cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.48322/0ydx-j139
title: FAST Electrostatic Analyzer (ESA), Electron Survey 0.625 s Data

description: The FAST IES and EES measure 32 pitch angle directions simultaneously, 11.25° resolution, and sweep over 48 energy steps in 1/64 of a spacecraft spin. The energy range is nominally 3 eV to 25 keV for ions and 4 eV to 30 keV for electrons, respectively. Each spectrometer consists of two half sensor heads each with 180° by 10° field-of-view, FOV, that are mounted on opposite sides of the spacecraft to form a 360° planar FOV. The out-of-plane response is roughly Gaussian with a full width, half maximum, FWHM, of about 5°. The planar FOV is within the spacecraft spin plane, which is oriented with the spin vector normal to the nominal magnetic field direction. This orientation facilitates continuous pitch angle measurements. Deflectors are used to steer the sensor FOV out of this plane by up to 10° to account for variations of the magnetic field direction during the orbit. In general, the pitch angle distribution always includes both the parallel and Anti-parallel magnetic field directions. Burst data consists of a 32 angle by 48 anergy bin array of counts. Counts are pseudo-log compressed from 16 to 8 bits onboard. The first energy step is a high voltage retrace and should be ignored. Detector anodes rotate by half an anode or 5.625° each sweep. Survey data is averaged burst data that has been despun onboard. Slow survey is averaged into a 32 angle by 48 energy array each half spin or about 2.5 s. Some blurring of the angular resolution results from the half anode rotation on alternate sweeps. Fast survey is averaged into a 64 angle by 48 energy array that maintains the angular resolution. Fast survey time resolution varies from 1/16 to 1/4 of a spin.
DOI: 10.48322/3chd-sj41
title: FAST Electrostatic Analyzer (ESA), Ion Burst 0.078 s Data

description: The FAST IES and EES measure 32 pitch angle directions simultaneously, 11.25° resolution, and sweep over 48 energy steps in 1/64 of a spacecraft spin. The energy range is nominally 3 eV to 25 keV for ions and 4 eV to 30 keV for electrons, respectively. Each spectrometer consists of two half sensor heads each with 180° by 10° field-of-view, FOV, that are mounted on opposite sides of the spacecraft to form a 360° planar FOV. The out-of-plane response is roughly Gaussian with a full width, half maximum, FWHM, of about 5°. The planar FOV is within the spacecraft spin plane, which is oriented with the spin vector normal to the nominal magnetic field direction. This orientation facilitates continuous pitch angle measurements. Deflectors are used to steer the sensor FOV out of this plane by up to 10° to account for variations of the magnetic field direction during the orbit. In general, the pitch angle distribution always includes both the parallel and Anti-parallel magnetic field directions. Burst data consists of a 32 angle by 48 anergy bin array of counts. Counts are pseudo-log compressed from 16 to 8 bits onboard. The first energy step is a high voltage retrace and should be ignored. Detector anodes rotate by half an anode or 5.625° each sweep. Survey data is averaged burst data that has been despun onboard. Slow survey is averaged into a 32 angle by 48 energy array each half spin or about 2.5 s. Some blurring of the angular resolution results from the half anode rotation on alternate sweeps. Fast survey is averaged into a 64 angle by 48 energy array that maintains the angular resolution. Fast survey time resolution varies from 1/16 to 1/4 of a spin.
DOI: 10.48322/9t9w-1q28
title: FAST Electrostatic Analyzer (ESA), Ion Survey 0.625 s Data

