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The Analysis of Physical, Physiological and Behavioral Data Collected From Sensors That Track the Mental Condition of Psychiatric Patients
ClinicalTrials.gov study NCT03714893. IPD Sharing: NO. Countries: 0. Publications: 0.
Data from: Synaptotagmin 7 functions as a Ca^2+ -sensor for synaptic vesicle replenishment
Open the record for dataset details and reuse information.
Sensors, Pathways and Transcription factors regulating IR-induced inflammatory transcriptional output [RNA-seq data set 1]
GEO Series GSE100961. Mus musculus. 241 samples. Type: Expression profiling by high throughput sequencing.
PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Cross Spectra, e-component, f-component, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board (DFB), SCMXlfhg ⨯ SCMXlfhg cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523
PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Cross Spectra, v-component, w-component, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board (DFB), SCMvlfhg ⨯ SCMwlfhg cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523
DMSP F16 Special Sensors-Ions, Electrons, and Scintillation (SSIES) Thermal Plasma Analysis Package, Level 2 (L2), 1 s Data in HDF Format
The Special Sensors-Ions, Electrons, and Scintillation (SSIES) thermal plasma analysis package is a suite of instruments built by the Center for Space Sciences at the University of Texas at Dallas and flown on a number of the DMSP satellites. SSIESS includes a Retarding Potential Analyzer (RPA), Ion Drift meter (IDM), scintillation meter, and Langmuir probe.
MMS 3 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Electrons, 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.
MMS 1 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Electrons, 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) DC-coupled Searchcoil Magnetometer, SCM, Cross Spectra, d-component, e-component, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board (DFB), SCMXlfhg ⨯ SCMXlfhg cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata.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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523
CASSINI E/J/S/SW MIMI CHEMS SENSOR UNCALIBRATED DATA V1.0
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.
MMS 2 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Electrons, 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.
PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Spectra, Low Frequency, High Gain, w-component, Sensor coordinates, Level 2 (L2), 6.99054 s Data
PSP FIELDS Digital Fields Board, DFB, SCMwlfhg 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 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 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 DC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB DC spectra data cadence is typically 30 NYseconds 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) AC-coupled Searchcoil Magnetometer, SCM, Cross Spectra, e-component, f-component, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board (DFB), XXX ⨯ YYY cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence). Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N. For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form 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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra 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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523
MMS 3 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.
PSP FIELDS Digital Fields Board (DFB) AC-coupled Searchcoil Magnetometer, SCM, Spectra, Medium Frequency, High Gain, x-component, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board, DFB, SCMmf 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, Spectra, Low Frequency, High Gain, v-component, Sensor coordinates, Level 2 (L2), 6.99054 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 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 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 DC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB DC spectra data cadence is typically 30 NYseconds 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) AC-coupled Differential Voltage, V1-V2, V3-V4 Antennae, Dipole Mode, Cross Spectra, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board (DFB), XXX ⨯ YYY cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence). Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N. For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form 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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra 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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523
MMS 2 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Electrons, 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.
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.
DMSP F16 Special Sensors-Ions, Electrons, and Scintillation (SSIES) Thermal Plasma Analysis Package, Level 2 (L2), 1 s Data in CDF Format
The Special Sensors-Ions, Electrons, and Scintillation (SSIES) thermal plasma analysis package is a suite of instruments built by the Center for Space Sciences at the University of Texas at Dallas and flown on a number of the DMSP satellites. SSIESS includes a Retarding Potential Analyzer (RPA), Ion Drift meter (IDM), scintillation meter, and Langmuir probe.
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Allen Brain Atlas
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
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OpenNeuro
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