary statistics, the clustering using spectra from SDSS-V<br> and galaxy-galaxy lensing with imaging from HSC, are measured and interpreted with halo occupation distribution and abundance<br> matching models. Both models successfully account for the observations. We obtain an exceptional complete view of the AGN 12<br> halo occupation distribution. The population of AGN is broadly distributed among halos with a mean mass of 3.9+2.0−2.4 × 10 M⊙ .<br> +0.08. This corresponds to a large-scale halo bias of b(z = 0.34) = 0.99−0.10 . The central occupation has a large transition parameter σlog10 (M) = 1.28 ± 0.2. The satellite occupation distribution is characterized by a shallow slope αsat = 0.73 ± 0.38. We find that AGNs in satellites are rare, with fsat < 20%. Most soft X-ray-selected AGNs are hosted by central galaxies in their dark matter halo. A weak correlation between soft X-ray luminosity and large-scale halo bias is confirmed (3.3σ). We discuss the implications of environmental-dependent AGN triggering. This study paves the way towards fully charting, in the coming decade, the co-evolution of X-ray AGN, their host galaxies, and dark matter haloes by combining eROSITA with SDSS-V, 4MOST, DESI, LSST, and Euclid.</p>
Reconstruction of simulated air shower footprints measured at a hypothetical ground-based cosmic-ray observatory
<p>Ultra-high energy cosmic rays produce extensive air showers of secondary particles upon entering the atmosphere. Sampling the footprint of these particles with surface detectors is a widely used detection technique. In this data set, the reconstruction of cosmic-ray properties like the shower maximum using the measured particle footprint can be investigated.</p> <p>The Observatory features 9 x 9 stations arranged in a Cartesian grid with a spacing of 1500 m. Each station can measure the time-dependent signals in a window of 80 bins a 25 ns.</p> <p>The data were simulated using a modified version of <a href="https://git.rwth-aachen.de/DavidWalz/airshower">https://git.rwth-aachen.de/DavidWalz/airshower</a> and used in <a href="https://arxiv.org/abs/2107.00656">https://arxiv.org/abs/2107.00656</a>.</p>
Hybrid origins of the cosmic-ray nuclei spectral hardening at a few hundred GV
<p>This dataset includes the posterior distribution samples of Scheme I, II, and III in the article.</p>
Data and Scripts used in "Analysis of Relations Between Solar Activity, Cosmic Rays and Earth Climate Using Machine Learning Techniques"
<p>This archive contains the data in relation to the work:</p> <p>Analysis of relations between solar activity, cosmic rays and earth climate using machine learning techniques<br> B. Belen, U. M. Leloglu, and M. B. Demirkoz </p> <p>See README file for more details.</p>
On the Combined Role of Cosmic Rays andSupernova-Driven Turbulence for Galactic Dynamos
<p>"b_data_cr.h5" contains the data from the model CR</p>
Subnanosecond scintillation detector for high energy cosmic rays Project
<p>The task objective is to develop a gamma ray scintillator technology with subnanosecond temporal resolution and the capability to withstand unprecedented rates and doses of high energy gamma radiation. This is a joint project with Caltech Prof. Dave Hitlin to detect BaF2 fast scintillation (&tau;&nbsp;~&nbsp;0.9ns at &lambda;&nbsp;~&nbsp;220nm) while rejecting slow scintillation (&tau;&nbsp;~&nbsp;650ns at &lambda;&nbsp;~&nbsp;330nm). We will also develop solar blind coatings using ALD technology for DUV bandpass filter.</p>
Deep Mapping of Small Solar System Bodies with Galactic Cosmic Ray Secondary Particle Showers Project
<p>Our Phase I study demonstrated that&nbsp;muons, the long-range charged component of GCR showers, can penetrate SSBs on the order of a km in diameter or less, providing&nbsp;information on their interior structure. Muons produced in Earth&rsquo;s atmosphere have been applied to image the interior of large&nbsp;objects, such as the Great Pyramids and volcanos. In Phase I, we found that the production of muons in the solid surfaces of airless&nbsp;bodies is much smaller than in Earth&rsquo;s atmosphere. Nevertheless, the flux of transmitted muons is sufficient to detect inclusions within&nbsp;an asteroid or comet in a reasonable period of time, ranging from hours to weeks, depending on the size of the SSB and the density&nbsp;contrast, position and size of the inclusion. The intrinsic spatial resolution of muon radiography (&ldquo;muography&rdquo;) is on the scale of&nbsp;a few meters. The spatial resolution that can be achieved in practice depends on signal intensity and integration time, the angular&nbsp;resolution of the muon tracker (hodoscope) and details of data reduction and analysis methodology.