description: The FAST IES and EES measure 32 pitch angle directions simultaneously, 11.25° resolution, and sweep over 48 energy steps in 1/64 of a spacecraft spin. The energy range is nominally 3 eV to 25 keV for ions and 4 eV to 30 keV for electrons, respectively. Each spectrometer consists of two half sensor heads each with 180° by 10° field-of-view, FOV, that are mounted on opposite sides of the spacecraft to form a 360° planar FOV. The out-of-plane response is roughly Gaussian with a full width, half maximum, FWHM, of about 5°. The planar FOV is within the spacecraft spin plane, which is oriented with the spin vector normal to the nominal magnetic field direction. This orientation facilitates continuous pitch angle measurements. Deflectors are used to steer the sensor FOV out of this plane by up to 10° to account for variations of the magnetic field direction during the orbit. In general, the pitch angle distribution always includes both the parallel and Anti-parallel magnetic field directions. Burst data consists of a 32 angle by 48 anergy bin array of counts. Counts are pseudo-log compressed from 16 to 8 bits onboard. The first energy step is a high voltage retrace and should be ignored. Detector anodes rotate by half an anode or 5.625° each sweep. Survey data is averaged burst data that has been despun onboard. Slow survey is averaged into a 32 angle by 48 energy array each half spin or about 2.5 s. Some blurring of the angular resolution results from the half anode rotation on alternate sweeps. Fast survey is averaged into a 64 angle by 48 energy array that maintains the angular resolution. Fast survey time resolution varies from 1/16 to 1/4 of a spin.
DOI: 10.48322/78b7-gk94
title: FAST Time-of-Flight Energy, Angle, Mass Spectrograph (TEAMS) Experiment Survey, Key Parameter (K0), PT5S Data

description: Data are derived from the FAST Time-of-flight Energy Angle Mass Spectrograph, TEAMS, Instrument that determines 3-Dimensional Distribution Functions of individual Ion Species over the Energy Range 1 eV to 12000 eV, within 2.5 s (one-half Spacecraft Spin). The Instrument consists of a toroidal Top-Hat Electrostatic Analyzer with instantaneous Acceptance of Ions over 360° in Polar Angle in 16 Sectors. Ions passing through the Electrostatic Analyzer are postaccelerated by up to 25 kV and then analyzed for Mass per Charge in a foil-based Time-of-Flight Analyzer. The Data used to construct CDF Data Products are derived from the Survey Data. Survey Data consists of four Mass Groups by 48 Energies by 64 Solid Angle Segments. The four Mass Groups are Hydrogen, H+, Oxygen, O+, singly-charged Helium, He+, and doubly-charged Helium, He++. Only the 16 Equatorial Angle Segments are used for the CDF Data Set. Each Equatorial Solid Angle Segment contains two (four) Samples at each Energy in the 32 (64) Sweep/Spin Mode. The full Angular Range is covered in Half of a Spin but the actual Time Resolution of the Survey Data Product depends upon the Telemetry Mode. In the highest Telemetry Mode Rate, Modes H+ and O+ Survey Data are read out every Half Spin. In the lowest Telemetry Mode Rate Mode, these Data are accumulated for four Spins. The minimum Accumulation Time included in the CDF is one Spin, so if the actual Accumulation Time is a Half Spin, two Data Points are averaged. Otherwise, the Full Resolution is included. In every Mode, He+ and He++ are accumulated twice as long as H+ and O+. To force the H+, O+, and He+ to have an equal Number of Data Points when H+ and O+ have twice the Time Resolution, each He+ Data Point is written twice consecutively in the File. The 3-D Plasma Distribution Function Analyzers with Time-of-Flight Mass Discrimination for CLUSTER, FAST,and Equator-S, E. Moebius, L.M. Kistler, M. Popecki, K. Crocker, M. Granoff, Y. Jiang, E. Satori, V. Ye, H. Reme, J.A. Sauvaud, A. Cros, A. Aoustin, T. Camus, J.L. Medale, J. Rouzaud, C.W. Carlson, J. McFadden, D. Curtis, H. Heetdirks, J. Croyle, C. Ingraham, E.G. Shelley, D.M. Klumpar, E. Hertzberg, B. Klecker, M. Ertl, F. Eberl, H. Kaestle, E. Kuenneth, P. Laeverenz, E. Seidenschwang, G. Parks, M. McCarthy, A. Korth, B. Graeve, H. Balsiger, U. Schwab, and M. Steinacher, Measurement Techniques for Space Plasmas: Particles, Geophys. Mono. Ser., 102, 243-248, 1998. The Time-of-Flight Energy, Angle, Mass Spectrograph (TEAMS) Experiment for FAST, D.M. Klumpar, E. Moebius, L.M. Kistler, M. Popecki, E.G. Shelley, E. Hertzberg, K. Crocker, M. Granoff, Li Tang, C.W. Carlson, J. McFadden, B. Klecker, F. Eberl, E. Kuenneth, H. Kaestle, M. Ertl, W.K. Peterson, and D. Hovestadt, Space Sci. Rev., 2001, 98, pages 197-291, doi:10.1023/A:1013127607414.
DOI: 10.48322/86pq-hb06
title: FAST Fluxgate Magnetometer High-Resolution 7.8125 ms Data

