Find research datasets worth reusing

opencc-by-4.0Dec 2020View details →

Datasets for "Hydrodynamic and hydromagnetic energy spectra from large eddy simulations"

<pre>This directory contains an index.html file with links to the run directories and idl plotting routines with secondary data for the other figures for the paper "Hydrodynamic and hydromagnetic energy spectra from large eddy simulations" Haugen & Brandenburg. If anything turns our to be incomplete, please email brandenb@nordita.org.</pre>

opencc-by-4.0Dec 2020View details →

Energy spectra and eigenvectors of the sine-Gordon and double sine-Gordon model

This dataset contains low-energy spectra and eigenvectors of two (1+1)-dimensional Quantum Field Theory models, the sine-Gordon (SG) and the double sine-Gordon (DSG) model, for a representative choice of parameter values. The data were computed using the Truncated Conformal Space Approach (TCSA), which is a Hamiltonian truncation method.   Parameters: <ul> <li>Cosine frequencies: β = 2.49239 for SG and β1 = 1.01066 and β2 = 2.49239 for DSG</li> <li>Dimensionless (mass)⨉(system size) parameter (m: first SG breather mass, L: system size): mL = 0.01, 0.1, 1, 2, 5</li> </ul> TCSA details:  <ul> <li>truncation basis: free massless boson CFT with Dirichlet boundary conditions, restricted to the ground state symmetry sector</li> <li>truncation cutoff (maximum CFT energy shell): 42 </li> <li>basis size: 85674</li> </ul> The spectra correspond to the full list of eigenvalues of the truncated Hamiltonian matrices in increasing order, and the eigenvectors correspond to matrices of dimensions 5173⨉5173, corresponding to the components of the lowest 5173 energy levels in the lowest 5173 basis states (the best convergent part of the eigenvector matrix at the top left corner). Each eigenvector corresponds to a column of the above matrices, in the same order as the eigenvalues. Format: Python NumPy .npy files The filenames are of the form: descriptor_model_mLx.npy where: descriptor = "Spectrum" or "Eigenvectors"  model = "SG" or "DSG" x = 0.01, 0.1, 1, 2 or 5 (mL value)

opencc-by-4.0Nov 2023View details →

Energy characteristics and the source of a ball lightning obtained by investigating its spectra

This work, based on quantitative spectrometric analysis, is an exploratory research on the radiated power density and its evolution feature of a ball lightning. The radiated power density has shown a periodic pulse feature, like the spectral characteristics and temperature evolution of this BL. We proposed that this BL may be the discharge from the residual charge at the bottom of the previous cloud-to-ground (CG) lightning channel initiating it. Meanwhile, the electromagnetic field produced by the power line may be a potential outside energy source that supports the life of the BL. The optical radiation from soil constituent dominates the bright light of this BL.

opencc-by-4.0Mar 2021View details →

The global wave energy spectra data

The data were downloaded from ftp://ftp.ifremer.fr/ifremer/ww3/HINDCAST/GLOBAL/2017_ECMWF/ef, which are derived by Wavewatch model.

zenodo36/100

Data release for the "First measurement of muon neutrino charged-current interactions on hydrocarbon without pions in the final state using multiple detectors with correlated energy spectra at T2K"

