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MMS 1 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Ions, Level 2 (L2), Burst Mode, 0.3025 s Data

Fly's Eye Electron Proton Spectrometer (FEEPS) Burst Data. The Energetic Particle Detector (EPD) investigation aboard the four MMS spacecraft consists of two instrument designs, the FEEPS and the EIS (Energetic Ion Spectrometer). A FEEPS consists of six Heads, each composed of two Eyes. Each eye is a particle telescope with a single silicon detector. There are nine electron eyes and three ion eyes per FEEPS. The energy coverage is from 25 keV to 650 keV for electrons and 45 keV to 650 keV for ions. Each eye has sixteen energy channels, the spacing of which can be modified by command. The fields of view and pointing of each eye are designed to provide a broad, instantaneous field of view for the twelve eyes per FEEPS.

MAVEN SEP Calibrated Ion and Electron Spectra Data Collection (Sensor 1)

Calibrated MAVEN Solar Energetic Particle (SEP) Instrument Sensor 1 ion and electron spectra. The data include total (integrated) and differential (as a function of 28 energy windows) ion and electron number fluxes in forward and reverse look directions. Description of the SEP instrument can be found on the SEP home page https://lasp.colorado.edu/maven/science/instrument-package/sep/ and in the SEP instrument publication https://doi.org/10.1007/s11214-015-0218-z.

MMS 1 Active Spacecraft Potential Control (ASPOC), Sensors 1 and 2, Level 2 (L2), Survey Mode, 1 s Data

MMS 1 Active Spacecraft Potential Control (ASPOC) - Sensors 1 and 2 Ion Beam Current Rates, Beam Energies, and Instrument Status variables. In tenuous plasma regions, the floating potential of a sunlit spacecraft is positively charged, reaching up to tens of Volts. The corresponding electric field disturbs the ambient plasma measurements obtained from electron and ion sensors and the large fluxes of attracted photo-electrons can significantly reduce the lifetime of the micro-channel plate. The electric field measurements can be also contaminated by the high spacecraft potential values. The Active Spacecraft Potential Control neutralizes the spacecraft potential by releasing positively charged Indium ions. The ASPOCs neutralize the electrical potential of the spacecraft, limiting or eliminating spurious electric fields that can contaminate measurements. This allows observations of the more scientifically important low-energy ions and electrons.

MMS 3 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Ions, Level 2 (L2), Survey Mode, 2.42 s Data

Fly's Eye Electron Proton Spectrometer (FEEPS) Survey Data. The Energetic Particle Detector (EPD) investigation aboard the four MMS spacecraft consists of two instrument designs, the FEEPS and the EIS (Energetic Ion Spectrometer). A FEEPS consists of six Heads, each composed of two Eyes. Each eye is a particle telescope with a single silicon detector. There are nine electron eyes and three ion eyes per FEEPS. The energy coverage is from 25 keV to 650 keV for electrons and 45 keV to 650 keV for ions. Each eye has sixteen energy channels, the spacing of which can be modified by command. The fields of view and pointing of each eye are designed to provide a broad, instantaneous field of view for the twelve eyes per FEEPS.

PSP FIELDS Digital Fields Board (DFB) AC-coupled Searchcoil Magnetometer, SCM, Spectra, Low Frequency, High Gain, f-component, Sensor coordinates, Level 2 (L2), 0.873813 s Data

PSP FIELDS Digital Fields Board, DFB, SCMflfhg data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time. These spectra are averaged over both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYsecond when the data cadence is equal to one NYsecond. Less data are averaged by a factor of 2^N for data cadences that are faster than one NYsecond by 2^N. For cadences slower than one NYsecond, the first 1/8 of each NYsecond of data included are averaged together to construct the reported data.The Level 2 data products contained in this data file have been calibrated for:* 1) The Hanning window used in the spectral calculation* 2) DFB in-band gain* 3) DFB analog filter gain response* 4) DFB digital filter gain response* 5) The search coil preamplifier response, when applicable* 6) The bandwidth of each spectral binNote that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts squared per Hertz. Likewise, all magnetic field quantities when present in these Level 2 data product are expressed by using units of nanoTesla squared per Hertz.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements. For solar orbits 1 and 2, the search coil magnetometer spectral data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field spectral data are in expressed in search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates into [u,v,w] search coil sensor coordinates, use the following matrix, written in IDL notation, and the following equation: spectra_uvw_vector = R ## spectra_def_vector.R = [[ 0.46834856, -0.81336422 , 0.34509170] [ -0.66921924, -0.071546954, 0.73961249] [ -0.57688408, -0.57733845 , -0.57782790]]The time resolution of the DFB AC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB AC spectra data cadence is typically NYsecond NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344

PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Bandpass filtered, Low Frequency, High Gain, v-component, Sensor coordinates, Level 2 (L2), 0.873813 s Data

PSP FIELDS Digital Fields Board, DFB, SCMvlfhg data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB DC bandpass data consist of peak and average values of the absolute value of bandpassed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3].The Level 2 data products contained in this data file have been calibrated for:* 1) The ~6.3 dB loss associated with forming the bandpass signal, see reference [3]* 2) DFB in-band gain* 3) The search coil preamplifier response, when applicable* 4) DFB digital filter time delays, the DFB filter time delays become significant in the lowest frequency DC bandpass binsCalibrations for the DFB digital filter gains and analog filter gains have not been implemented as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response and because all bins except the highest frequency bin have a flat gain response equal to one due to these filters. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts. Likewise, all magnetic field quantities when present in these Level 2 data products are expressed by using units of nanoTelsas.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements and [u,v,w] for the searchcoil magnetometer.The time resolution of the DFB DC bandpass filtered data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB DC bandpass filtered data cadence is typically 1 NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344

RENU2 Ion Gauge (IG2) Sensor Pressure, High Time Resolution (H0), 1 ms Data

Rocket Experiment for Neutral Upwelling 2, RENU2, Ionization Gauge, Neutral Gas Pressure Measurements

restrictedcc-by-4.0Feb 2024View details →

zenodo16/100

Sensor foil CO2 measurements and codes for data analysis

Repository containing the sensor foil images (CO2_sensor_foils_data.zip) and containing the codes for the extrapolation of root properties and data analysis (optodes.zip).

geo12/100

Expression data from Arabidopsis seedlings expressing a synthetic oxygen sensor device

GEO Series GSE118364. Arabidopsis thaliana. 2 samples. Type: Expression profiling by array.

openGEO-OpenNov 2018View details →

zenodo12/100

Biometric sensor and smartwatch response data collected during VR user studies for Worker Safety III

Two related datasets are included documenting users' sensor data and responses to alarms on a smartwatch during virtrual reality (VR) worker safety experiments on an integrated traffic simulation and VR platform. <ul> <li>watchData.csv records the times at which the user received an alarm on an Apple Watch and times when they tapped the watch screen to acknowledge the alarm.</li> <li>HRData.csv records blood volume pulse (BVP), inter-beat interval (IBI), and heart rate (HR) data for each user Data was recorded using an Empatica E4 PPG (photoplethysmography) wristband.</li> </ul> Both csv files shared the same column headers with the following descriptions: <ul> <li>UserID - Each user has a unique 4 digit ID randomly assigned to them at their first VR experiment.</li> <li>Scenario - Indicates which work zone safety Scenario the user experienced. <ul> <li>Scenario 1: Placing cones in a mobile work zone</li> <li>Scenario 2: Sensor installation on highway</li> <li>Scenario 3: Surveying in urban intersections</li> </ul> </li> <li>Trial - Indicates how many times they have experienced the same VR scenario (i.e. Scenario 3, Trial 2 means the user is experiencing Scenario 3 for the second time)</li> <li>VibrationOnly - Indicates the modality of alarms the user received during the trial. <ul> <li>VibrationOnly = 1 indicates that the alarms were haptic/vibrations only.</li> <li>VibrationOnly = 0 indicates that the alarms were haptic/vibrations AND sounds.</li> </ul> </li> <li>Timestamp - Local timestamp of the data recording</li> <li>Time Elapsed - Time that has passed since the start of the trial</li> <li>From - Indicates the source of the data <ul> <li>From = PPG - indicates the data is from the heart rate sensor</li> <li>From = Watch - indicates the data is from the Apple smartwatch, generally applies to when the user has responded on the watch/acknowledged the watch alarm</li> <li>From = VR - indicates the data is from the traffic simulation, generally applies to when speeding/collision cars trigger an alarm on the Apple smartwatch</li> <li>From = Ultrasonic - indicates the data is from an ultrasonic sensor detecting when the user was on the edge of the work zone perimeter.</li> </ul> </li> <li>Event - indicates the event being recorded <ul> <li>BVP/IBI/HR - indicates the meaning of the three numbers in the Values column (see Values below)</li> <li>Start Simulation - indicates when the trial began</li> <li>Received car approaching alert, mode=x, id=xxx <ul> <li>Mode indicates the type of alarm duration, frequency, and number of repetitions.</li> <li>ID indicates the cause of the alarm</li> </ul> </li> </ul> </li> <li>Type - indicates additional categorizations of events <ul> <li>Speeding/Collision - indicates the alarm was caused by a speeding or collision car</li> <li>Perimeter - indicates the alarm was triggered when the user was on the edge of the work zone perimeter.</li> <li>Response - indicates the user responded/acknowledged the alarm on the smartwatch by tapping the watch screen.</li> <li>BVP/IBI/HR - indicates the meaning of the three numbers in the Values column (see Values below)</li> </ul> </li> <li>Values <ul> <li>For Type=Response, Values indicates the alarm id the user responded to. Response time has to be calculated by subtracting the Time Elapsed of the Response row with the corresponding Time Elapsed of the alarm id row</li> <li>For Type="Received...", Values indicates the alarm mode and id</li> <li>For Type=BVP/IBI/HR, three values are listed indicating respectively blood volume pulse (BVP), inter-beat interval (IBI), and heart rate (HR) data</li> </ul> </li> </ul> Data requests and inquiries can be made by contacting Dr. Semiha Ergan at semiha@nyu.edu

