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College (CIGO) Ground-based Vector Magnetic Field (L2) 0.5 s Data

College (College International Geophysical Observatory), AK, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (CIGO), Station Location: (GEO Latitude 64.9, Longitude 212.1), University of Alaska Network

MMS 3 Digital Signal Processor (DSP) Double Probe (ADP, SDP), Electric Field Power Spectral Density, Level 2 (L2), Slow Mode, 16 s Data

The MMS electric field power spectral density (EPSD) is computed onboard by the Digital Signal Processor (DSP). The fast Fourier transform (FFT) calculation is performed on a digitized version of analog signals from the Axial Double Probe (ADP) and Spin-Plane Double Probe (SDP). This data product is computed in space from individual components that are not synchronized to the 1 second pulse. Therefore, the timing between channels can be inaccurate by a fraction of a second. The samples times are interval start times taken from the x component. The spectra are calculated via a 1024-point FFT algorithm on piecewise continuous sets of waveform data. Nine signals can be processed simultaneously. Six of the twelve DC-coupled E, DC-coupled V, or SCM signals (16384 samples/s) are selected for spectral processing at 100% duty cycle. In addition, the three AC-coupled signals (262,144 kS/s) each can be processed at 6.25% duty cycle. Each of the nine signals has 16, 1024-point FFT operations every second; the field-programmable gate array (FPGA) performs 144 FFTs per second. The FFT is performed by an arithmetic logic unit (ALU), which is controlled by a state machine. Both are hard-coded into the FPGA. The operation starts by applying a 1024-point Hanning window onto a waveform. Next, an FFT is implemented. The FFT is broken into a series of "butterfly" operations performed by the ALU. The result has real and imaginary data. Power spectra are calculated by taking the sum of squares of real and imaginary values (the ALU includes a multiplier), which produces a power spectrum with 512 frequency bins. The frequency bins are then combined to give pseudo-logarithmic frequency spacing (del f)/f. The spectra are reduced to 56 frequency bins with (del f)/f between 6% and 12% when possible. Narrow-band emissions can be fit to an accuracy of (del f)/f ~3%, allowing for an accurate determination of plasma density. The spectra can be averaged in time. The fastest reporting rate of any signal is 16 spectra per second. Reporting rates can be as slow a one spectra every 16 s (averaging 256 spectra). The averaging process has 48-bit accuracy to maximize the dynamic range. The amplitudes undergo a pseudo-logarithmic compression to an 8-bit number representing over 120 dB of dynamic range at ~5% precision.

San Juan (SJG) Ground-based Vector Magnetic Field (L2) 1.0 s Data

San Juan (Cayey), PR, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (SJG), Station Location: (GEO Latitude 18.1, Longitude 293.8), USGS Network

MMS 4 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Level 2 (L2), Fast Mode, 2 s Data

The MMS magnetic field power spectral density (BPSD) is computed onboard by the Digital Signal Processor (DSP). The fast Fourier transform (FFT) calculation is performed on a digitized version of analog signals from the Search Coil Magnetometer (SCM) in the SCM123 coordinate system, see SCM data product guide for details, https://lasp.colorado.edu/mms/sdc/public/datasets/fields/. This data product is computed in space from individual components that are not synchronized to the 1 second pulse. Therefore, the timing between channels can be inaccurate by a fraction of a second. The samples times are interval start times taken from the x component. The spectra are calculated via a 1024-point FFT algorithm on piecewise continuous sets of waveform data. Nine signals can be processed simultaneously. Six of the twelve DC-coupled E, DC-coupled V, or SCM signals (16384 samples/s) are selected for spectral processing at 100% duty cycle. In addition, the three AC-coupled signals (262,144 kS/s) each can be processed at 6.25% duty cycle. Each of the nine signals has 16, 1024-point FFT operations every second; the field-programmable gate array (FPGA) performs 144 FFTs per second. The FFT is performed by an arithmetic logic unit (ALU), which is controlled by a state machine. Both are hard-coded into the FPGA. The operation starts by applying a 1024-point Hanning window onto a waveform. Next, an FFT is implemented. The FFT is broken into a series of "butterfly" operations performed by the ALU. The result has real and imaginary data. Power spectra are calculated by taking the sum of squares of real and imaginary values (the ALU includes a multiplier), which produces a power spectrum with 512 frequency bins. The frequency bins are then combined to give pseudo-logarithmic frequency spacing (del f)/f. The spectra are reduced to 88 frequency bins with (del f)/f between 6% and 12% when possible. Narrow-band emissions can be fit to an accuracy of (del f)/f ~3%, allowing for an accurate determination of plasma density. The spectra can be averaged in time. The fastest reporting rate of any signal is 16 spectra per second. Reporting rates can be as slow a one spectra every 16 s (averaging 256 spectra). The DSP and SCM instrument papers can be found at https://link.springer.com/article/10.1007/s11214-014-0115-x and https://link.springer.com/article/10.1007/s11214-014-0096-9, respectively. The DSP and SCM data product guides can be found at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.

