cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15468/dl.g3an3r
title: Occurrence Download

description: A dataset containing 5619 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Myzus persicae",
 "Year 1970-2025"
 ]
}

 The dataset includes 5619 records from 76 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0068901-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.ezgwet
title: Occurrence Download

description: A dataset containing 37034 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Nudibranchia",
 "Country is one of (Indonesia, Philippines)",
 "HasCoordinate is true",
 "HasGeospatialIssue is false"
 ]
}

 The dataset includes 37034 records from 42 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0068902-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.5281/zenodo.18091135
title: Wearable IMU Dataset for Human Balance and Stability Monitoring

description: This dataset corresponds to a first version of experimental stability tests, conducted using inertial measurement units (IMUs) during balance exercises performed on unstable BOSU platforms.The measurements were collected from four (4) subjects, who performed static and/or dynamic stability tasks aimed at characterizing balance behavior under controlled instability conditions. The IMU sensors recorded multiaxial inertial signals, including accelerations and angular velocities, enabling the analysis of stability metrics, postural control, and movement variability.This dataset is released as a preliminary version (v1), intended for the validation of experimental protocols, exploratory data analysis, and the initial development of processing, modeling, or machine learning methodologies based on inertial data. The data are provided as open-access to support reuse in stability studies, biomechanics, motion control, and related applications.
DOI: 10.5281/zenodo.18091134
title: Wearable IMU Dataset for Human Balance and Stability Monitoring

description: This dataset corresponds to a first version of experimental stability tests, conducted using inertial measurement units (IMUs) during balance exercises performed on unstable BOSU platforms.The measurements were collected from four (4) subjects, who performed static and/or dynamic stability tasks aimed at characterizing balance behavior under controlled instability conditions. The IMU sensors recorded multiaxial inertial signals, including accelerations and angular velocities, enabling the analysis of stability metrics, postural control, and movement variability.This dataset is released as a preliminary version (v1), intended for the validation of experimental protocols, exploratory data analysis, and the initial development of processing, modeling, or machine learning methodologies based on inertial data. The data are provided as open-access to support reuse in stability studies, biomechanics, motion control, and related applications.
DOI: 10.48322/35v3-c331
title: RENU2 COrnell Wire BOom Yo-yo (COWBOY) Electric Field, High Time Resolution (H0), 1 ms Data

description: Rocket Experiment for Neutral Upwelling 2, RENU2, COrnell Wire BOom Yo-yo, COWBOY, Electric Field Measurements
DOI: 10.48322/7pss-6w70
title: RENU2 COrnell Wire BOom Yo-yo (COWBOY) Electric Field Very Low Frequency Waves, High Time Resolution (H0), 1 ms Data

description: Rocket Experiment for Neutral Upwelling 2, RENU2, COrnell Wire BOom Yo-yo, COWBOY, Very Low Frequency, VLF, Electric Field Measurements
DOI: 10.48322/5zvf-1q82
title: RENU2 Electron Plasma Detector (EPLAS) Precipitating Electron Total Energy Flux, (H0), 42 ms Data

description: RENU2 Electron Plasma Detector (EPLAS) Precipitating Electron Total Energy Flux
DOI: 10.48322/7hy6-k889
title: RENU2 Electron Retarding Potential Analyzer (ERPA) Thermal Electron Temperature (Main), (H0), 0.5 ms Data

description: RENU2 Electron Retarding Potential Analyzer (ERPA) Thermal Electron Temperature (Main)
DOI: 10.48322/cy19-2944
title: RENU2 Electron Retarding Potential Analyzer (ERPA) Thermal Electron Temperature (Sub), (H0), 0.5 ms Data

description: RENU2 Electron Retarding Potential Analyzer (ERPA) Thermal Electron Temperature (Sub)
DOI: 10.48322/ndrv-ds51
title: RENU2 Science Magnetometer (FGM) Magnetic Field, High Time Resolution (H0), 1 ms Data