### On-/Off-Axis Data Release #### (Version 1.0.1, dated 2024/08/12) This tar archive contains the data release for ‘First measurement of muon neutrino charged-current interactions on hydrocarbon without pions in the final state using multiple detectors with correlated energy spectra at T2K’. It contains the cross-section data points and supporting information in ROOT and text format, which are detailed below: + `onoffaxis_xsec_data.root` This ROOT file contains the extracted cross section and the nominal MC prediction as TH1D histograms for both the flattened 1D array of bins and in the angle binning for the analysis. The ROOT file also contains both the covariance and inverted covariance matrix for the result stored as TH2D histograms. The angle bin numbering and the corresponding bin edges are detailed at the end of the README. + `flux_analysis.root` This ROOT file contains the nominal and post-fit flux histograms for ND280 and INGRID. Two different binnings are included: a fine binned histogram (220 bins) and a coarse binned histogram (20 bins). The coarse binned histogram corresponds to the flux parameters detailed in the paper (and bin edges listed in the appendix). + `xsec_data_mc.csv` The extracted cross-section data points and the nominal MC prediction for each bin is stored as a comma-separated value (CSV) file with header row. + `cov_matrix.csv` and `inv_matrix.csv` The covariance matrix and the inverted covariance matrix are both stored as CSV files with each row stored as a single line and columns separated by commas (there is no header row). Matrix element (0,0) corresponds to the first number in the file. + `nd280_analysis_binning.csv` and `ingrid_analysis_binning.csv` The analysis bin edges are included as CSV files. The columns are labeled with a header row and denote the linear bin index and the lower and upper bin edge for the angle and momentum bins. The units are in cos(angle) for the angle bins and in MeV/c for the momentum bins. + `calc_chisq.cxx` This is an example ROOT script to calculate the chi-square between the data and the nominal MC prediction using the ROOT file in the data release. To run, open ROOT and load the script (`.L calc_chisq.cxx`) and execute the function `calc_chisq("/path/to/file.root")`. + `calc_chisq.py` This is an example Python script to calculate the chi-square between the data and the nominal MC prediction using the text/CSV files in the data release. The code requires NumPy as an external dependency, but otherwise uses built-in modules. To run, execute using a Python3 interpreter and give the file paths to the data/MC text file and the inverse covariance text file as the first and second arguments respectively -- e.g. `python3 calc_chisq.py /path/to/xsec_data_mc.csv /path/to/inv_matrix.csv` + ND280 angle bin numbering     - 0: `-1.0 < cos(#theta) < 0.20`     - 1: `0.20 < cos(#theta) < 0.60`     - 2: `0.60 < cos(#theta) < 0.70`     - 3: `0.70 < cos(#theta) < 0.80`     - 4: `0.80 < cos(#theta) < 0.85`     - 5: `0.85 < cos(#theta) < 0.90`     - 6: `0.90 < cos(#theta) < 0.94`     - 7: `0.94 < cos(#theta) < 0.98`     - 8: `0.98 < cos(#theta) < 1.00` + INGRID angle bin numbering     - 0: `0.50 < cos(#theta) < 0.82`     - 1: `0.82 < cos(#theta) < 0.94`     - 2: `0.94 < cos(#theta) < 1.00`      ### Changelog #### v1.0.1 Fix transcription error in INGRID momentum binning. The lowest momentum bin edge is at 350 MeV/c, not 300 MeV/c.

opencc-by-4.0Mar 2023View details →

zenodo32/100

Electron energy loss spectra of several organic compounds

We placed crystals of different compounds to explore the possibility of fingerprinting them through EELS. Here are representative datasets of 7 different compounds: <ul> <li>b-cyclodextrin</li> <li>hexacarboxy cyclohexane</li> <li>tannin</li> <li>TH-15 peptide</li> <li>TH-27 peptide</li> <li>two different forms of piroxicam</li> </ul> The datasets were collected at EMAT, using a monochromated FEI Titan3 TEM, within the scope of an EUSMI request. More information as well as analysis methodologies adopted for the data are detailed in the paper: Das et al. "Reliable Characterization of Organic & Pharmaceutical Compounds with High Resolution Monochromated EEL Spectroscopy", Polymers 2020, 12(7), 1434. The paper is Open Access gold and the full text is available at: <a href="https://doi.org/10.3390/polym12071434">https://doi.org/10.3390/polym12071434</a>

opencc-by-4.0Dec 2019View details →

zenodo24/100

Dataset - Learning Grain Boundary Segregation Energy Spectra in Polycrystals

Accompanying Dataset for the article "Learning Grain Boundary Segregation Energy Spectra in Polycrystals". The dataset contains 1) an example Jupyter Notebook with all necessary code to train and use the machine learning models outlined in the paper, and 2) a database of segregation spectra of 250+ binary alloys, in the form of LAMMPS text dump files of solvent polycrystals with predicted grain boundary solute segregation energies. Please refer to the README.pdf for detailed file description.

