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STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Fluxgate Magnetometer (MAG) Burst Mode, Magnetic Field Vector, Radial-Tangential-Normal (RTN) Coordinates, Level 1 (L1), 31 ms Data
This data product contains Level 1 0.03125-s or 32 Hz burst-mode values of solar wind magnetic field data measured by the IMPACT Magnetometer on STEREO-B in Radial-Tangential-Normal, RTN, coordinates.
MMS 1 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Quiet conditions), Level 2 (L2), Burst Mode, 30 ms Data
Magnetospheric Multiscale 1 (MMS 1) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for quiet magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.
PSP FIELDS Digital Fields Board (DFB) Searchcoil Magnetometer Waveform, Level 2 (L2), 3.413 ms Data
PSP FIELDS Digital Fields Board, DFB, Search Coil Magnetometer 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].The DFB continuous waveform data consist of time series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3].The Level 2 data products contained in this data file have been calibrated for:* 1) DFB in-band gain* 2) DFB analog filter gain and phase response* 3) DFB digital filter phase response* 4) The search coil preamplifier gain and phase response, when applicableCalibrations for the DFB digital filter gain response have not been implemented, but the required convolution kernel is provided in this file. It was decided not to apply the digital filter gain response calibration to these Level 2 data because the application of the calibrations can introduce non-physical power 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 voltage sensor preamplifiers have not been implemented as the preamplifier response is flat and equal to one throughout the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data. 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 in spacecraft coordinates (e.g. x,y,z) or in sensor coordinates (e.g. dV12, dV34 for voltage measurements and [u,v,w] for the searchcoil magnetometer.The time resolution of the DFB continuous waveform data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB continuous waveform data cadence is typically 256 samples/NYsecond [2].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
MMS 4 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Instrument Distributions, Level 2 (L2), Burst Mode, 30 ms Data
The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. This Product contains Phase Space Distribution Maps of those Burst Resolution Data selected for downlink. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Burst Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.
MMS 2 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM2), Level 2 (L2), Survey Mode, 31.25 ms Data
Electron Drift Instrument (EDI) Ambient Survey, Level 2, 0.03125 s Data (32 samples/s). EDI has two scientific data acquisition modes, called electric field mode and ambient mode. In electric field mode, two coded electron beams are emitted such that they return to the detectors after one or more gyrations in the ambient magnetic and electric field. The firing directions and times-of-flight allow the derivation of the drift velocity and electric field. In ambient mode, the electron beams are not used. The detectors with their large geometric factors and their ability to adjust the field of view quickly allow continuous sampling of ambient electrons at a selected pitch angle and fixed but selectable energy. To find the beam directions that will hit the detector, EDI sweeps each beam in the plane perpendicular to B at a fixed angular rate of 0.22 °/ms until a signal has been acquired by the detector. Once signal has been acquired, the beams are swept back and forth to stay on target. Beam detection is not determined from the changes in the count-rates directly, but from the square of the beam counts divided by the background counts from ambient electrons, i.e., from the square of the instantaneous signal-to-noise ratio (SNR). This quantity is computed from data provided by the correlator in the Gun-Detector Electronics that also generates the coding pattern imposed on the outgoing beams. If the squared SNR ratio exceeds a threshold, this is taken as evidence that the beam is returning to the detector. The thresholds for SNR are chosen dependent on background fluxes. They represent a compromise between getting false hits (induced by strong variations in background electron fluxes) and missing true beam hits. The basic software loop that controls EDI operations