description: Rocket Experiment for Neutral Upwelling 2, RENU2, Science Magnetometer, Magnetic Field Measurements
DOI: 10.48322/k3hd-7y51
title: RENU2 Ion Gauge (IG2) Sensor Pressure, High Time Resolution (H0), 1 ms Data

description: Rocket Experiment for Neutral Upwelling 2, RENU2, Ionization Gauge, Neutral Gas Pressure Measurements
DOI: 10.48322/f1c4-b375
title: RENU2 UltraViolet PhotoMultiplier Tube (UVPMT) Atomic Oxygen Density, High Time Resolution (H0), 42 ms Data

description: Rocket Experiment for Neutral Upwelling 2, RENU2, UltraViolet PhotoMultiplier Tube, UVPMT, Counts. The UVPMT Instrument is used to observe Atomic Oxygen Signatures in Sunlight, that is, above the Payload.
DOI: 10.48322/hwz5-q486
title: RENU2 PhotoMultiplier Tube (PMT) Auroral Red and Green Line Luminosity in Raylieghs, Background subtracted, High Time Resolution (H0), 4 ms Data

description: RENU2 PMT Counts converted to Rayleighs and Background subtracted
DOI: 10.48322/m7w8-8d83
title: SAMPEX Polar-Cap-Averaged Fluxes, all instruments

description: This data set contains 17 differential fluxes of protons (mainly), helium ions, Z.GE.6 ions, and electrons, plus one integral flux of protons and electrons, as averaged over polar cap passes of the SAMPEX spacecraft. A polar cap pass covers the time poleward of geomagnetic latitude 70 deg. (Not all orbits have two polar cap passes.). For any given species, the fluxes typically come from more than one of the sensors (LICA, HILT, MAST, PET). Hence the inclusion of all instruments' data in each single record. Differential fluxes are those for (mainly) protons (Z.GE.1 channels at 5-12 and 19-27 MeV/n), helium ions (0.50-6.6, 4-9, 8-15, 9-38 MeV/n), Z.GE.6 ions (0.49-8.3, 8-42, 19.3-22.8, 22.8-31.0, 31.0-51.7, 41-220, 51.7-76.2, 76.2-113, 113-156 MeV/n), and electrons (1.5-6.0 MeV from PET only). One LICA channel measured integral fluxes of ions .GT. 0.8 MeV/n plus electrons .GT. 0.6 MeV). Data available for each polar cap pass are time tags of the begin and end points of the averaging interval, the fluxes, statistical uncertainties in the fluxes, instrument-specific flags, and a flag indicating a north or south polar cap pass. Data are organized in two different ways. Monthly ~500-KB ASCII files with records organized by instrument are available from the SAMPEX Data Center at Caltech and from nssdcftp at GSFC/SPDF, while monthly ~260 KB CDF-formatted files with records organized by species are available from the ftp area underlying CDAWeb. The parameter level information given below in this descriptor corresponds to the CDAWeb organization of data. Format information for the ASCII version is given in the Information URL of this descriptor.
DOI: 10.48322/2x9v-jv02
title: SAMPEX Fluxes, all instruments

description: This set of 30-s averaged fluxes are derived from measurements made by all 4 instruments (HILT, LICA, MAST and PET) onboard the Solar Anomalous and Magnetospheric Particle Explorer (SAMPEX). Each file covers one full day of 30-s averaged fluxes of cosmic rays from selected channels from all experiments. There are 156 variables per record, and the file size is about 4 MB. After an extensive list of ancillary data, the particle fluxes follow. (1) LICA provides fluxes of electrons and protons in the energy range of about >0.7 Mev, of (mainly) helium in the range 0.49-8.3 MeV/nucleon. (2) HILT provides fluxes of helium from two channels, 4-9 and 9-38, of Z > 5 from two channels, 8.2-42 and 41-220 MeV/n. (3) MAST provides fluxes protons (mainly) in 5-12 MeV range, of helium in 8-15, and of Z > 5 in 19.3-22.8, 22.8-31.0, 31.0-51.7, 51.7-76.2, 76.2-113, 113-156 MeV/n. (4) PET provides fluxes of electrons in the ranges 1.5-6, and 2.5-14 MeV, and of (mainly) protons in 19-27 MeV/n. All flux values are accompanied by their standard deviations and quality flags. The fluxes available in this file are from a subset of (30-s resolution) rate channels. Energy spectra are assembled by pick-and-choose across instrument boundaries; an example is the eight-element array of Z>3 fluxes that have contributions from all four instruments
DOI: 10.48322/nb4b-f027
title: SOHO Charge, Element, and Isotope Analysis System (CELIAS) Proton Monitor (PM) 30-second Solar Wind Data in CDF Format