restrictedJun 2022View details →

zenodo12/100

Environmental sensor data for occupancy detection

This dataset consist of measurements from environmental sensors, installed in different rooms of a building under construction. The data were collected during the EU project ASHVIN and can be used for occupancy detection. The dataset includes the following variables: timestamp; date; time; sound level; temperature; relative humidity; dust; pressure; activity; activity (boolean). The columns 'activity' can be used as ground truth for occupancy detection.

restrictedJul 2023View details →

CASSINI E/J/S/SW MIMI INCA SENSOR UNCALIBRATED DATA V1.0

The Cassini Magnetospheric Imaging Instrument(MIMI) Imaging Neutral Camera (INCA) uncalibrated data set includes all data collected from the MIMI Data Processing Unit during the mission. The original data has been decommutated and decoded by software at the Applied Physics Laboratory (APL) and has been then further ordered and filtered by software at Fundamental Technologies, LLC. The data is provided in an uncalibrated form in conjunction with a PDS MIMI calibration volume COMIMI_0000 which provides specific algorithms for the derivation of calibrated data. This data set includes uncalibrated values of counts in the form of rates and of rate images for the INCA sensor for all times during the mission including the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data are presented in a set of tables which are of variable length and use a comma to separate various fields. This data set is intended to be the most comprehensive and complete data set included in the Cassini MIMI INCA archive. A browse data set is included with Key Parameter data that is calibrated using the algorithms provided in the Calibration volume. In addition, a series of images are provided with the KP browse data that displays the KP data which can lead the user to the particular times of interest. This data set should be among the first used by a user of any of the MIMI INCA archive as it will lead one to information required to search for more detailed or highly specialized features in the original data.

CASSINI E/J/S/SW MIMI LEMMS SENSOR UNCALIBRATED DATA V1.1

The Cassini Magnetospheric Imaging Instrument(MIMI) Low Energy Magnetospheric Measurement System (LEMMS) uncalibrated data set includes all data collected from the MIMI Data Processing Unit during the mission. The original data has been decommutated and decoded by software at the Applied Physics Laboratory (APL) and has been then further ordered and filtered by software at Fundamental Technologies, LLC. The data is provided in an uncalibrated form in conjunction with a PDS MIMI calibration volume COMIMI_0000 which provides specific algorithms for the derivation of calibrated data. This data set includes uncalibrated values for each energy channel for the LEMMS sensor for all times during the mission including the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data are presented in a set of tables which are of variable length and use a comma to separate various fields. This data set is intended to be the most comprehensive and complete data set included in the Cassini MIMI LEMMS archive. A browse data set is included with Key Parameter data that is calibrated using the algorithms provided in the Calibration volume. In addition, a series of images are provided with the KP browse data that displays the KP data which can lead the user to the particular times of interest. This data set should be among the first used by a user of any of the MIMI LEMMS archive as it will lead one to information required to search for more detailed or highly specialized features in the original data.

CASSINI E/J/S/SW MIMI INCA SENSOR UNCALIBRATED DATA V1.1

CASSINI S MIMI LEMMS SENSOR CALIBRATED DATA V1.0

The Cassini Magnetospheric Imaging Instrument (MIMI) Low Energy Magnetospheric Measurements (LEMMS) measures ions and electrons in the energy range 0.03 to 18 MeV for ions and 0.015 to 0.884 MeV for electrons. The LEMMS calibrated data set includes two types of daily plots -- one presenting energy-time spectorgrams in units of intensity, and one with plots of particle pressures. There are also four types of averaged data -- minute and hourly averages for accumulator rate data and PHA data (ions and electrons). These data have been created at the Johns Hopkins University Applied Physics Laboratory by applying the calibrations and averaging. Averaging is done by first defining time periods, and then averaging all data points within those fixed intervals. The time reported is the midpoint time of the interval.

