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Petersburg (PTRS) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Petersburg, AK, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (PTRS), Station Location: (GEO Latitude 56.8, Longitude 226.8), THEMIS EPO/UCLA Network

OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 1 min Data

Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 1 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005

Inuvik (INUV) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Inuvik, NT, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (INUV), Station Location: (GEO Latitude 68.4, Longitude 226.2), Athabasca University Network

Parker Solar Probe (PSP) Merged Magnetic Field, Plasma, and Ephemeris, Hourly Data

The SPDF Coordinated Heliospheric Observations Web, COHOWeb, hourly and daily Parker Solar Probe, PSP, data were made by using high resolution data from from CDAWeb.The PSP COHO file include data derived from the PSP FIELDS Fluxgate Magnetometer data as well as Densities, Vector Velocities, and Scalar Radial Component Temperatures of Solar Wind Protons measured by the PSP SWEAP Solar Probe Cup, SPC. The original PSP magnetic field data comes from the PSP_FLD_L2_MAG_RTN_1MIN data product while the original plasma data comes from the PSP_SWP_SPC_L3I data product by applying the following conditions:* Proton bulk velocity from 1-dimensional Maxwellian fitting, only good quality, in the inertial RTN frame* Total proton number density from 1-dimensional Maxwellian fitting, only good quality* Proton most probable thermal speed, radial component, from 1-dimensional maxwellian Fitting, only good qualityCitation: Papitashvili, N. E. (2020). Parker Solar Probe (PSP) Merged Magnetic Field, Plasma, and Ephemeris, Hourly Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/19ed-kz70

MMS 1 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/.

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

PSP FIELDS Digital Fields Board, DFB, SCMflfhg data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB 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

Priddis (ROTH) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Priddis, AB, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (ROTH), Station Location: (GEO Latitude 50.9, Longitude 245.7), Athabasca University Network

Chibougamau (CHBG) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Chibougamau, QC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (CHBG), Station Location: (GEO Latitude 49.8, Longitude 285.6), THEMIS GBO/UCLA Network

Wind Magnetic Field Investigation (MFI) 15-sec magnetic field data, solar wind only

Data consist of 15-sec averages of magnetic field magnitude and GSE Cartesian components, from the MFI magnetometer on Wind. Data are for only the solar wind phases of the Wind orbit.

Van Allen Probe B Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Waveform Receiver (WFR) Cross Spectral Matrix, Level 2 (L2), 6 s Data

Van Allen Probe B Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Waveform Receiver (WFR) Three-Axis Electric Field (EU, EV, EW) and Magnetic Field (BU, BV, BW) Cross Spectral Matrix, Six Diagonal and 15 Off-Diagonal Components, 10 kHz to 487 kHz, 82 Frequency Bins

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/.

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ICE PLASMA WAVE ELECTRIC FIELD MEASUREMENT DATA

The Plasma Wave Data were submitted to National Space Science Data Center after the Principal Investigator's death (Scarf) by S. Chang of TRW. For the electric field data, the time interval submitted was Sept 9 - 14, 1985 was included. That information, as well as an explanation of the reformatted data is detailed.

ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, Coordinates, Preliminary Values, Key Parameter (K0), 5 min 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.

Akulivik (AKUL) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Akulivik, QC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (AKUL), Station Location: (GEO Latitude 60.8, Longitude 281.9), AUTUMNX Network

Ukiah (UKIA) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Ukiah, OR, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (UKIA), Station Location: (GEO Latitude 45.1, Longitude 241.1), THEMIS EPO/UCLA Network

MESSENGER Magnetometer (MAG) Interplanetary Magnetic Field, Radial-Tangential-Normal, RTN, Coordinates, High Resolution, 1 s Data