description: Calibrated Fluxgate Data acquired by the Fast Auroral SnapshoT Small Explorer, FAST, Magnetometer Instrument. Data have been calibrated, despun, and detrended against the International Geomagnetic Reference Field, IGRF, using IGRF Coefficients for the Date of Acquisition. Data are provided in several Coordinate Systems. Non detrended Data in Spacecraft and Geocentric Equatorial Inertial Coordinates are provided. Ephemeris Data are also provided.
DOI: 10.5281/zenodo.18019754
title: Dataset: Teachers' and Their Pupils' Performance on Plant Nutrition (graphic task)

description: Dataset:

García-Fernández, B., Sobrino-Costoso, C. E., & Ruiz-Gallardo, J. R. (2022). Teachers’ and their pupils’ performance on plant nutrition: A comparative case. Research in Science Education, 52(4), 1109-1129. https://doi.org/10.1007/s11165-020-09987-x
DOI: 10.5281/zenodo.18019755
title: Dataset: Teachers' and Their Pupils' Performance on Plant Nutrition (graphic task)

description: Dataset:

García-Fernández, B., Sobrino-Costoso, C. E., & Ruiz-Gallardo, J. R. (2022). Teachers’ and their pupils’ performance on plant nutrition: A comparative case. Research in Science Education, 52(4), 1109-1129. https://doi.org/10.1007/s11165-020-09987-x
DOI: 10.48322/wdvm-s118
title: Genesis 3D Ion Moments

description: Genesis level 2 3-dimensional ion moments and a bidirectional electron streaming flag
DOI: 10.48322/etz7-wx98
title: Hawkeye Electric and Magnetic Field Radio Frequency Spectrum Analyzer High Time Resolution
title: Hawkeye 1 VLF instrument CDFs at NASA's CDAWeb

description: The CDF file contains approximately 22 second time resolution Electric and Magnetic field data, average magnetic field magnitude, and orbital position data from Hawkeye 1. The VLF experiment measured electric and magnetic fields using a 42.45-m electric dipole (tip-to-tip) which extended perpendicular to the spin axis and a search coil antenna deployed 1.58 m from the spacecraft. The electric field spectrum measurements were made in 16 logarithmically spaced frequency channels extending from 1.78 Hz to 178 kHz, and dc electric fields were also measured. The bandwidth of these channels varied from 7.5% to 30% depending on center frequency. Channel sensitivity and dynamic range were 1E-6 V/m and 100 dB, respectively. A wideband receiver was also used, with two selectable bandwidth ranges: 0.15 to 10 kHz or 1 to 45 kHz. The magnetic field spectrum was measured in eight discrete, logarithmically spaced channels from 1.78 Hz to 5.62 kHz. The bandwidth of these channels varied from 7.5% to 30% depending on frequency. The dynamic range was 100 dB, and the sensitivity ranged from 0.1 nT at 1.78 Hz to 3.4E-4 nT at 5.62 kHz. The wideband receiver described above could be used with the magnetic antenna. Each discrete channel was sampled once every 11.52 s.
DOI: 10.48322/nzxp-3e54
title: Helios 1 E3 Magnetometer (Ness et al.) 6-sec Data