is executed every 2 ms. As the times when the beams hit their detectors are neither synchronized with the telemetry nor equidistant, EDI data have no fixed time-resolution. Data are reported in telemetry slots. In Survey, using the standard packing mode 0, there are eight telemetry slots per second and Gyn Detector Unit (GDU). The last beam detected during the previous slot will be reported in the current slot. If no beam has been detected, the data quality will be set to zero. In Burst telemetry there are 128 slots per second and GDU. The data in each slot consists of information regarding the beam firing directions (stored in the form of analytic gun deflection voltages), times-of-flight (if successfully measured), quality indicators, time stamps of the beam hits, and some auxiliary correlator-related information. Whenever EDI is not in electron drift mode, it uses its ambient electron mode. The mode has the capability to sample at either 90 degrees pitch angle or at 0/180 degrees (field aligned), or to alternate between 90 degrees and field aligned with selectable dwell times. While all options have been demonstrated during the commissioning phase, only the field aligned mode has been used in the routine operations phase. The choices for energy are 250 eV, 500 eV, and 1 keV. The two detectors, which are facing opposite hemispheres, are looking strictly into opposite directions, so while one detector is looking along B the other is looking antiparallel to B (corresponding to pitch angles of 180 and 0 degrees, respectively). The two detectors switch roles every half spin of the spacecraft as the tip of the magnetic field vector spins outside the field of view of one detector and into the field of view of the other detector. Starting January 4, 2016, the anodes were chosen such that the projection of the magnetic field vector was best aligned with the center of the first (that is, outer) of the four anodes. This provides coverage of a larger range of pitch angles in general. Data taken in this configuration are identified by the term "amb-pm2" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, channel 1 represents best the pitch angle of 0 degrees (or 180 degrees). The EDI instrument paper can be found at: http://link.springer.com/article/10.1007%2Fs11214-015-0182-7. The EDI instrument data products guide can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.
RENU2 UltraViolet PhotoMultiplier Tube (UVPMT) Atomic Oxygen Density, High Time Resolution (H0), 42 ms Data
Rocket Experiment for Neutral Upwelling 2, RENU2, UltraViolet PhotoMultiplier Tube, UVPMT, Counts. The UVPMT Instrument is used to observe Atomic Oxygen Signatures in Sunlight, that is, above the Payload.
MMS 1 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 2 (PM2), Level 2 (L2), Burst Mode, 0.9765625 ms Data
Electron Drift Instrument (EDI) Ambient Burst Survey, Level 2, 0.0009765625 s Data (1024 samples/s). EDI has two scientific data acquisition modes, called electric field mode and ambient mode. In electric field mode, two coded electron beams are emitted such that they return to the detectors after one or more gyrations in the ambient magnetic and electric field. The firing directions and times-of-flight allow the derivation of the drift velocity and electric field. In ambient mode, the electron beams are not used. The detectors with their large geometric factors and their ability to adjust the field of view quickly allow continuous sampling of ambient electrons at a selected pitch angle and fixed but selectable energy. To find the beam directions that will hit the detector, EDI sweeps each beam in the plane perpendicular to B at a fixed angular rate of 0.22 °/ms until a signal has been acquired by the detector. Once signal has been acquired, the beams are swept back and forth to stay on target. Beam detection is not determined from the changes in the count-rates directly, but from the square of the beam counts divided by the background counts from ambient electrons, i.e., from the square of the instantaneous signal-to-noise ratio (SNR). This quantity is computed from data provided by the correlator in the Gun-Detector Electronics that also generates the coding pattern imposed on the outgoing beams. If the squared SNR ratio exceeds a threshold, this is taken as evidence that the beam is returning to the detector. The thresholds for SNR are chosen dependent on background fluxes. They represent a compromise between getting false hits (induced by strong variations in background electron fluxes) and missing true