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Polar Plasma Wave Instrument (PWI), Sweep Frequency Receivers A and B - 2 sec resolution fields
The PO_H1_PWI CDF files contain spectral densities of magnetic and electric field measurements from the Sweep Frequency Receiver-A and B. These files also contain correlation, electron cyclotron frequency, upper hybrid frequency and electron number density data. A full frequency sweep for the SFR takes about 33 seconds. From about 12.5 kHz to 800 kHz a full frequency spectrum can be obtained every 2.4 sec in the log mode. There are 224 SFR frequency bands, logarithmically spaced. When SFR_MODE is Linear, the 448 linear frequency bands are mapped to 224 logarithmic bands. The Polar Sweep Frequency Receiver-A (SFR-A) made use of either the Eu (130 m, spin-plane) or Ez (14 m, spin axis) two-sphere electric dipole antennas. Between March 25, 1996 and May 26, 1996, the Eu antenna was the default antenna, from May 27, 1996 through February 9, 1997 the Ez antenna was used and from February 10, 1997 until September 17, 1997 the SFR-A returned to using the Eu antenna. The SFR-A receiver spanned the frequency range from 26 Hz to 808 kHz in 5 bands: 26-200 Hz, 0.2 - 1.6 kHz, 1.7 - 12.6 kHz, 13-100 kHz, 100-808 kHz. The Polar PWI Sweep Frequency Receiver-B (SFR-B) collected data from March 1996 to September 1997. The SFR-B used the magnetic loop antenna (mounted on a 6m boom and oriented parallel to the Eu antenna). The SFR-B receiver spanned the frequency range from 26 Hz to 808 kHz in 5 bands: 26-200 Hz, 0.2 - 1.6 kHz, 1.7 - 12.6 kHz, 13-100 kHz, 100-808 kHz.
MMS 3 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM1), 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. Up until January 4, 2016 the anodes were chosen such that the magnetic field vector projected into the plane of the micro-channel plate entry surface was best aligned with the center of the four anodes ( that is, with the gap between the inner two of the four anodes). Data taken in this configuration are using the term "amb" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, the average (or sum) of the center two channels (channels 2 and 3) 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/.
Swift XRT Instrument Log
The XRT runs only one type of configuration mode/window in a given time interval. The table therefore contains for a given time interval a single record that describes one configuration. A new record is generated when the following is changing within an observation: new operating mode , new pointing mode, or new window configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
MMS 3 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Instrument Distributions, Level 2 (L2), Fast Mode, 4.5 s 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 are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. This Product contains Phase Space Distribution Maps of Results from surveying the High Resolution Observations during each 4.5 s Period. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Fast Survey Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.
MMS 3 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.
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 10 s Data
Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 10 s Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/6b2f-mx69
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 1 h Data
Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 1 h Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/ahkk-d044
MMS 2 Electron Drift Instrument (EDI) Quality 0 Counts, Level 2 (L2), Burst Mode, 7.8125 ms Data
Electron Drift Instrument (EDI) Q0 Burst Survey, Level 2, 0.0078125 s Data (128 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. These data are a by-product generated from data collected in electric field mode. Whenever no return beam is found in a particular time slot by the flight software to be reported will be flagged with the lowest quality level (quality zero). The ground processing generates a separate data product from these counts data. 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/.
Geotail Linearly Interpolated 60 s Resolution Coordinates Comprehensive Plasma Instrumentation (CPI) data in GSE
Geotail linearly interpolated to have the measurements on the minute at 60 s resolution CPI data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument (ISOIS EPI) Merged Summary, Level 2 (L2), 1 min Data
Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi and EPI-Lo, Summary data: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument (ISOIS EPI) Merged Summary, Level 2 (L2), 1 min Data [Data set]. NASA Space Physics Data Facility.
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) Low Energy Telescope 2 (LET2) Rates, Level 2 (L2), 1 h Data
Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, Low Energy Telescope 2, LET2, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) Low Energy Telescope 2 (LET2) Rates, Level 2 (L2), 1 h Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/2xj3-hj37
MMS 2 Fast Plasma Investigation, Dual Ion Spectrometer (FPI, DIS) Instrument Distributions, Level 2 (L2), Fast Mode, 4.5 s 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 are aggregated onboard and made available at Survey (4.5 s) Resolution in this Mode. This Product contains Phase Space Distribution Maps of Results from surveying the High Resolution Observations during each 4.5 s Period. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Fast Survey Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.
MMS 3 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM1), 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. Up until January 4, 2016 the anodes were chosen such that the magnetic field vector projected into the plane of the micro-channel plate entry surface was best aligned with the center of the four anodes ( that is, with the gap between the inner two of the four anodes). Data taken in this configuration are using the term "amb" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, the average (or sum) of the center two channels (channels 2 and 3) 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 1 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM1), 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. Up until January 4, 2016 the anodes were chosen such that the magnetic field vector projected into the plane of the micro-channel plate entry surface was best aligned with the center of the four anodes ( that is, with the gap between the inner two of the four anodes). Data taken in this configuration are using the term "amb" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, the average (or sum) of the center two channels (channels 2 and 3) 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 4 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM1), 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. Up until January 4, 2016 the anodes were chosen such that the magnetic field vector projected into the plane of the micro-channel plate entry surface was best aligned with the center of the four anodes ( that is, with the gap between the inner two of the four anodes). Data taken in this configuration are using the term "amb" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, the average (or sum) of the center two channels (channels 2 and 3) 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/.
East China Sea validation measurements for GOCI instrument
Measurements made in the East China Sea in 2013 to validate the South Korean GOCI instrument.
MMS 1 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 3 Electron Drift Instrument (EDI) Quality 0 Counts, Level 2 (L2), Burst Mode, 7.8125 ms Data
Electron Drift Instrument (EDI) Q0 Burst Survey, Level 2, 0.0078125 s Data (128 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. These data are a by-product generated from data collected in electric field mode. Whenever no return beam is found in a particular time slot by the flight software to be reported will be flagged with the lowest quality level (quality zero). The ground processing generates a separate data product from these counts data. 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/.
PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument (ISOIS EPI) Merged Summary, Level 2 (L2), 1 min Data
Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi and EPI-Lo, Summary data: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument (ISOIS EPI) Merged Summary, Level 2 (L2), 1 min Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/mede-7j02
MMS 2 Electron Drift Instrument (EDI) Ambient Electron Flux, Projection Method 1 (PM1), 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. Up until January 4, 2016 the anodes were chosen such that the magnetic field vector projected into the plane of the micro-channel plate entry surface was best aligned with the center of the four anodes ( that is, with the gap between the inner two of the four anodes). Data taken in this configuration are using the term "amb" in the data product names. In the burst data where four channels (corresponding to the four adjacent sensor anode pads) are sampled per GDU, the average (or sum) of the center two channels (channels 2 and 3) 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/.
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.