cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15468/dl.58v974
title: Occurrence Download

description: A dataset containing 2790 species occurrences available in GBIF matching the query:
{
 "and" : [
 "Geometry POLYGON((-23.47132 45.59454,42.84833 45.59454,42.84833 72.11104,-23.47132 72.11104,-23.47132 45.59454))",
 "HasCoordinate is true",
 "HasGeospatialIssue is false",
 "OccurrenceStatus is Present",
 "TaxonKey is Cyclopterus lumpus Linnaeus, 1758"
 ]
}

 The dataset includes 2790 records from 98 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0134364-220831081235567/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.tbf2bh
title: Occurrence Download

description: A dataset containing 9 species occurrences available in GBIF matching the query:
{
 "TaxonKey" : [
 "is Plectrohyla ephemera (Meik, Canseco-Márquez, Smith & Campbell, 2005)"
 ]
}

 The dataset includes 9 records from 1 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0114209-220831081235567/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.22008/fk2/ohi23z/qifcnm
title: MB_region.nc

description: MB region. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/nj63qg
title: MB_sector.nc

description: MB by sector. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/z2rd2r
title: MB_SMB_D_BMB.csv

description: MB CSV. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/bq5yti
title: MB_region.nc

description: MB region. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/hmfdga
title: MB_sector.nc

description: MB by sector. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/xc5yll
title: MB_SMB_D_BMB.csv

description: MB CSV. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/mmrqz1
title: MB_region.nc

description: MB region. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/25ynvt
title: MB_sector.nc

description: MB by sector. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/bkj9ip
title: MB_SMB_D_BMB.csv

description: MB CSV. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/mi9w8t
title: MB_region.nc

description: MB region. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/rnmfh8
title: MB_sector.nc

description: MB by sector. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/u3l9ly
title: MB_SMB_D_BMB.csv

description: MB CSV. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/ym3feg
title: MB_region.nc

description: MB region. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/mqwel7
title: MB_sector.nc

description: MB by sector. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/xvzkvk
title: MB_SMB_D_BMB.csv

description: MB CSV. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/kvlbni
title: MB_region.nc

description: MB region. Git hash: 20af941
DOI: 10.22008/fk2/ohi23z/k1me66
title: MB_sector.nc

description: MB by sector. Git hash: 20af941
DOI: 10.15468/dl.j77g5v
title: Occurrence Download

description: A dataset listing the 2376377 species recorded in GBIF matching the query:
{
 "and" : [
 "HasCoordinate is true",
 "HasGeospatialIssue is false"
 ]
}

 The dataset's 2376377 records were derived from 35539 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0111172-220831081235567/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.zhrckz
title: Occurrence Download

description: A dataset containing 134 species occurrences available in GBIF matching the query:
{
 "and" : [
 "Country is Nepal",
 "HasCoordinate is true",
 "HasGeospatialIssue is false",
 "TaxonKey is one of (Canis aureus, Canis aureus aureus)"
 ]
}

 The dataset includes 134 records from 11 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0080836-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.ptrtj2
title: Occurrence Download

description: A dataset containing 10734 species occurrences available in GBIF matching the query:
{
 "and" : [
 "Country is Egypt",
 "DatasetKey is EOD – eBird Observation Dataset",
 "HasCoordinate is true",
 "HasGeospatialIssue is false",
 "OccurrenceStatus is Present",
 "TaxonKey is Charadriidae",
 "Year 2002-2025"
 ]
}

 The dataset includes 10734 records from 1 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0080835-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.48322/yd5h-ty18
title: Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Energy-Resolved Pitch-Angle Distributions (ERPAs), Level 2 (L2), 30-minute Data in Solar Wind

description: The data include Wind STICS 30-minute Energy-Resolved Pitch-Angle Distributions (ERPAs) for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the solar wind. ERPAs organize the data by the angle relative to the magnetic field vector direction, in 7.5 degree bins. The energy separation is preserved at the native resolution of the E/q bins. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf .
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space.  The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
DOI: 10.48322/wnzt-eh29
title: Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Moments, Level 2 (L2), 3-minute Data in Magnetosphere

description: The data include Wind STICS 3-minute density (0th moment) and mean value of the energy distribution (1st moment), together with their statistical errors, for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the magnetosphere. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space.  The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
DOI: 10.48322/2mh5-qw88
title: Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Moments, Level 2 (L2), 3-minute Data in Solar Wind

description: The data include Wind STICS 3-minute density (0th moment) and mean value of the energy distribution (1st moment), together with their statistical errors, for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the solar wind. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space.  The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
DOI: 10.48322/6vrg-6n41
title: Wind Solar Wind Experiment (SWE) Faraday Cup, Solar Wind Plasma Reduced Ion Distribution Functions, 92 s Data

description: WIND Solar Wind Experiment, SWE, Faraday cup data: this data set contains three-dimensional measurements of ions in the energy range 150 eV to 8 keV. Placed 15° above and below equatorial plane of the spacecraft, the Faraday Cups measure ion charge flux as a function of epoch, cup number, orientation angle, and bias grid potential. For each time point, a full spectrum is comprised of charge flux measurements at the two Faraday cup sensors at 20 azimuth angles for each of 31 energy-per-charge windows with 1240 data points per spectrum. Spectra are built up over approximately 92 s intervals. The effective area of the Faraday cup sensor as a function of incidence angle onto the cup is also provided.
DOI: 10.48322/nasd-j276
title: Wind Solar Wind Experiment (SWE) 92-sec Definitive Solar Wind Proton Data