description: Task of the HELIOS mission was the exploration of the inner heliosphere, inside the Earth's orbit to 0.3 AU. The Rome-GSFC magnetic field experiment has been a joint venture of an italian group (University of Rome and CNR/Istituto Fisica Spazio Interplanetario, Frascati) and an american group of NASA/Goddard Space Fligth Center, under the responsibility of F. Mariani and N.F.Ness, respectively. A description of the experiment can be found in the NASA-GSFC report X-692-75-112 (1975), by C. Scearce et al. The instrument is a dual configuration of two tri-axial fluxgate magnetometers operating at four different sensitivities (from 0.84 to 0.03 nT). The time resolution, depending the operation mode, telemetry format, and bit rate, for most cases varied from 0.07 to 1.5 seconds. The present data set contains six-second averages of the magnetic field elements in solar-ecliptic (SE) spacecraft-centered coordinates. Data are stored in files on a daily basis. File names are hNYYDDD.asc, with N the Helios number (1 or 2), YY the year (last two digits), and DDD the day of year (1 = January 1st). For instance, h276105.asc is the file with Helios 2 data for day 105, 1976.
DOI: 10.48322/zxcr-jp63
title: Helios 2 E3 Magnetometer (Ness et al.) 6-sec Data

description: Task of the HELIOS mission was the exploration of the inner heliosphere, inside the Earth's orbit to 0.3 AU. The Rome-GSFC magnetic field experiment has been a joint venture of an italian group (University of Rome and CNR/Istituto Fisica Spazio Interplanetario, Frascati) and an american group of NASA/Goddard Space Fligth Center, under the responsibility of F. Mariani and N.F.Ness, respectively. A description of the experiment can be found in the NASA-GSFC report X-692-75-112 (1975), by C. Scearce et al. The instrument is a dual configuration of two tri-axial fluxgate magnetometers operating at four different sensitivities (from 0.84 to 0.03 nT). The time resolution, depending the operation mode, telemetry format, and bit rate, for most cases varied from 0.07 to 1.5 seconds. The present data set contains six-second averages of the magnetic field elements in solar-ecliptic (SE) spacecraft-centered coordinates. Data are stored in files on a daily basis. File names are hNYYDDD.asc, with N the Helios number (1 or 2), YY the year (last two digits), and DDD the day of year (1 = January 1st). For instance, h276105.asc is the file with Helios 2 data for day 105, 1976.
DOI: 10.48322/0vjh-ph32
title: IBEX High Energy Neutral Atom Imager (Hi) Data Release 02, not Compton-Getting corrected, not Survival Probability corrected, Omnidirectional, West Longitude Ecliptic Maps, Level H3 (H3), semiannually averaged Data

description: * 1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 17 releases of IBEX-HI and/or IBEX-LO data covering 2009-2020.
* 2: This data set is from the Release 2 (6 months-cadence) IBEX-Hi map data for the year 2009 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) between 1 and 100 AU.
* 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:
* 4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.),
* 5: http://doi.org/10.3847/1538-4365/aa66d8
* 6. The following codes are used to define dataset types:
- cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs.
- nocg = no Compton-Getting corrections
- sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular.
- noSP - no survival probability corrections have been applied to the data.
- omni = data from all directions.
- ram = data was collected when the spacecraft was ramming into the incoming ENAs.
- antiram = data was collected when the spacecraft was moving away from the incoming ENAs.
* 7. The following list associates Release 2 map numbers (1-2) with mission year 1
- Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009
- Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009
* 8: This particular data set, denoted in the original ascii files as mapN for N=1-2, which indicates a map number, includes pixel map data from all directions (omnidirectional), no CG, no SP, 6 month cadence.
DOI: 10.48322/rcw2-kh18
title: IBEX High Energy Neutral Atom Imager (Hi) Data Release 02, Compton-Getting corrected, not Survival Probability corrected, Omnidirectional, West Longitude Ecliptic Maps, Level H3 (H3), semiannually averaged Data

