cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15468/dl.6wfjpd
title: Occurrence Download

description: A dataset containing 165 species occurrences available in GBIF matching the query:
{
 "TaxonKey" : [
 "is Desmopuntius johorensis"
 ]
}

 The dataset includes 165 records from 28 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0063208-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.7hqd3z
title: Occurrence Download

description: A dataset containing 23771 species occurrences available in GBIF matching the query:
{
 "and" : [
 "HasCoordinate is true",
 "HasGeospatialIssue is false",
 "TaxonKey is Eretmochelys imbricata",
 "Year 1901-2025"
 ]
}

 The dataset includes 23771 records from 178 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0063209-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.25574/27308
title: Chandra X-ray Observatory ObsId 27308

description: Calibration Observations of ACIS-S2 and S3 with Cas A at a Non-Standard Focal Plane Temperature of -105C
DOI: 10.15482/usda.adc/30896291
title: Data from: Sensitivity of soil nutrient pools, but stability of microbial processes, under reduced rainfall and altered grazing management in northern mixed-grass prairie

description: Nutrient cycling is a key ecosystem service provided by soils, which may be impacted by global change-induced droughts and alterations to grazing pressure. While the belowground abiotic and biotic responses to drought are increasingly studied, linkages among plant, animal, and microbial responses to drought remain poorly understood. Here we used an innovative experimental approach to enable understanding the relative importance of rainfall reduction, bovine grazing, and their interplay on soil nutrient pools and processes during and after treatments. Specifically, we experimentally imposed a two-year drought of varying intensity (five levels) at two northern mixed-grass prairie sites in Montana and Wyoming. Crossed with this drought treatment, we also imposed a gradient of bovine grazing pressure during the two drought years and three years of recovery following the drought. We found that rainfall reductions at both sites resulted in reductions in soil available P and micronutrients during treatment application. Conversely, rainfall reductions caused both immediate and persistent increases in soil NO<sub>3</sub><sup>-</sup>. Soil nutrients were generally unaffected by grazing treatments. In contrast, biotic soil properties including the activities of six extracellular enzymes and bacterial and fungal community compositions were relatively resistant to rainfall reduction treatments. However, grazing treatments appeared to have a greater effect on extracellular enzyme activity potentials and soil microbial community composition. Overall, our results highlight the relative stability of belowground processes in semi-arid rangelands in the face of drought and land management strategies.The article utilizing this dataset is at https://doi.org/10.1016/j.soilbio.2025.110071.
DOI: 10.15482/usda.adc/30896291.v1
title: Data from: Sensitivity of soil nutrient pools, but stability of microbial processes, under reduced rainfall and altered grazing management in northern mixed-grass prairie

description: Nutrient cycling is a key ecosystem service provided by soils, which may be impacted by global change-induced droughts and alterations to grazing pressure. While the belowground abiotic and biotic responses to drought are increasingly studied, linkages among plant, animal, and microbial responses to drought remain poorly understood. Here we used an innovative experimental approach to enable understanding the relative importance of rainfall reduction, bovine grazing, and their interplay on soil nutrient pools and processes during and after treatments. Specifically, we experimentally imposed a two-year drought of varying intensity (five levels) at two northern mixed-grass prairie sites in Montana and Wyoming. Crossed with this drought treatment, we also imposed a gradient of bovine grazing pressure during the two drought years and three years of recovery following the drought. We found that rainfall reductions at both sites resulted in reductions in soil available P and micronutrients during treatment application. Conversely, rainfall reductions caused both immediate and persistent increases in soil NO<sub>3</sub><sup>-</sup>. Soil nutrients were generally unaffected by grazing treatments. In contrast, biotic soil properties including the activities of six extracellular enzymes and bacterial and fungal community compositions were relatively resistant to rainfall reduction treatments. However, grazing treatments appeared to have a greater effect on extracellular enzyme activity potentials and soil microbial community composition. Overall, our results highlight the relative stability of belowground processes in semi-arid rangelands in the face of drought and land management strategies.The article utilizing this dataset is at https://doi.org/10.1016/j.soilbio.2025.110071.
DOI: 10.15468/dl.jbes86
title: Occurrence Download

description: A dataset containing 4711 species occurrences available in GBIF matching the query:
{
 "TaxonKey" : [
 "is Pyrrhura calliptera"
 ]
}

 The dataset includes 4711 records from 53 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0063210-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.kcks6r
title: Occurrence Download

description: A dataset containing 10145 species occurrences available in GBIF matching the query:
{
 "and" : [
 "BasisOfRecord is one of (Observation, Machine Observation, Human Observation, Occurrence evidence)",
 "Country is United States of America",
 "OccurrenceStatus is Present",
 "TaxonKey is Simuliidae"
 ]
}