Solund (SOL) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Solund, Norway, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (SOL), Station Location: (GEO Latitude 61.1, Longitude 4.8), TGO Network

Fresno (FRN) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Fresno, CA, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (FRN), Station Location: (GEO Latitude 37.1, Longitude 240.3), USGS Network

Mekrijarvi (MEK) Ground-based Vector Magnetic Field (L2) 10.0 s Data

Mekrijarvi, Finland, Ground-based Vector Magnetic Field Level 2 Data, 10.0 s Time Resolution, Station Code: (MEK), Station Location: (GEO Latitude 62.8, Longitude 31.0), IMAGE Network

THEMIS-E: On Board spin fits (FIT) of Electric (EFI) and Magnetic (FGM) field. On-Board Spin-fit electric and magnetic field data

THEMIS-E: On Board spin fits of Electric (EFI) and Magnetic (FGM) fields. This file contains data EFI and FGM that has been despun on-board to 3 second resolution. It stores meta information like the number of points that contributed to each spin and the standard deviation of those points. For the EFI data it also stores variables with the Z component of the EFI data zeroed and the Z component of the EFI estimated using the E.B=0 equality. The need to use an estimated Z axis for the EFI is due to error in measurements from the EFI axial booms. These data are provided in DSL (despun spacecraft L-Z vector), GSM, and GSE coordinates.

Anchorage (HLMS) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Anchorage (High-Latitude Monitoring Station), AK, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (HLMS), Station Location: (GEO Latitude 61.2, Longitude 210.1), University of Alaska Network

Toolik Lake (TOOL) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Toolik Lake, AK, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (TOOL), Station Location: (GEO Latitude 66.6, Longitude 210.4), GIMA Network

Nurmijarvi (NUR) Ground-based Vector Magnetic Field (L2) 10.0 s Data

Nurmijarvi, Finland, Ground-based Vector Magnetic Field Level 2 Data, 10.0 s Time Resolution, Station Code: (NUR), Station Location: (GEO Latitude 60.5, Longitude 24.7), IMAGE Network

FIELD EXP E SIRIS RESAMP REDUCED DATA RECORD SPECTRUM V1.0

The SIRIS measurement objectives were: 1) to measure reflectance spectra of a bright and dark target at each GRSFE site for potential use in AVIRIS calibration characterize selected sites at the GRSFE modeling site (Lunar Lake, NV) using visible/infrared reflectance reflectance spectra for selected endmember materials at each of the GRSFE sites inter-instrument calibration.

THEMIS-D: On Board spin fits (FIT) of Electric (EFI) and Magnetic (FGM) field. On-Board Spin-fit electric and magnetic field data

THEMIS-D: On Board spin fits of Electric (EFI) and Magnetic (FGM) fields. This file contains data EFI and FGM that has been despun on-board to 3 second resolution. It stores meta information like the number of points that contributed to each spin and the standard deviation of those points. For the EFI data it also stores variables with the Z component of the EFI data zeroed and the Z component of the EFI estimated using the E.B=0 equality. The need to use an estimated Z axis for the EFI is due to error in measurements from the EFI axial booms. These data are provided in DSL (despun spacecraft L-Z vector), GSM, and GSE coordinates.