beam hits. The basic software loop that controls EDI operations is executed every 2 ms. As the times when the beams hit their detectors are neither synchronized with the telemetry nor equidistant, EDI data have no fixed time-resolution. Data are reported in telemetry slots. In Survey, using the standard packing mode 0, there are eight telemetry slots per second and Gyn Detector Unit (GDU). The last beam detected during the previous slot will be reported in the current slot. If no beam has been detected, the data quality will be set to zero. In Burst telemetry there are 128 slots per second and GDU. The data in each slot consists of information regarding the beam firing directions (stored in the form of analytic gun deflection voltages), times-of-flight (if successfully measured), quality indicators, time stamps of the beam hits, and some auxiliary correlator-related information. Whenever EDI is not in electron drift mode, it uses its ambient electron mode. The mode has the capability to sample at either 90 degrees pitch angle or at 0/180 degrees (field aligned), or to alternate between 90 degrees and field aligned with selectable dwell times. While all options have been demonstrated during the commissioning phase, only the field aligned mode has been used in the routine operations phase. The choices for energy are 250 eV, 500 eV, and 1 keV. The two detectors, which are facing opposite hemispheres, are looking strictly into opposite directions, so while one detector is looking along B the other is looking antiparallel to B (corresponding to pitch angles of 180 and 0 degrees, respectively). The two detectors switch roles every half spin of the spacecraft as the tip of the magnetic field vector spins outside the field of view of one detector and into the field of view of the other detector. Starting January 4, 2016, the anodes were chosen such that the projection of the magnetic field vector was best aligned with the center of the first (that is, outer) of the four anodes. This provides coverage of a larger range of pitch angles in general. Data taken in this configuration are identified by the term "amb-pm2" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, channel 1 represents best the pitch angle of 0 degrees (or 180 degrees). The EDI instrument paper can be found at: http://link.springer.com/article/10.1007%2Fs11214-015-0182-7. The EDI instrument data products guide can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.
STEREO-A In-Situ Measurements of Particles and CME Transients (IMPACT) Fluxgate Magnetometer (MAG) Burst Mode, Magnetic Field Vector, Radial-Tangential-Normal (RTN) Coordinates, Level 1 (L1), 31 ms Data
This data product contains Level 1 0.03125-s or 32 Hz burst-mode values of solar wind magnetic field data measured by the IMPACT Magnetometer on STEREO-A in Radial-Tangential-Normal, RTN, coordinates.
MMS 3 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Distribution Moments, Level 2 (L2), Burst Mode, 30 ms Data
The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually Operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Results from integrating the standard Moments of Phase Space Distributions formed from the indicated Data Type (DES/DIS Burst, FS or SS). For Convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.
MMS 2 Electron Drift Instrument (EDI) Electric Field, Level 2 (L2), Burst Mode, 0.9765625 ms Data
Electron Drift Instrument (EDI) Electric Field Burst Survey, Level 2, 0.0009765625 s Data (1024 samples/s). EDI has two scientific data acquisition modes, called electric field mode and ambient mode. In electric field mode, two coded electron beams are emitted such that they return to the detectors after one or more gyrations in the ambient magnetic and electric field. The firing directions and times-of-flight allow the derivation of the drift velocity and electric field. In ambient mode, the electron beams are not used. The detectors with their large geometric factors and their ability to adjust the field of view quickly allow continuous sampling of ambient electrons at a selected pitch angle and fixed but selectable energy. To find the beam directions that will hit the detector, EDI sweeps each beam in the plane perpendicular to B at a fixed angular rate of 0.22 °/ms until a signal has been acquired by the detector. Once signal has been acquired, the beams are swept back and forth to stay on target. Beam detection is not determined from the changes in the count-rates directly, but from the square of the beam counts divided by the background counts