 The dataset includes 10145 records from 5 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0063211-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.48322/7x96-1j49
title: Cassini Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

description: Heliocentric trajectories for Cassini in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinates The original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth. The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch", which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage: +---------------------------------------------------------------------+   Method Name   FPA Longitude Definition    ---------------------------------------------------------------------    B1950.0   the actual FPA at 22:09 UT on December 31, 1949     J2000.0   the smoothed FPA at 12:00 UT on January 1, 2000     True of Date   the actual FPA at 00:00 UT on the date of interest     Mean of Date   the smoothed FPA at 00:00 UT on the date of interest   +---------------------------------------------------------------------+ The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method. More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.
DOI: 10.48322/cyec-7n35
title: BepiColombo Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

description: Heliocentric trajectories for Comet Borrelly in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinates The original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth. The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch", which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage: +---------------------------------------------------------------------+   Method Name   FPA Longitude Definition    ---------------------------------------------------------------------    B1950.0   the actual FPA at 22:09 UT on December 31, 1949     J2000.0   the smoothed FPA at 12:00 UT on January 1, 2000     True of Date   the actual FPA at 00:00 UT on the date of interest     Mean of Date   the smoothed FPA at 00:00 UT on the date of interest   +---------------------------------------------------------------------+ The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method. More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.
DOI: 10.48322/nh8r-qw87
title: Cluster Summary Parameter Electron Drift Instrument (EDI) Data
title: Cluster Summary Parameter EDI data

description: This instrument (EDI: Electron Drift Instrument) measures the drift of a weak beam of test electrons that, when emitted in certain directions, return to the spacecraft after one gyration. This drift is related to the electric field and the gradient in the magnetic field, and these quantities can, by the use of different electron energies, be determined separately. The fundamental time step to determine the new parameters and direct the beams and the detectors is 2 ms. Inter-experiment links include: magnetic field information from FGM and STAFF, a blanking pulse received from WHISPER to warn of possible interference from that active experiment, and a similar blanking pulse sent to PEACE when the EDI electron beam could interfere with the PEACE electron measurement. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Electron Drift Instrument for Cluster, by G. Paschmann et al., from which this information was obtained.
DOI: 10.48322/nnve-y327
title: Cassini Radio and Plasma Wave Science (RPWS) Low Rate Full Resolution
title: RPWS_RPWS_LOW_RATE_FULL

description: The Cassini Radio and Plasma Wave Science (RPWS) Low Rate Full Resolution Calibrated (RPWS_LOW_RATE_FULL) is a data set including all spectral density measurements acquired by the RPWS in units of electric or magnetic field spectral density. This data set includes calibrated values for each frequency channel for each sensor for all times during the mission including the two Venus flybys, the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data for this data set are acquired from the RPWS Low Frequency Receiver (LFR), Medium Frequency Receiver (MFR), Medium Frequency Digital Receiver (MFDR) (which can be used to replace MFR band 2 data) and High Frequency Receiver (HFR). Data are presented in a set of tables organized so as to have fixed-length records for ease in data handling. This data set is intended to be the most comprehensive and complete data set included in the Cassini RPWS archive. A browse data set is included with these data which provides for a graphical search of the data using a series of thumbnail and full-sized spectrograms which lead the user to the particular data file(s) of interest. This data set should be among the first used by a user of any of the RPWS archive as it will lead one to information required to search for more detailed or highly specialized products.
DOI: 10.48322/yhj0-qz98
title: Cluster-Rumba Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive
title: Cluster 2 Rumba Electron Drift Instrument (EDI) Data at the ESA Cluster Active Archive

description: The Electron Drift Instrument (EDI) data products from the Cluster spacecraft in three main categories: (1) Electron enegergies measured between 0.5 and 1.0 keV for the Windshield Wiper mode: time series of the three components of the electron drift velocity and of the three components of the electric field in Cartesian GSE coordinate system (corrected for spacecraft motion) with different qualities and time resolution at 1-4 sec (PP, PPP, MPD); (2) Ambient electron measurements at fixed enegeris of 0.5 or 1.0 keV: time series of electron counts normally at 16 ms for the three pitch angles 0 deg, 90 deg, 180 deg, the detector look direction in the spacecraft frame and in GSE and the status for AE mode; and (3) Overview plot of the main parameters for both modes for every 3 h for one reference spacecraft (usually Cluster III).  Besides the main products, there also are raw data and auxiliary data. Raw data consist of merged science files (MSF) that are obtained by merging the housekeeping and science (burst (BM) and normal (NM) mode) telemetry files. They are in binary format.  Auxiliary are either data used internally by the main data production software or data dedicated to intercalibration or time-interval lists of the EDI operation modes. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.
DOI: 10.48322/3cp4-n849
title: Cluster-Rumba Prime Parameter Electron Drift Instrument (EDI) Data
title: Cluster 1 Prime Parameter EDI data

description: This instrument (EDI: Electron Drift Instrument) measures the drift of a weak beam of test electrons that, when emitted in certain directions, return to the spacecraft after one gyration. This drift is related to the electric field and the gradient in the magnetic field, and these quantities can, by the use of different electron energies, be determined separately. The fundamental time step to determine the new parameters and direct the beams and the detectors is 2 ms. Inter-experiment links include: magnetic field information from FGM and STAFF, a blanking pulse received from WHISPER to warn of possible interference from that active experiment, and a similar blanking pulse sent to PEACE when the EDI electron beam could interfere with the PEACE electron measurement. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Electron Drift Instrument for Cluster, by G. Paschmann et al., from which this information was obtained.
DOI: 10.48322/1cyr-x753
title: Cluster-Salsa Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive
title: Cluster 2 Salsa Electron Drift Instrument (EDI) Data at CAA