This MESSENGER Magnetic field data set contains cruise-phase magnetic field vectors in RTN coordinates at time resolutions typically of 0.5 s or 1.0 s and sometimes as fine as 0.05 s. The Mercury Surface, Space Environment, Geochemistry, and Ranging, MESSENGER, mission is designed to study the characteristics and environment of Mercury from orbit. The nominal orbit is planned to have a periapsis of 200 km at 60° N latitude, an apoapsis of 15,193 km, a period of 12 hours, and an inclination of 80°. The periapsis will slowly rise due to solar perturbations to over 400 km at the end of 88 days, one Mercury year, at which point it will be readjusted to a 200 km, 12 hour orbit via a two burn sequence. Data will be collected from orbit for one Earth year, the nominal primary mission was planned to end in March 2012. Specifically, the scientific objectives of the mission are to characterize: * the chemical composition of the surface of Mercury * the geologic history * the nature of the magnetic field * the size and state of the core * the volatile inventory at the poles * the nature of the Hermean exosphere and magnetosphere The MESSENGER mission should also yield: * global composition maps * a 3-D model of the magnetosphere of Mercury * topographic profiles of the northern hemisphere * gravity field to degree and order sixteen * altitude profiles of elemental species * a characterization of the volatiles in permanently shadowed craters at the poles The MESSENGER spacecraft is a squat box (1.27 m ⨯ 1.42 m ⨯ 1.85 m) with a semi-cylindrical thermal shade, roughly 2.5 m tall and 2 m wide, for protection from the Sun and two solar panel wings extending radially about 6 m from tip to tip. Five science instruments are mounted externally on the bottom deck of the main body: the Mercury Dual Imaging System, MDIS, Gamma-Ray and Neutron Spectrometer, GRNS, X-ray Spectrometer, XRS, Mercury Laser Altimeter, MLA, and Atmospheric and Surface Composition Spectrometer, MASCS. Radio Science, RS, experiments will use the existing communications system. The Energetic Particle and Plasma Spectrometer, EPPS, is mounted on the side and top deck, and the magnetometer, MAG, is at the end of the 3.6 m boom. The Messenger MAG instrument is a miniature three-axis ring-core fluxgate magnetometer with low-noise electronics. It is mounted on a 3.6 m boom in the anti-sunward direction. The MAG has ±1530 and ±51300 nT ranges with 20-bit internal resolution and 17-bit output resolution. The MAG probe samples magnetic field values along the X, Y, and Z axes at a rate of up to 20 samples/s. The rate is commandable and can vary. This data set has 3-axis calibrated samples of the magnetic field in heliospheric RTN coordinates, Br, Bt, Bn, in units of nT. The spacecraft position data in these files are identified by radial distance from the Sun, latitude above the ecliptic plane, and azimuth with respect to the Earth-Sun line in the ecliptic plane. The MESSENGER Magnetometer data are also available from the Planetary Data System, Planetary Plasma Interactions, PDS/PPI, node via the URL; https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MESS-E_V_H_SW-MAG-3-CDR-CALIBRATED-V1.0/DATA/RTN/. Hovever, the data are listed in plain text, space delimeted ASCII tables. Note that this SPASE Numerical Description only describes the MESSENGER Magnetometer data stored in Common Data Files.

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Lidar Atmopheric Sensing Experiment (LASE) Data Obtained During the Southern Great Plains (SGP97) Field Experiment

The LASE Southern Great Plains (SGP97) field experiment was conducted in Oklahoma during June-July 1997. SGP97 was a NASA EOS Interdisciplinary Science Investigation to validate soil moisture retrieval algorithms at satellite temporal and spatial scales using remote sensing moisture measurements from aircraft and in situ soil measurements. One of the major objectives of SGP97 was the study of the impact of soil moisture on the atmospheric boundary layer (ABL) development. To aid convective boundary layer (CBL) studies, LASE was deployed on the NASA P-3B aircraft along with other instruments. LASE (Lidar Atmospheric Sensing Experiment) airborne lidar produces measurements of aerosols and water vapor vertical profiles from the aircraft altitude (6-8 km) down to the surface. Such profiles show the vertical context in which the SGP97 in situ and radiometric measurements are made, thus supporting the vertical extension of the in situ measurements and detecting any unsampled layers or inhomogeneities, which would impact the surface and airborne measurements.

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ICE PLASMA WAVE MAGNETIC FIELD MEASUREMENT DATA V1.0

The Plasma Wave Data were submitted to National Space Science Data Center after the Principal Investigator's death (Scarf) by S. Chang of TRW. For the magnetic field data, the time interval submitted was Sept 9 - 14, 1985 was included. That information, as well as an explanation of the reformatted data is detailed.

MMS 4 Search Coil Magnetometer (SCM) AC Magnetic Field Level 2 (L2), Burst Mode, 8192 Sample/s Data

Search Coil Magnetometer (SCM) AC Magnetic Field (8192 samples/s), Level 2, 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/.

ACE Magnetic Field (MAG) Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSM, Coordinates, Level 2 (H2), 1 h Data