description: SWE is a comprehensive plasma instrument for the WIND spacecraft, see K.W.Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995. This product provides solar wind proton parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. Data reported within this product do not exceed the limits of various parameters listed in the following section. There may be more valid data in the original dataset that requires additional work to interpret but were discarded due to the limits. In particular we have tried to exclude non-solar wind data from these files. We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow angles or any other derived parameter. For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining parallel and perpendicular temperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and converting the result back to a thermal speed. The uncertainties are also propagated through.
DOI: 10.48322/wx5n-w132
title: Wind Solar Wind Experiment (SWE) Electron Pitch-Angle Distributions (6-12s rate) (VEIS-era Mode)
title: WI_H4_SWE_v01

description: Wind SWE electron pitch angle product providing electron fluxes at 30 directional bins relative to the instantaneous magnetic field direction at 16 different energy levels from the old mode (VEIS-era) of the electron instrument. The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Pitch-angle distrubutions, organized by energy, are computed from 3s measurements which are spaced either 6s or 12s in time. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 16 energy channels ranging from about 10 eV to as much as 3 keV. The exact energies at which observations are made is time-varying, and this data set reports the energy each channel observes (along with the observations themselves) at any time. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12, f_pitch_E13, f_pitch_E14, f_pitch_E15 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 16 spin-averaged energy bins). For reference, the electron speeds ( V , in cm/s) corresponding to the energy channels used, are reported in this data set.
DOI: 10.48322/xdpr-7352
title: Wind Solar Wind Experiment (SWE) Electron Pitch-Angle Distributions (12-15s rate) (New Mode)
title: WI_H3_SWE_v01

description: Wind SWE electron pitch angle product providing electron fluxes at 30 directional bins relative to the instantaneous magnetic field direction at 13 different energy levels from a later mode (post-VEIS-era) of the electron instrument. The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995). Pitch-angle distrubutions, organized by energy, are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 13 spin-averaged energy bins). For reference, the electron speeds ( V , in cm/s) corresponding to the energy channels used, are reported in this data set.
DOI: 10.48322/chaz-z942
title: Wind Solar Wind Experiment (SWE) Electron Quadrature Moments Parameters (12-15s rate) (New Mode)
title: WI_H5_SWE_v01

description: Wind SWE electron moments from a later mode (post-VEIS-era) of the electron instrument. The electron moments included in this data set are derived from quadrature integration of the solar wind electron distributions (with some fitting) measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995). Moment parameters are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the prime quantities of this data set, the electron density, bulk-velocity and temperature. We compensate for the limited nature of our observations under this instrument mode by combining electron observations with bulk-velocity estimates derived from corresponding ion observations. The (13) energy channels over which observations are made are: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV; f(E,Az,El) [#/{cc*(cm/s)^3}] being obtained for each E, using an 8x6 grid of look-directions (Azimuth x Elevation, with ~45x9 deg. "pixels")--thus constituting an 'electron distribution'. A fitted Maxwellian model supplements the "core" regime of each distribution. N_elec [#/cc] gives the density value derived for the full distribution, while NcElec [#/cc] gives that of the core. U_eGSE and UceGSE [km/s, GSE], resp. supply the full and core bulk-velocity. P_eGSE [erg/cc, GSE] has the [Pxx, Pxy, Pxz, Pyy, Pyz, Pzz] components of the derived pressure-tensor. T_elec and TcElec [K], resp. provide the full and core total-temperatures; W_elec and WcElec [eV] specifying the corresponding thermal-energies. Te_pal, Te_per, TecPal and TecPer [K] give resp. full and core parallel- and perpendicular-temperatures (wrt B), with Te_ani and TecAni [unitless] furnishing the perpendicular/parallel temperature-anisotropies for each regime. Finally, Gyrtrp [unitless] indicates the derived electron gyrotropy. The data set reported here contains: N_elec, NcElec, U_eGSE, UceGSE, P_eGSE, T_elec, TcElec, W_elec, WcElec, Te_pal, Te_per, TecPal, TecPer, Te_ani, TecAni, and Gyrtrp (as described above).
DOI: 10.48322/dq7x-fd74
title: Wind Solar Wind Experiment (SWE) Averaged Electron Pitch Angle Distribution (6-12s rate)
title: WI_M2_SWE_v01

description: Averaged Wind SWE electron pitch angle data (6-12 seconds rate) from an earlier mode (VEIS-era) of the electron instrument. The electron pitch-angle distribution averages included in this data set are derived from integrating the electron pitch-angle distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995). Averages of phase-space density (f) over key regions of the unit sphere (the set of all possible electron velocity directions) are computed from 3s measurements which are spaced either 6s or 12s in time. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the averages reported in this data set. We begin this analysis with a measure of f for each pitch-angle bin, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). The f values for pitch-angles from 0-90 degrees (parallel streaming) are integrated (with angluar weighting and assumptions of gyrotropy) over this half-sphere, then averaged by dividing out the 2-pi solid angle of the half-sphere; the result being referred to as the 'f_para' average. Similarly, the 'f_perp' (flux nearly perpendicular to B) average is the result of integrating f for pitch-angles from 60-120 degrees (a region also 2-pi in solid angle). Next, the 'f_anti' (flux nearly anti-parallel to B) average covers the half-sphere of "backward" streaming electrons; having pitch-angles from 90-180 degrees. Finally, the 'f_omni' (omni-directional) average provides the integral of f over the full sphere, divided by the full 4-pi solid angle; providing a measure of total electron flux into the region of observation. The above analysis is carried out for each of 16 energy channels ranging from about 10 eV to as much as 3 keV. The exact energies at which observations are made is time-varying, and this data set reports the electron speeds each channel observes ( V , in cm/s, along with the observations themselves) at any time. Hence the data set reported here contains: f_para, f_perp, f_anti, f_omni (for each of 16 values of V ), and the 16 values of V (time-varying, although usually much more slowly than the order of a day).