opencc-by-4.0Oct 2020View details →

zenodo20/100

Impact of Convective Parameterizations on Atmospheric Mesoscale Kinetic Energy Spectra in Global High-resolution Simulations

Open the record for dataset details and reuse information.

opencc-by-4.0Nov 2023View details →

restrictedus-pdMar 2025View details →

LP ELECTRON REFLECTOMETER 3D ENERGY SPECTRA 80SEC V1.0

Time ordered 3-D spectrum data from the Lunar Prospector Electron Reflectometer, in units of particles/cm**2/sec/steradian/eV, for dates 1998-01-16 to 1999-07-29.

MMS 4 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Electron Energy Spectra, Level 2 (L2), Survey Mode, 2.42 s Data

Energetic Particle Detector (EPD), Energetic Ion Spectrometer (EIS) Electron Energy Spectra, Level 2, Quick-Look Survey, 2.42 s Data. The EIS provides ion composition measurements (protons versus oxygen ions) and angular distributions over the energy range from approximately 45 to 500 keV.

MMS 3 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Electron Energy Spectra, Level 2 (L2), Survey Mode, 2.42 s Data

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Electron Energy Spectra, Level 2 (L2), 1.74 s Data

SPAN-E Level 2 ELectron Energy Spectra Data-------------------------------------------File Naming Format: psp_swp_spa_sf1_L2_32E_YYYYMMDD_v01.cdfThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.The larger Theta angles (deflection angles) are artificially enhanced in the "sf1" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.Parker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes--------------------------------------------------------------------------------November 19, 2019 Initial Data Release--------------------------------------Overview of Measurements------------------------The SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.The prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.Each SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.SPAN-E Level 2 Version 01 Release Notes---------------------------------------The SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of ±60° in Theta and 240° in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.The data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)General Remarks for Version 01 Data-----------------------------------Users interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.Due to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.The fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.The instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.A general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.Lastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.SPAN-E Encounter 1 Remarks--------------------------SPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an inst

MMS 1 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Electron Energy Spectra, Level 2 (L2), Survey Mode, 2.42 s Data

MAVEN SWEA Survey Rate Omni-Directional Electron Energy Spectra Data Collection

MAVEN Solar Wind Electron Analyzer (SWEA) omni-directional electron energy spectra in units of differential energy flux (eV/cm^2 sec ster eV) at the MAVEN survey telemetry rate. Description of the SWEA instrument can be found on the SWEA home page https://lasp.colorado.edu/maven/science/instrument-package/swea/ and in the SWEA instrument publication https://doi.org/10.1007/s11214-015-0232-1.

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-B Electron Energy Spectra, Level 2 (L2), 1.74 s Data

SPAN-E Level 2 ELectron Energy Spectra Data-------------------------------------------File Naming Format: psp_swp_spb_sf1_L2_32E_YYYYMMDD_v01.cdfThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.The larger Theta angles (deflection angles) are artificially enhanced in the "sf1" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.Parker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes--------------------------------------------------------------------------------November 19, 2019 Initial Data Release--------------------------------------Overview of Measurements------------------------The SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.The prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.Each SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.SPAN-E Level 2 Version 01 Release Notes---------------------------------------The SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of ±60° in Theta and 240° in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.The data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)General Remarks for Version 01 Data-----------------------------------Users interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.Due to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.The fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.The instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.A general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.Lastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.SPAN-E Encounter 1 Remarks--------------------------SPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an inst

MMS 2 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Electron Energy Spectra, Level 2 (L2), Survey Mode, 2.42 s Data