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Loysburg (LOYS) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Loysburg, PA, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (LOYS), Station Location: (GEO Latitude 40.2, Longitude 281.6), THEMIS EPO/UCLA Network

PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Spectra, Low Frequency, High Gain, d-component, Sensor coordinates, Level 2 (L2), 6.99054 s Data

PSP FIELDS Digital Fields Board, DFB, SCMdlfhg 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, V3-V4 Antennae, Dipole Mode, Spectra, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data

PSP FIELDS Digital Fields Board, DFB, dV34hg 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

MMS 1 Search Coil Magnetometer (SCM) AC Magnetic Field Level 2 (L2), Survey Mode, 32 Sample/s Data

Search Coil Magnetometer (SCM) AC Magnetic Field (32 samples/s), Level 2, Survey Mode Data. The tri-axial Search-Coil Magnetometer with its associated preamplifier measures three-dimensional magnetic field fluctuations. The analog magnetic waveforms measured by the SCM are digitized and processed inside the Digital Signal Processor (DSP), collected and stored by the Central Instrument Data Processor (CIDP) via the Fields Central Electronics Box (CEB). Prior to launch, all SCM Flight models were calibrated by LPP team members at the National Magnetic Observatory, Chambon-la-Foret (Orleans). Once per orbit, each SCM transfer function is checked thanks to the onboard calibration signal provided by the DSP. The SCM is operated for the entire MMS orbit in survey mode. Within scientific Regions Of Interest (ROI), burst mode data are also acquired as well as high speed burst mode data. This SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in the GSE frame. The SCM instrument paper can be found at http://link.springer.com/article/10.1007/s11214-014-0096-9 and the SCM data product guide at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.

MMS 4 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/.

Kuujjuarapik (KJPK) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Kuujjuarapik, QC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (KJPK), Station Location: (GEO Latitude 55.3, Longitude 282.2), AUTUMNX Network

Pinawa (PINA) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Pinawa, MB, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (PINA), Station Location: (GEO Latitude 50.2, Longitude 263.9), THEMIS GBO/Carisma Network

Pine Ridge (PINE) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Pine Ridge, SD, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (PINE), Station Location: (GEO Latitude 43.1, Longitude 257.4), THEMIS EPO/UCLA Network

Cambridge Bay (CBB) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Cambridge Bay, NU, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (CBB), Station Location: (GEO Latitude 69.1, Longitude 255.0), NRCan Network

PSP FIELDS Fluxgate Magnetometer (MAG) Magnetic Field Vectors, Spacecraft, SC, Coordinates, Full Resolution, 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

Kiana (KIAN) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Kiana, AK, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (KIAN), Station Location: (GEO Latitude 67.0, Longitude 199.6), THEMIS EPO/UCLA Network

ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, Coordinates, Preliminary Values, Key Parameter (K1), 16 s Data

This Data Product contains Measurements from the ACE Magnetic Field Instrument (MAG). The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. MAG References: http://www.srl.caltech.edu/ACE/. ACE Browse Data is designed for monitoring large-scale Particle and Field Behavior and for selecting interesting Time Periods. The Data are automatically generated from the Spacecraft Data Stream using simple Algorithms provided by the Instrument Teams. The Data are not routinely checked for Accuracy and is subject to Revision. Use this Data at your own Risk, and consult with the appropriate Instrument Teams about citing it. The Magnetometer Browse Data is not validated by the Experimenters and should not be used except for preliminary Examination prior to detailed Studies.

MMS 1 Electron Drift Instrument (EDI) Electric Field, Level 2 (L2), Burst Mode, 0.9765625 ms Data

Baker Lake (BLC) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Baker Lake, NT, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (BLC), Station Location: (GEO Latitude 64.3, Longitude 264.0), NRCan Network

Americus (AMER) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Americus, KS, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (AMER), Station Location: (GEO Latitude 38.5, Longitude 263.7), McMAC Network

Parker Solar Probe, FIELDS Radio Frequency Spectrometer, RFS, Low Frequency Receiver, LFR, Spectra, Level 2 (L2), 7 s and 56 s Data