from ambient electrons, i.e., from the square of the instantaneous signal-to-noise ratio (SNR). This quantity is computed from data provided by the correlator in the Gun-Detector Electronics that also generates the coding pattern imposed on the outgoing beams. If the squared SNR ratio exceeds a threshold, this is taken as evidence that the beam is returning to the detector. The thresholds for SNR are chosen dependent on background fluxes. They represent a compromise between getting false hits (induced by strong variations in background electron fluxes) and missing true beam hits. The basic software loop that controls EDI operations is executed every 2 ms. As the times when the beams hit their detectors are neither synchronized with the telemetry nor equidistant, EDI data have no fixed time-resolution. Data are reported in telemetry slots. In Survey, using the standard packing mode 0, there are eight telemetry slots per second and Gyn Detector Unit (GDU). The last beam detected during the previous slot will be reported in the current slot. If no beam has been detected, the data quality will be set to zero. In Burst telemetry there are 128 slots per second and GDU. The data in each slot consists of information regarding the beam firing directions (stored in the form of analytic gun deflection voltages), times-of-flight (if successfully measured), quality indicators, time stamps of the beam hits, and some auxiliary correlator-related information. Whenever EDI is not in electron drift mode, it uses its ambient electron mode. The mode has the capability to sample at either 90 degrees pitch angle or at 0/180 degrees (field aligned), or to alternate between 90 degrees and field aligned with selectable dwell times. While all options have been demonstrated during the commissioning phase, only the field aligned mode has been used in the routine operations phase. The choices for energy are 250 eV, 500 eV, and 1 keV. The two detectors, which are facing opposite hemispheres, are looking strictly into opposite directions, so while one detector is looking along B the other is looking antiparallel to B (corresponding to pitch angles of 180 and 0 degrees, respectively). The two detectors switch roles every half spin of the spacecraft as the tip of the magnetic field vector spins outside the field of view of one detector and into the field of view of the other detector. This is the primary data product generated from data collected in electric field mode. The science data generated are drift velocity and electric field data in various coordinate systems. They are derived from triangulation and/or time-of-flight analysis. Where both methods are applicable, their results will be combined using a weighting approach based on their relative errors. The EDI instrument paper can be found at: http://link.springer.com/article/10.1007%2Fs11214-015-0182-7. The EDI instrument data products guide can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.
MMS 1 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Partial Distribution Moments, Level 2 (L2), Burst Mode, 30 ms Data
FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually operates in Slow Survey (SS) Mode (60 s Resolution) outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Partial Moments that come from performing the Standard Moment Integrals over a limited Portion of Velocity Space. The resulting Quantities are named similarly to their corresponding Standard Moments, but are decorated with 'part' to differentiate. For example, density_part is the Density Moment integrated from a particular Energy Step to Infinity. These Partial Moments are formed from the indicated Data Type (DES/DIS Burst, FS or SS). For convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.
MMS 2 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Dynamic conditions), Level 2 (L2), Burst Mode, 30 ms Data
Magnetospheric Multiscale 2 (MMS 2) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for disturbed magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.
RENU2 COrnell Wire BOom Yo-yo (COWBOY) Electric Field Very Low Frequency Waves, High Time Resolution (H0), 1 ms Data
Rocket Experiment for Neutral Upwelling 2, RENU2, COrnell Wire BOom Yo-yo, COWBOY, Very Low Frequency, VLF, Electric Field Measurements
MMS 4 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Quiet conditions), Level 2 (L2), Burst Mode, 30 ms Data
Magnetospheric Multiscale 4 (MMS 4) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for quiet magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.