CASSINI E/J/S/SW MIMI CHEMS SENSOR UNCALIBRATED DATA V1.1

The Cassini Magnetospheric Imaging Instrument(MIMI) Charge Energy Mass Spectrometer (CHEMS) uncalibrated data set includes all data collected from the MIMI Data Processing Unit during the mission. The original data has been decommutated and decoded by software at the Applied Physics Laboratory (APL) and has been then further ordered and filtered by software at Fundamental Technologies, LLC. The data is provided in an uncalibrated form in conjunction with a PDS MIMI calibration volume COMIMI_0000 which provides specific algorithms for the derivation of calibrated data. This data set includes uncalibrated values for each energy and mass channel for the CHEMS sensor for all times during the mission including the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data are presented in a set of tables which are of variable length and use a comma to separate various fields. This data set is intended to be the most comprehensive and complete data set included in the Cassini MIMI CHEMS archive. A browse data set is included with Key Parameter data that is calibrated using the algorithms provided in the Calibration volume. In addition, a series of images are provided with the KP browse data that displays the KP data which can lead the user to the particular times of interest. This data set should be among the first used by a user of any of the MIMI CHEMS archive as it will lead one to information required to search for more detailed or highly specialized features in the original data.

CASSINI S MIMI CHEMS SENSOR CALIBRATED DATA V1.0

The Cassini Magnetospheric Imaging Instrument(MIMI) Charge Energy Mass Spectrometer (CHEMS) contains a deflection system and an overall field of view of 159 x 4 deg. that is comprised of three distinct energetic particle telescopes each having a field of view of 53 x 4. All telescopes share the same deflection mechanism, but each has its own start and stop microchannel plate (MCP) and its own solid-state detector (SSD). Much of the data returned by CHEMS is separated by telescope. The deflection plate power supply (DPPS) has 32 different voltages that can be applied across the deflection plates. For any single DPPS step, the electrostatic analyzer only transmits incoming ions within a narrow range of energy per charge (a 3% pass band). The CHEMS calibrated data set includes the Pulse Height Analysis (PHA) data collected during the Saturn tour. CHEMS PHA provides a list of individually detected particles, with specific detection parameters for each event, including TOF, energy deposited in the SSD, and telescope number. The energy per charge data for six ion species (H+, He+, H2+, He++, O++, W+) are presented in two forms. (The W+ water ion group includes O+, OH+, H20+ and H30+). One form is a set of tables which are of variable length and use a comma to separate various fields, and the other is a PDF file containing the energy per charge spectrograms and are based on CHEMS PHA data. The original data has been decommutated and decoded by software at the Applied Physics Laboratory (APL) and calibrated and further processed by software at the University of Maryland. This data set should be among the first used by a user of any of the MIMI CHEMS archive as it will lead one to information required to search for more detailed or highly specialized features in the original data.

DMSP F18 Special Sensor J, SESS/SSJ5, Precipitating Electrons and Ions Observed at 850 km, 1 s Data

Precipitating Electrons And ions observed at nominally 850 km Altitude and over a Range of Energies from 30 eV to 30 keV by using the Special Sensor J, SSJ, Instrument. Please contact Rob.Redmon@noaa.gov with Questions and Comments. Many Individuals made Important Contributions including: D. Hardy, E. Holeman, F. Rich, D. Ober, G. Wilson, J. Machuzak, K. Kadinsky-Cade, J. McGarity, W.F. Denig, K. Martin, R. Redmon, D. Knipp, L. Kilcommons.

CASSINI S MIMI INCA SENSOR CALIBRATED DATA V1.0

The Ion and Neutral Camera (INCA) obtains remote images of the global distribution of energetic ions for energies from 7 keV/nucleon to 8 MeV/nucleon, discriminated according to energy and mass species (oxygen and hydrogen). To obtain the images, INCA measures the arrival directions, energy and mass species of Energetic Neutral Atoms (ENA's) using the relatively new technique of ENA imaging. INCA also can be commanded to obtain very high sensitivity ion measurements, providing the angular, energy and species distributions of in-situ O and H ions. The Cassini Magnetospheric Imaging Instrument(MIMI) Imaging Neutral Camera (INCA) calibrated data set includes all image data collected from the MIMI Data Processing Unit during the Saturn tour. The original data has been decommutated, decoded, calibrated and further processed by software at the Applied Physics Laboratory (APL). The calibrated image data is provided in three forms: an averaged form where the original image N x N pixel images pixels intensity are averaged to a single value for one species and time-of-flight (TOF) combination, browse images which display rows and columns of images for one species and TOF combination, and movies which display averaged ENA image skymaps. Calibration of INCA data has been described fully in the Cassini/MIMI Data User Guide. [VANDEGRIFFETAL2012] This data set should be among the first used by a user of any of the MIMI INCA archive as it will lead one to information required to search for more detailed or highly specialized features in the original data.

DMSP F17 Special Sensor J, SESS/SSJ5, Precipitating Electrons and Ions Observed at 850 km, 1 s Data