description: The Electron Drift Instrument (EDI) data products from the Cluster spacecraft in three main categories: (1) Electron enegergies measured between 0.5 and 1.0 keV for the Windshield Wiper mode: time series of the three components of the electron drift velocity and of the three components of the electric field in Cartesian GSE coordinate system (corrected for spacecraft motion) with different qualities and time resolution at 1-4 sec (PP, PPP, MPD); (2) Ambient electron measurements at fixed enegeris of 0.5 or 1.0 keV: time series of electron counts normally at 16 ms for the three pitch angles 0 deg, 90 deg, 180 deg, the detector look direction in the spacecraft frame and in GSE and the status for AE mode; and (3) Overview plot of the main parameters for both modes for every 3 h for one reference spacecraft (usually Cluster III).  Besides the main products, there also are raw data and auxiliary data. Raw data consist of merged science files (MSF) that are obtained by merging the housekeeping and science (burst (BM) and normal (NM) mode) telemetry files. They are in binary format.  Auxiliary are either data used internally by the main data production software or data dedicated to intercalibration or time-interval lists of the EDI operation modes. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.
DOI: 10.48322/rwbc-0g86
title: Cluster-Samba Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive
title: Cluster 2 Samba Electron Drift Instrument (EDI) Data at the ESA Cluster Active Archive

description: The Electron Drift Instrument (EDI) data products from the Cluster spacecraft in three main categories: (1) Electron enegergies measured between 0.5 and 1.0 keV for the Windshield Wiper mode: time series of the three components of the electron drift velocity and of the three components of the electric field in Cartesian GSE coordinate system (corrected for spacecraft motion) with different qualities and time resolution at 1-4 sec (PP, PPP, MPD); (2) Ambient electron measurements at fixed enegeris of 0.5 or 1.0 keV: time series of electron counts normally at 16 ms for the three pitch angles 0 deg, 90 deg, 180 deg, the detector look direction in the spacecraft frame and in GSE and the status for AE mode; and (3) Overview plot of the main parameters for both modes for every 3 h for one reference spacecraft (usually Cluster III).  Besides the main products, there also are raw data and auxiliary data. Raw data consist of merged science files (MSF) that are obtained by merging the housekeeping and science (burst (BM) and normal (NM) mode) telemetry files. They are in binary format.  Auxiliary are either data used internally by the main data production software or data dedicated to intercalibration or time-interval lists of the EDI operation modes. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.
DOI: 10.48322/pn1d-v155
title: Cluster-Samba Prime Parameter Electron Drift Instrument (EDI) Data
title: Cluster 3 Prime Parameter EDI data

description: This instrument (EDI: Electron Drift Instrument) measures the drift of a weak beam of test electrons that, when emitted in certain directions, return to the spacecraft after one gyration. This drift is related to the electric field and the gradient in the magnetic field, and these quantities can, by the use of different electron energies, be determined separately. The fundamental time step to determine the new parameters and direct the beams and the detectors is 2 ms. Inter-experiment links include: magnetic field information from FGM and STAFF, a blanking pulse received from WHISPER to warn of possible interference from that active experiment, and a similar blanking pulse sent to PEACE when the EDI electron beam could interfere with the PEACE electron measurement. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Electron Drift Instrument for Cluster, by G. Paschmann et al., from which this information was obtained.
DOI: 10.17630/f4a20a60-4afe-4e8c-b64d-6ea24808538d
title: Data underpinning Tegan Knott's thesis

description: Indefinite embargo applied. Embargo reason: permission not provided to allow public access
DOI: 10.48322/sw7q-1m23
title: Cluster-Tango Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive
title: Cluster 2 Tango Electron Drift Instrument (EDI) Data at the ESA Cluster Active Archive

description: The Electron Drift Instrument (EDI) data products from the Cluster spacecraft in three main categories: (1) Electron enegergies measured between 0.5 and 1.0 keV for the Windshield Wiper mode: time series of the three components of the electron drift velocity and of the three components of the electric field in Cartesian GSE coordinate system (corrected for spacecraft motion) with different qualities and time resolution at 1-4 sec (PP, PPP, MPD); (2) Ambient electron measurements at fixed enegeris of 0.5 or 1.0 keV: time series of electron counts normally at 16 ms for the three pitch angles 0 deg, 90 deg, 180 deg, the detector look direction in the spacecraft frame and in GSE and the status for AE mode; and (3) Overview plot of the main parameters for both modes for every 3 h for one reference spacecraft (usually Cluster III).  Besides the main products, there also are raw data and auxiliary data. Raw data consist of merged science files (MSF) that are obtained by merging the housekeeping and science (burst (BM) and normal (NM) mode) telemetry files. They are in binary format.  Auxiliary are either data used internally by the main data production software or data dedicated to intercalibration or time-interval lists of the EDI operation modes. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.