</p><p>Our Phase II project will continue to assess remaining unknowns for the application of muography to determining the interior&nbsp;structure of SSBs, assess risks for implementation, and provide a roadmap for development of SSB muography beyond the NIAC&nbsp;program. To achieve our objectives, we will work on four interrelated tasks:</p><ul><li>Signal and background characterization: Characterize the production and transmission of muons and secondary particle backgrounds&nbsp;made by cosmic ray showers in SSBs;</li><li>Imaging studies: Develop methods to determine the density structure of SSB interiors and near-surface features from radiographic and&nbsp;tomographic data;</li><li>Instrument design: Using simulations and bench-top laboratory experiments, investigate specific concepts for the design of compact&nbsp;hodoscopes that can be deployed on a spacecraft or in situ;</li><li>Synthesis: Determine the range of applicability of the concept, identify the steps needed for maturation of the concept, and explore&nbsp;concepts for a pilot muography mission.</li></ul><p>Successful implementation of SSB muography requires a thorough understanding of muon production and transmission as well as&nbsp;sources of background. Phase I demonstrated that muon production is sensitive to the density of the top-most meter of the regolith.&nbsp;Thus, unknown variations in regolith density may obscure interior structure. Limb imaging of muons and the use of radar data&nbsp;to remotely map near-surface density will be explored as possible ways to mitigate variations in muon production. A compact,&nbsp;inexpensive system that could be deployed on a spacecraft or in situ appears to be feasible and warrants further study. A successful&nbsp;design must be capable of separately measuring the transmitted muon signal from the primary GCRs and secondary particles that&nbsp;scatter into the field-of-view of the hodoscope. This can be accomplished, for example, using Cherenkov radiators to reject lower&nbsp;energy scattered particles and to determine particle direction. Concepts for imaging systems identified in Phase I will be scrutinized.</p><p>Phase II will be carried out by a multidisciplinary project team with broad experience in cosmic ray physics, remote sensing,&nbsp;meteoritics and planetary science. While the development of muography for SSBs is risky, the potential benefits are significant.&nbsp;There are presently no established methods to directly characterize the interior structure and macroporosity of an asteroid or comet.&nbsp;Muography could provide a direct and cost-effective means of probing the interior density structure.
Simulated Galactic Cosmic Ray Exposure Activates Dose-Dependent DNA Repair Response and Downregulates Glucosinolate Pathway in Arabidopsis Seedlings
This study's objective was to develop an understanding of the biological effects of space radiation on plants with the goal of producing fresh food during long duration space missions to support astronauts' nutritional and psychological needs.10-day-old Arabidopsis seedlings were exposed to simulated Galactic Cosmic Rays (GCR) and assessed for transcriptomic changes. The simulated GCR irradiation was carried out in the NASA Space Radiation Laboratory (NSRL) at Brookhaven National Lab (BNL). The exposures were conducted acutely for two dose points at 40 cGy or 80 cGy, with sequential delivery of proton, helium, oxygen, silicon, and iron ions. Control and irradiated seedlings were then harvested and stabilized in RNAlater at 3 hrs. post irradiation. Total RNA was isolated for transcriptomic analyses using RNAseq. The data revealed that the transcriptomic responses were dose-dependent, with significant upregulation of DNA repair pathways and downregulation of glucosinolate biosynthetic pathways. Glucosinolates are important for plant pathogen defense and for the taste of a plant, which are both relevant to growing plants for spaceflight. These findings fill in knowledge gaps of how plants respond to radiation in beyond-Earth environments.
ULY JUP GRB SOLAR X-RAY/COSMIC GAMMA-RAY RAW COUNT RATE
The archived data consist of count rates from the sum of two hemispherical detectors covering 4 pi steradians and operating continuously. The detectors are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but the below table should be consulted to find the accurate thresholds for any day of the mission. Although the prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x- radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992 (particles in the Jovian magnetosphere). The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds.
Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) High Energy Telescope (HET) Ion and Electron Spin-Averaged Coincidence Counting Rates, 10 min Data
This Data Set contains 10 min Average Ion and Electron Spin-Averaged Coincidence Counting Rates from the COSPIN High Energy Telescope (HET). The Parameter Keys in the Parameter Level Segments below are specifically relevant to the UFA accessible Versions of the Data.
Voyager 1 Cosmic Ray Subsystem (CRS) Proton and Helium Energy Fluxes, Level H3 (H3), Daily Data
The joint California Institute of Technology, Caltech, Goddard Space Flight Center, GSFC, Cosmic Ray Subsystem, CRS, experiment on Voyager consists of three types of solid state detector telescopes: * Two High Energy Telescopes: HET-I and HET-II * Four Low Energy Telscopes (dE/dx versus E): LET A, LET B, LET C, and LET D * The Electron Telescope, TET The HETs and LETs are redundant and are designed to complement each other and to cover a broad range in energy, intensity, and charge spectra. The HETs covered an energy range between 6 MeV/n and 500 MeV/n for nuclei ranging in atomic numbers from 1 through 30. In addition, electrons in the energy range between 3 MeV and 100 MeV were measured by this telescope and an electron telescope. The LETs measured the energy and determined the identity of nuclei for energies between 0.15 MeV/n and 30 MeV/n and atomic numbers from 1 to 30. The instruments also measured the anisotropies of electrons and nuclei. The CRS looks only for very energetic particles in plasma, and has the highest sensitivity of the three particle detectors. Very energetic particles can often be found in the intense radiation fields surrounding some planets (like Jupiter). Particles with the highest-known energies come from other stars. The CRS looks for both. The CRS makes no attempt to slow or capture the super-energetic particles. They simply pass completely through the CRS. However, in passing through, the particles leave signs that they were there. Cosmic Ray Subsystem Science Objectives: * To measure the energy spectrum of electrons from 3 Mev to 110 MeV. * To measure the energy spectra and elemental composition of all cosmic ray nuclei from hydrogen through iron over an energy range from approximately 1 - 500MeV/nuc. * To provide information on the energy content, origin, acceleration process, life history, and dynamics of cosmic rays in the galaxy, and contribute to an understanding of the nucleosynthesis of elements in cosmic ray sources. * To provide information on the transport of cosmic rays, Jovian electrons, and low energy interplanetary particles over an extended region of interplanetary space. * To measure the three-dimensional streaming patterns of nuclei from Hydrogen through Iron and electrons over an extended range. * To measure particle charge compostion in the magnetosphere of Jupiter, Saturn, Uranus, and Neptune.
ACE Cosmic Ray Isotope Spectrometer (CRIS) Daily Level 2 Data
ACE Cosmic Ray Isotope Spectrometer (CRIS) intensities and counts, for each of 7 energy bins for each of 24 elements (Z=5, boron, to Z=28, nickel) at 1-hour time resolution. Overall energy ranges coveredgo from 49-172 MeV/n for boron to 130-496 MeV/n for nickel. Calibrated science quality data. Parameter segments below address intensities but not alsothe count rates included in the data set. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. Daily averaged L2 fluxes and rates are also available from these access paths. The "parameter keys" given below are as used by CDAWeb.
ULY JUP GRB SOLAR X-RAY/COSMIC GAMMA-RAY RAW COUNT RATE
The archived data consist of count rates from the sum of two hemispherical detectors covering 4 pi steradians and operating continuously. The detectors are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but the below table should be consulted to find the accurate thresholds for any day of the mission. A more complete description of the instrument may be found in [HURLEYETAL1992] and [COTINETAL1983]. Although the prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x- radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992 (particles in the Jovian magnetosphere). The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds.
ACE Cosmic Ray Isotope Spectrometer (CRIS) 1-Hour Level 2 Data
ACE Cosmic Ray Isotope Spectrometer (CRIS) intensities and counts, for each of 7 energy bins for each of 24 elements (Z=5, boron, to Z=28, nickel) at 1-hour time resolution. Overall energy ranges covered go from 49-172 MeV/n for boron to 130-496 MeV/n for nickel. Calibrated science quality data. Parameter segments below address intensities but not also the count rates included in the data set. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. Daily averaged L2 fluxes and rates are also available from these access paths. The "parameter keys" given below are as used by CDAWeb.
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Allen Brain Atlas
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DANDI Archive for NWB datasets
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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.