MMS 1 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM2), Level 2 (L2), Survey Mode, 31.25 ms Data
Electron Drift Instrument (EDI) Ambient Survey, Level 2, 0.03125 s Data (32 samples/s). EDI has two scientific data acquisition modes, called electric field mode and ambient mode. In electric field mode, two coded electron beams are emitted such that they return to the detectors after one or more gyrations in the ambient magnetic and electric field. The firing directions and times-of-flight allow the derivation of the drift velocity and electric field. In ambient mode, the electron beams are not used. The detectors with their large geometric factors and their ability to adjust the field of view quickly allow continuous sampling of ambient electrons at a selected pitch angle and fixed but selectable energy. To find the beam directions that will hit the detector, EDI sweeps each beam in the plane perpendicular to B at a fixed angular rate of 0.22 °/ms until a signal has been acquired by the detector. Once signal has been acquired, the beams are swept back and forth to stay on target. Beam detection is not determined from the changes in the count-rates directly, but from the square of the beam counts divided by the background counts from ambient electrons, i.e., from the square of the instantaneous signal-to-noise ratio (SNR). This quantity is computed from data provided by the correlator in the Gun-Detector Electronics that also generates the coding pattern imposed on the outgoing beams. If the squared SNR ratio exceeds a threshold, this is taken as evidence that the beam is returning to the detector. The thresholds for SNR are chosen dependent on background fluxes. They represent a compromise between getting false hits (induced by strong variations in background electron fluxes) and missing true beam hits. The basic software loop that controls EDI operations is executed every 2 ms. As the times when the beams hit their detectors are neither synchronized with the telemetry nor equidistant, EDI data have no fixed time-resolution. Data are reported in telemetry slots. In Survey, using the standard packing mode 0, there are eight telemetry slots per second and Gyn Detector Unit (GDU). The last beam detected during the previous slot will be reported in the current slot. If no beam has been detected, the data quality will be set to zero. In Burst telemetry there are 128 slots per second and GDU. The data in each slot consists of information regarding the beam firing directions (stored in the form of analytic gun deflection voltages), times-of-flight (if successfully measured), quality indicators, time stamps of the beam hits, and some auxiliary correlator-related information. Whenever EDI is not in electron drift mode, it uses its ambient electron mode. The mode has the capability to sample at either 90 degrees pitch angle or at 0/180 degrees (field aligned), or to alternate between 90 degrees and field aligned with selectable dwell times. While all options have been demonstrated during the commissioning phase, only the field aligned mode has been used in the routine operations phase. The choices for energy are 250 eV, 500 eV, and 1 keV. The two detectors, which are facing opposite hemispheres, are looking strictly into opposite directions, so while one detector is looking along B the other is looking antiparallel to B (corresponding to pitch angles of 180 and 0 degrees, respectively). The two detectors switch roles every half spin of the spacecraft as the tip of the magnetic field vector spins outside the field of view of one detector and into the field of view of the other detector. Starting January 4, 2016, the anodes were chosen such that the projection of the magnetic field vector was best aligned with the center of the first (that is, outer) of the four anodes. This provides coverage of a larger range of pitch angles in general. Data taken in this configuration are identified by the term "amb-pm2" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, channel 1 represents best the pitch angle of 0 degrees (or 180 degrees). The EDI instrument paper can be found at: http://link.springer.com/article/10.1007%2Fs11214-015-0182-7. The EDI instrument data products guide can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.
MMS 3 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM2), Level 2 (L2), Survey Mode, 31.25 ms Data
Electron Drift Instrument (EDI) Ambient Survey, Level 2, 0.03125 s Data (32 samples/s). EDI has two scientific data acquisition modes, called electric field mode and ambient mode. In electric field mode, two coded electron beams are emitted such that they return to the detectors after one or more gyrations in the ambient magnetic and electric field. The firing directions and times-of-flight allow the derivation of the drift velocity and electric field. In ambient mode, the electron beams are not used. The detectors with their large geometric factors and their ability to adjust the field of view quickly allow continuous sampling of ambient electrons at a selected pitch angle and fixed but selectable energy. To find the beam directions that will hit the detector, EDI sweeps each beam in the plane perpendicular to B at a fixed angular rate of 0.22 °/ms until a signal has been acquired by the detector. Once signal has been acquired, the