description: * 1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 17 releases of IBEX-HI and/or IBEX-LO data covering 2009-2020.
* 2: This data set is from the Release 2 (6 months-cadence) IBEX-Hi map data for the year 2009 in the form of omnidirectional ENA (hydrogen) fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) between 1 and 100 AU.
* 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:
* 4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.),
* 5: http://doi.org/10.3847/1538-4365/aa66d8
* 6. The following codes are used to define dataset types:
- cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs.
- nocg = no Compton-Getting corrections
- sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular.
- noSP - no survival probability corrections have been applied to the data.
- omni = data from all directions.
- ram = data was collected when the spacecraft was ramming into the incoming ENAs.
- antiram = data was collected when the spacecraft was moving away from the incoming ENAs.
* 7. The following list associates Release 2 map numbers (1-2) with mission year 1
- Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009
- Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009
* 8: This particular data set, denoted in the original ascii files as mapN for N=1-2, which indicates a map number, includes pixel map data from all directions (omnidirectional), CG, no SP, 6 month cadence.
DOI: 10.48322/qmwe-ve75
title: IBEX High Energy Neutral Atom Imager (Hi) Data Release 04, not Compton-Getting corrected, not Survival Probability corrected, Omnidirectional, West Longitude Ecliptic Maps, Level H3 (H3), three year average Data

description: * 1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008 updating our knowledge of the outer heliosphere and its interaction with the local interstellar medium. Start-time: 2008-12-25. There are currently 14 releases of IBEX-HI and/or IBEX-LO data covering 2009-2011.
* 2: This data set is from the Release 4 (3 year-cadence) IBEX-Hi map data for the years 2009-2011 in the form of omnidirectional ENA (hydrogen) fluxes with no Compton-Getting correction (nocg) of flux spectra for spacecraft motion and no correction for ENA survival probability (nosp) between 1 and 100 AU.
* 3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west) and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95, 0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the data and enabled science from Release 10 are given in the following journal publication:
* 4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.),
* 5: http://doi.org/10.3847/1538-4365/aa66d8
* 6. The following codes are used to define dataset types:
- cg = Compton-Getting corrections have been applied to the data to account for the speed of the spacecraft relative to the direction of arrival of the ENAs.
- nocg = no Compton-Getting corrections
- sp = survival probability corrections have been applied to the data to account for the loss of ENAs due to radiation pressure, photoionization and ionization via charge exchange with solar wind protons as they stream through the heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU. In the original data this mode is denoted as Tabular.
- noSP - no survival probability corrections have been applied to the data.
- omni = data from all directions.
- ram = data was collected when the spacecraft was ramming into the incoming ENAs.
- antiram = data was collected when the spacecraft was moving away from the incoming ENAs.
* 7. The following list associates Release 4 map numbers (1-6) with mission year (1-3) each year is associated with two consecutive maps:
- Map 1: Map2009A, year 1, orbits 11-34, dates 12/25/2008-06/25/2009
- Map 2: Map2009B, year 1, orbits 35-58, dates 06/25/2009-12/25/2009
- Map 3: Map2010A, year 2, orbits 59-82, dates 12/25/2009-06/26/2010
- Map 4: Map2010B, year 2, orbits 83-106, dates 06/26/2010-12/26/2010
- Map 5: Map2011A, year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
- Map 6: Map2011B, year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
* 8: This particular data set, denoted in the original ascii files as comb-year123, includes pixel map data from all directions (omnidirectional), noCG, noSP, 3 year cadence.
DOI: 10.6084/m9.figshare.30858263
title: <b>A long-term, high-density, minute-resolution rainfall dataset from the Da-Tun Mountain region</b>

description: This dataset contains high-resolution precipitation observations from the Da-Tun rain gauge network (DTRGN), located in the mountainous region of northern Taiwan. The network consists of 25 automatic rain gauges that provide continuous 1-minute rainfall measurements from June 2009 to December 2023. The dataset also includes derived 10-minute, hourly, daily, and monthly precipitation products generated through a rate-based aggregation method and a multi-stage quality-control procedure.The DTRGN dataset is designed to support research on mountain meteorology, precipitation enhancement, hydrological applications, and orographic processes under typhoon and monsoonal environments. All missing values are clearly flagged, and station metadata and data availability records are included. The dataset accompanies the Scientific Data manuscript “A long-term, high-density, minute-resolution rainfall dataset from the Da-Tun Mountain region.”