description: The data include 30-second proton speed, density, most probable thermal speed, and arrival direction, as well as predicted alpha-particle speed. Also included are the SOHO spacecraft predicted positon in GSE coordinates, Heliocentric Range, Heliographic Latitude and Longitude, and Earth Carrington Rotation Number. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. Description of the CELIAS-PM instrument and scientific scope can be found on the CELIAS instrument home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO mission home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.
DOI: 10.48322/a1m9-qh25
title: SOHO Charge, Element, and Isotope Analysis System (CELIAS) Proton Monitor (PM) 5-minute Solar Wind Data in CDF Format

description: The data include 5-minute proton speed, density, most probable thermal speed, and arrival direction, as well as predicted alpha-particle speed. Also included are the SOHO spacecraft predicted positon in GSE coordinates, Heliocentric Range, Heliographic Latitude and Longitude, and Earth Carrington Rotation Number. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. Description of the CELIAS-PM instrument and scientific scope can be found on the CELIAS instrument home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO mission home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.
DOI: 10.48322/d93q-e053
title: SOHO Charge, Element, and Isotope Analysis System (CELIAS) Solar Extreme-Ultra-Violet Monitor (SEM) Daily Data in CDF Format

description: The data include daily average raw count rates in Channels 1 - 3 and First Order (26 - 34 nm, average of Ch1 and Ch3) and Central Order (0.1 - 50 nm, Ch2) photon fluxes, as well as SOHO Heliocentric location and distance. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. The original ASCII dataset Version 4 Science Product Release Notes are available at https://lasp.colorado.edu/eve/data_access/eve_data/lasp_soho_sem_data/long/LASP_SOHO_SEM_release_notes_v4.pdf. Description of the CELIAS-SEM instrument and scientific scope can befound on the CELIAS home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO mission home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.
DOI: 10.48322/perq-dq14
title: SOHO Charge, Element, and Isotope Analysis System (CELIAS) Solar Extreme-Ultra-Violet Monitor (SEM) 15-second Data in CDF Format

description: The data include 15-second average raw count rates in Channels 1 - 3 and First Order (26 - 34 nm, average of Ch1 and Ch3) and Central Order (0.1 - 50 nm, Ch2) photon fluxes, as well as SOHO Heliocentric location and distance. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. The original ASCII dataset Version 4 science product release notes are available at https://lasp.colorado.edu/eve/data_access/eve_data/lasp_soho_sem_data/long/LASP_SOHO_SEM_release_notes_v4.pdf. Description of the CELIAS-SEM instrument and scientific scope can be found on the CELIAS home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.
DOI: 10.48322/a8q8-am07
title: SOHO LASCO C1 Level 0.5 FITS Data

description: The LASCO C1 Raw FITS Data. 

LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).
DOI: 10.48322/h5kj-3939
title: SOHO LASCO C2 Level 1.0 FITS Data

description: The LASCO C2 Calibrated FITS Data. 

LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).
DOI: 10.48322/r515-1367
title: SOHO LASCO C2 Percent Polarized FITS Data

description: The Percent Polarized data from the LASCO C2 coronagraph

LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).
DOI: 10.48322/6q0p-cj91
title: SOHO LASCO C3 Level 0.5 FITS Data

description: The LASCO C3 Raw FITS Data. 

LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).