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CASSINI SCALAR MAGNETOMETER CALIB DATA V1.0

This data set contains magnetic-field data acquired during the cruise and tour phases of the Cassini mission to Saturn. Data collection began on 16 August (day 228), 1999. On this date, two days before the spacecraft commenced Earth swingby, the magnetometer boom was unfurled into its extended position; a configuration it maintained for the remainder of the mission. This dataset contains the data collected from the helium magnetometer while in scalar mode (SHM). The SHM mode is used only when high fields are expected, this means that SHM data is only collected infrequently and ceased being collected after 17 November (day 321), 2005 due to an instrument failure.

VOYAGER 2 JUPITER MAGNETOMETER RESAMPLED DATA 9.60 SEC

This data set includes Voyager 2 Jupiter encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979A Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

MGS SAMPLER MAGNETOMETER/ELECTRON REFLECTOMETER DATA

MAG/ER data included on this volume consist of a suite of GIF files thatare plots of derived electron and magnetic field observations acquired during the assessment orbits [see: Acuna et al., 1998]. The plots include electron fluxes at 10, 50, 130, 300, and 1000 eV, a color spectrogram of the same data, and magnetic field amplitude and rms, and spacecraft altitude. The numerical data will be released later on MAG/ER archive volumes, after further validation and calibration procedures have been applied.

Pioneer 10 Helium Vector Magnetometer (MAG), Magnetic Field in RTN Coordinates and One Way Light Time Delays, Cruise Phase

This Data Set from the Pioneer 10 Helium Vector Magnetometer, HVM, consists of 1 min Averages of Vector Components and Scalar Magnitudes of the Interplanetary Magnetic Field. The three Components, Br, Bt, Bn, are given in Radial-Tangential-Normal, RTN, Coordinates and all Magnetic Fields are expressed in nT. The Scalar Magnitudes, B, are Averages of higher-resolution Scalar Magnitudes. The Time Tag for each 1 min Interval is the Midpoint of the averaging Interval in Spacecraft Event Time-UT, SCET-UT. The Averages were originally calculated over 1 min Intervals in Ground Received Time, and the Midpoints have been converted to SCET-UT. The File P10_LIGHTTIME contains Daily Values for the one way Light Time Delay. No records are written for Data Gaps. Most Files cover from 28 up to 35 Days, but there are a Number of shorter Files, particularly at Year Boundaries. Data for the Jupiter Encounter, Days 329 through 349 of 1973, are not included. The RTN System is fixed to the Sun-Spacecraft Line and aligned with the Solar Heliographic Equator. The R Axis is the Radial Direction to the Spacecraft, the T Axis is the Cross Product of the Solar Rotation Axis and the R Axis, and N is the Cross Product of the R and T Axes. The File P10HVM_15M.SFD provides a detailed Description of the Pioneer Spacecraft, the HVM Experiment, and the Data. This ASCII Document is written in Standard Formatted Data Unit, SFDU, Format as Part of NSSDC Data Set 72-012A-01I for 15 min. Averaged Data covering 1972-03-03 to 1975-11-17. Data Set Files: P10HVMMN_FMT.txt, this Document, ASCII; P10HVM_15M.SFD, SFDU Metadata Extract from Pioneer 10 HVM 15 min Data Set; Myyddd.asc, 1 min Data Files from Pioneer 10 HVM starting at Date yyddd; and P10_LIGHTTIME.asc, Data File with One Way Light Time Delays, ASCII. Related Information and Data: Further Details on the Spacecraft, Experiment, Data Sets at NSSDC, and related WWW Sites can be found on the Pioneer 10/Pioneer 11 Flight Project Page under https://nssdc.gsfc.nasa.gov/space/. Pioneer 10 and Pioneer 11 Hourly of the Interplanetary Solar Wind Data Averages and Heliocentric Coordinates and other Interplanetary Spacecraft may be also be accessed and plotted Online through the COHOWeb Service, https://cohoweb.gsfc.nasa.gov/coho/. Pioneer Data on the NASA Data Archive and Distribution Service, NDADS, may be located on the WWW via the SPyCAT Service at the first URL listed above or by an E-Mail Message to the Automated Retrieval Mail System, ARMS, at archives@ndadsa.gsfc.nasa.gov with $apos;HOLDINGS$apos; on the Subject Line. Data Set Coverage, yyyy-mm-dd: 1972-03-03 to 1975-11-17, Data Set Contact: Joyce Wolf, NASA JPL.