beams are swept back and forth to stay on target. Beam detection is not determined from the changes in the count-rates directly, but from the square of the beam counts divided by the background counts from ambient electrons, i.e., from the square of the instantaneous signal-to-noise ratio (SNR). This quantity is computed from data provided by the correlator in the Gun-Detector Electronics that also generates the coding pattern imposed on the outgoing beams. If the squared SNR ratio exceeds a threshold, this is taken as evidence that the beam is returning to the detector. The thresholds for SNR are chosen dependent on background fluxes. They represent a compromise between getting false hits (induced by strong variations in background electron fluxes) and missing true beam hits. The basic software loop that controls EDI operations is executed every 2 ms. As the times when the beams hit their detectors are neither synchronized with the telemetry nor equidistant, EDI data have no fixed time-resolution. Data are reported in telemetry slots. In Survey, using the standard packing mode 0, there are eight telemetry slots per second and Gyn Detector Unit (GDU). The last beam detected during the previous slot will be reported in the current slot. If no beam has been detected, the data quality will be set to zero. In Burst telemetry there are 128 slots per second and GDU. The data in each slot consists of information regarding the beam firing directions (stored in the form of analytic gun deflection voltages), times-of-flight (if successfully measured), quality indicators, time stamps of the beam hits, and some auxiliary correlator-related information. Whenever EDI is not in electron drift mode, it uses its ambient electron mode. The mode has the capability to sample at either 90 degrees pitch angle or at 0/180 degrees (field aligned), or to alternate between 90 degrees and field aligned with selectable dwell times. While all options have been demonstrated during the commissioning phase, only the field aligned mode has been used in the routine operations phase. The choices for energy are 250 eV, 500 eV, and 1 keV. The two detectors, which are facing opposite hemispheres, are looking strictly into opposite directions, so while one detector is looking along B the other is looking antiparallel to B (corresponding to pitch angles of 180 and 0 degrees, respectively). The two detectors switch roles every half spin of the spacecraft as the tip of the magnetic field vector spins outside the field of view of one detector and into the field of view of the other detector. Starting January 4, 2016, the anodes were chosen such that the projection of the magnetic field vector was best aligned with the center of the first (that is, outer) of the four anodes. This provides coverage of a larger range of pitch angles in general. Data taken in this configuration are identified by the term "amb-pm2" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, channel 1 represents best the pitch angle of 0 degrees (or 180 degrees). The EDI instrument paper can be found at: http://link.springer.com/article/10.1007%2Fs11214-015-0182-7. The EDI instrument data products guide can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.
MMS 3 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Quiet conditions), Level 2 (L2), Burst Mode, 30 ms Data
Magnetospheric Multiscale 3 (MMS 3) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for quiet magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.
MMS 1 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Dynamic conditions), Level 2 (L2), Burst Mode, 30 ms Data
Magnetospheric Multiscale 1 (MMS 1) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for disturbed magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.
PSP FIELDS Fluxgate Magnetometer (MAG) Magnetic Field Vectors, Radial-Tangential-Normal, RTN, Coordinates, 4 samples/cycle, Level 2 (L2), 3.413 ms Data
Parker Solar Probe FIELDS Instrument Suite Fluxgate Magnetometer, MAG, Data: The time resolution of the MAG time series data varies with instrument mode ranging from 2.289 samples/s to 292.9 samples/s. These two data sampling rates corresponding to 2 samples or 256 samples per 0.874 s where 0.874 s is equal to 2^25 divided 38.4 MHz. See reference [2] for a complete explanation of the MAG instrument sampling methodology. The Magnetometer has four ranges: ±1024 nT, ±4096 nT, ±16,384 nT, and ±65,536 nT. The Magnetometer Range is selected by an algorithm based on the strength of the ambient magnetic field. The magnetic field measurement precision is ±15 bits, based on the 16-bit Analog to Digital Converter, ADC.References:* 1. Fox, N.J., Velli, M.C., Bale, S.D. et al. Space Sci Rev (2016) 204: 7. https://doi.org/10.1007/s11214-015-0211-6* 2. Bale, S.D., Goetz, K., Harvey, P.R. et al. Space Sci Rev (2016) 204: 49. https://doi.org/10.1007/s11214-016-0244-5
MMS 4 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Dynamic conditions), Level 2 (L2), Burst Mode, 30 ms Data
Magnetospheric Multiscale 4 (MMS 4) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for disturbed magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.
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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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