PSP FIELDS Radio Frequency Spectrometer, RFS, Low Frequency Reciever, LFR, Data:The RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1]. For a full description of the FIELDS experiment, see reference [2]. For a description of the RFS, see reference [3].The RFS produces auto and cross spectral data products in two frequency ranges, the Low Frequency Reciever range and the High Frequency Receiver range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR high-resolution spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the Polyphase Filter Bank, PFB, and the Fast Fourier Transform, FFT, spectral processing as described in reference [3]. Corrections for base capacitance and antenna effective length have not been applied. These corrections will be applied in Level 3 RFS data. Therefore, the units for all spectral quantities are given in V^2/Hz.The time resolution of the RFS data vary with instrument mode. During encounter, which is when PSP is within 0.25 astronomical units, AU, of the Sun, the cadence for RFS HFR and LFR spectra is typically about 7 s. During cruise mode, which is the default mode for operations outside of 0.25 AU, the cadence for HFR and LFR spectra is about 56 s.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D., et al., Space Sci Rev (2016), 204:7, DOI:10.1007/s11214-015-0211-6* 2) Bale, S.D., Goetz, K., Harvey, P.R., et al., Space Sci Rev (2016), 204:49, DOI:10.1007/s11214-016-0244-5* 3) Pulupa, M., Bale, S.D., Bonnell, J.W., et al., JGR Space Physics (2017), 122, 2836-2854, DOI:10.1002/2016JA023345

Parker Solar Probe, FIELDS Radio Frequency Spectrometer, RFS, High Frequency Receiver, HFR, Spectra, Level 2 (L2), 7 s and 56 s Data

PSP FIELDS Radio Frequency Spectrometer, RFS, High Frequency Receiver, HFR, Data:The RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1]. For a full description of the FIELDS experiment, see reference [2]. For a description of the RFS, see reference [3].The RFS produces auto and cross spectral data products in two frequency ranges, the Low Frequency Reciever range and the High Frequency Receiver range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR high-resolution spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.The Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the Polyphase Filter Bank, PFB, and the Fast Fourier Transform, FFT, spectral processing as described in reference [3]. Corrections for base capacitance and antenna effective length have not been applied. These corrections will be applied in Level 3 RFS data. Therefore, the units for all spectral quantities are given in V^2/Hz.The time resolution of the RFS data vary with instrument mode. During encounter, which is when PSP is within 0.25 astronomical units, AU, of the Sun, the cadence for RFS HFR and LFR spectra is typically about 7 s. During cruise mode, which is the default mode for operations outside of 0.25 AU, the cadence for HFR and LFR spectra is about 56 s.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D., et al., Space Sci Rev (2016), 204:7, DOI:10.1007/s11214-015-0211-6* 2) Bale, S.D., Goetz, K., Harvey, P.R., et al., Space Sci Rev (2016), 204:49, DOI:10.1007/s11214-016-0244-5* 3) Pulupa, M., Bale, S.D., Bonnell, J.W., et al., JGR Space Physics (2017), 122, 2836-2854, DOI:10.1002/2016JA023345

ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSM, Coordinates, Level 2 (H3), 1 s Data

STEREO-A In-Situ Measurements of Particles and CME Transients (IMPACT) Fluxgate Magnetometer (MAG) Burst Mode, Magnetic Field Vector, Spacecraft (SC) 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 Spacecraft, SC, coordinates.

MMS 3 Search Coil Magnetometer (SCM) AC Magnetic Field Level 2 (L2), High Speed Burst Mode, 16384 Sample/s Data

Search Coil Magnetometer (SCM) AC Magnetic Field (16384 samples/s), Level 2, High Speed Burst Mode Data. The tri-axial Search-Coil Magnetometer with its associated preamplifier measures three-dimensional magnetic field fluctuations. The analog magnetic waveforms measured by the SCM are digitized and processed inside the Digital Signal Processor (DSP), collected and stored by the Central Instrument Data Processor (CIDP) via the Fields Central Electronics Box (CEB). Prior to launch, all SCM Flight models were calibrated by LPP team members at the National Magnetic Observatory, Chambon-la-Foret (Orleans). Once per orbit, each SCM transfer function is checked thanks to the onboard calibration signal provided by the DSP. The SCM is operated for the entire MMS orbit in survey mode. Within scientific Regions Of Interest (ROI), burst mode data are also acquired as well as high speed burst mode data. This SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in the GSE frame. The SCM instrument paper for SCM can be found at http://link.springer.com/article/10.1007/s11214-014-0096-9 and the SCM data product guide at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.