Narsarsuaq (NRSQ/NAQ) Ground-based Vector Magnetic Field (L2) 20.0 s Data

Narsarsuaq, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 20.0 s Time Resolution, Station Code: (NRSQ/NAQ), Station Location: (GEO Latitude 61.2, Longitude 314.6), DTU Network

Danmarkshavn (DMH) Ground-based Vector Magnetic Field (L2) 20.0 s Data

Danmarkshavn, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 20.0 s Time Resolution, Station Code: (DMH), Station Location: (GEO Latitude 76.8, Longitude 341.4), DTU Network

Narsarsuaq (NRSQ/NAQ) Ground-based Vector Magnetic Field (L2) 1.0 min Data

Narsarsuaq, Greenland, Ground-based Vector Magnetic Field Level 2 Data, 1.0 min Time Resolution, Station Code: (NRSQ/NAQ), Station Location: (GEO Latitude 61.2, Longitude 314.6), DTU Network

STEREO-B In-situ Measurements of Particles And CME Transients (IMPACT) Magnetic Field Vectors and Ancillary Data

This data product contains Level 1 0.125-s values of solar wind magnetic field data taken by the IMPACT/Magnetometer on STEREO-B. The interface at UCB provides access to CDF-formatted files of magnetic field data in RTN coordinates. The interface at UCLA allows selection of STEREO A or STEREO B data and of vector quantities in RTN or spacecraft coordinates. It also allows selection of either of two parameter sets: [Bx, By, Bz, B ] or [RBx, RBy, RBz, B , cone and clock angles]. Further, this interface enables easy migration between plot vs. ASCII data presentation options and among the three available resolutions (1, 8, 32 Hz). The parameter level information given below is specific to the CDF version of the data at UCB.

Laurel (LREL) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Laurel, MD, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (LREL), Station Location: (GEO Latitude 39.1, Longitude 283.2), THEMIS GBO Network

Voyager 2 48-s Triaxial Fluxgate Magnetometer (MAG) Magnetic Field Data Near and Beyond Termination Shock in CDF Format

The main science objectives for the Voyager Interplanetary Mission, VIM, are as follows: - investigate the structure of the solar wind magnetic fields and plasma in the inner and outer heliosphere; - conduct long term study of heliospheric evolution during different phases of the 22-year solar magnetic cycle and the 11-year solar activity cycle; - study the long term solar modulation and determine the elemental and isotopic abundances of galactic cosmic ray particles in the heliosphere; - measure radial gradients, spectra, and nuclear abundances of the anomalous component of cosmic rays from acceleration at the solar wind termination shock; - investigate local particle acceleration in the interplanetary medium from solar flare shocks and corotating interaction regions; - study propagation of solar energetic particles in the heliosphere. The average magnetic field strength produced by the spacecraft at the location of the outboard magnetometer of the dual magnetometers system on Voyager 1 and Voyager 2 is about 0.1-0.2 nT, comparable to the most probable magnetic field strength in the inner heliosheath and significantly larger than the most probable magnetic field strength in the distant supersonic solar wind. The spacecraft magnetic field is a complex, time-dependent signal that must be removed from the measured magnetic field signal in order to derive the ambient magnetic fields of the solar wind and heliosheath. Corrections must also be made for spurious magnetic signals and noise associated with the telemetry system, ground tracking systems, and other factors. Extracting the signal describing the solar wind and heliosheath from the many sources of uncertainty is a complex and partly subjective process that requires understanding of the instrument and judgement based on experience in dealing with the ever-changing extraneous signals. We estimate that for the Voyager magnetic field data the 1-sigma the uncertainty of the 48-s averages for each of the components of the magnetic field BR, BT, and BN is typically +/- 0.02 nT; the uncertainty in magnitude F1 is typically +/- 0.03 nT. F1, BR, BT, and BN can differ from one another and they may vary with time, but there is no practical way to determine these uncertainties more precisely at present. References: D.B. Berdichevsky, Voyager Mission, Detailed processing of weak magnetic fields; I - Constraints to the uncertainties of the calibrated magnetic field signal in the Voyager missions, 2009; https://vgrmag.gsfc.nasa.gov/Berdichevsky-VOY_sensor_opu090518.pdf Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., Spacecraft studies of the interplanetary magnetic field, 76, 3564, 1971.

Snap Lake (SNAP) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Snap Lake, NT, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (SNAP), Station Location: (GEO Latitude 63.6, Longitude 249.1), THEMIS GBO/UCLA Network