ISEE 3 Vector Helium Magnetometer (MAG), Magnetic Field, 1 min CDF Data

This Data Set contains averaged 1 min magnetic field data converted from simple ASCII records. It was created at the NSSDC from a more complex, multi-resolution data set with the current NSSDC ID of SPHE-00673 and old NSSDC ID of 78-079A-02D, provided by the Principal Investigator Team and now available from ftps://spdf.gsfc.nasa.gov/pub/data/isee/isee3/magnetic_fields/1min_ascii_extracted/. The Coordinate System for the magnetic field components is the JPL-defined I,S Coordinate System set at the origin at the spacecraft: I is the unit vector in the direction of the ISEE 3 spin axis, positive in the northward direction, and S is the unit vector from the spacecraft to the sun. The Z-Axis is parallel to I, the Y-Axis is parallel to the cross product I ⨯ S, and the X-Axis is parallel to Y ⨯ Z. The I,S coordinate system is approximately the same as the Solar Ecliptic, SE, System since the Spacecraft Z-Axis, the Spin Axis, is maintained within 0.5° of perpendicular to the Ecliptic Plane. The SE coordinate system is defined in the same way as GSE, but with the spacecraft point of observation substituted for the position of the earth. For years 1984 through 1990 the spacecraft position in HGI coordinates was added to the data product. The HGI coordinate system is sun-centered and inertially fixed with respect to an X-Axis directed along the intersection line of the Ecliptic and Solar Equatorial planes, which defines the 0° longitude direction. The Solar Equatorial plane is inclined at 7.25° from the Ecliptic. This direction was towards an Ecliptic longitude equal to 74.367° on January 1, 1900 at 12:00 UT, but because of the precession of the earth's equator, this longitude increases by 1.4° per century. The Z-Axis is directed perpendicular to and northward of the solar equator and the Y-Axis completes the right-handed Set. The HGI longitude increase from 0° in the X-Direction towards the positive Y-Direction. The HGI latitude increases to +90° at the north pole and decreases to -90° at the south pole. Note that the values listed are 1 min averages, so that B ^2 may not equal B^2 .

STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Fluxgate Magnetometer (MAG) Magnetic Field Vectors, in Spacecraft (SC) Coordinates

STEREO Behind In-situ Measurements of Particles and CME Transients, IMPACT, Magnetometer Instrument, MAG, Magnetic Field Vectors, Level 1 Data

IMP-8 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates

IMP-8 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution Tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. 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 References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

Helios 1 E3 Magnetometer (Ness et al.) 6-sec Data

Task of the HELIOS mission was the exploration of the inner heliosphere, inside the Earth's orbit to 0.3 AU. The Rome-GSFC magnetic field experiment has been a joint venture of an italian group (University of Rome and CNR/Istituto Fisica Spazio Interplanetario, Frascati) and an american group of NASA/Goddard Space Fligth Center, under the responsibility of F. Mariani and N.F.Ness, respectively. A description of the experiment can be found in the NASA-GSFC report X-692-75-112 (1975), by C. Scearce et al. The instrument is a dual configuration of two tri-axial fluxgate magnetometers operating at four different sensitivities (from 0.84 to 0.03 nT). The time resolution, depending the operation mode, telemetry format, and bit rate, for most cases varied from 0.07 to 1.5 seconds. The present data set contains six-second averages of the magnetic field elements in solar-ecliptic (SE) spacecraft-centered coordinates. Data are stored in files on a daily basis. File names are hNYYDDD.asc, with N the Helios number (1 or 2), YY the year (last two digits), and DDD the day of year (1 = January 1st). For instance, h276105.asc is the file with Helios 2 data for day 105, 1976.

VEGA1 CRUISE MAGNETOMETER DATA

On Dec 15, 1984, the Vega spacecraft was launched to first flyby Venus at which time landers were released and then continue to a flyby of Halley. The magnetic field experiments MISCHA carried four fluxgate sensors, with three sensors mounted on a boom at the end of the solar panels and the fourth sensor mounted one meter closer. During the cruise phase, the TRASSA-1 mode of the instrument (1 vector/2.5 min) was used. The sensors were switched to the TRASSA-2 mode (1 vector/min) during the flyby which started roughly two days before the encounter. From 3 h before closest approach (CA) until 1 hour after CA, the HS-mode 1 vector/6s) and the DT-mode (1 vector/100ms) was used [DELVAETAL1991].

STEREO-A In-Situ Measurements of Particles and CME Transients from the Magnetometer and the Plasma and Suprathermal Ion and Composition Instruments (IMPACT/MAG, PLASTIC) Solar Wind Plasma Data

STEREO-A In-situ Measurements of Particles and CME Transients, IMPACT, Magnetometer Instrument, MAG, Magnetic Field Vector and PLAsma and SupraThermal Ion Composition, PLASTIC, Solar Wind Parameter, Level 2, Data

GALILEO MAGNETOMETER CRUISE EDR DATA

This data set contains data acquired by the Galileo Magnetometer during the Interplanetary Cruise to Jupiter. The data are at varying resolution depending on the averaging constant applied to the instrument. The EDR files are given in IBM 370 binary representation and are stored in an extremely compact format.

ISEE 1 magnetometer 1-min data

This data set contains magnetic field component and magnitude averages every minute, with components given in spacecraft, GSE and GSM coordinates. Standard deviations in the averages are given, as are differences between the averages and model field vectors. Geocentric (GSE and GSM) spacecraft position information is given, as is ISEE1-ISEE2 separation vector information. ISEE 1 spin vector direction and ISEE 1 velocity vector information, relative to the Earth and to ISEE 2, are given. Miscellaneous other parameters are also given. Data are accessible as plots, lists and files from CDAWeb, and as CDF files from CDAWeb's ftp area.

MMS 4 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Level 2 (L2), Slow Mode, 16 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 (scm1 = - x sensor; scm2 = -z sensor; scm3 = -y sensor). 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 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.

MMS 1 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Level 2 (L2), Slow Mode, 16 s Data

THEMIS-B: Probe Electric Field Instrument and Search Coil Magnetometer Instrument, Digital Fields Board - digitally computed Filter Bank spectra and E12 peak and average in HF band (FBK).

The Filter Bank is part of the Digital fields board and provides band-pass filtering for EFI and SCM spectra as well as E12HF peak and average value calculations. The Filter Bank provides band-pass filtering for less computationally and power intensive spectra than the FFT would provide. The process is as follows: Signals are fed to the Filter Bank via a low-pass FIR filter with a cut-off frequency half that of the original signal maximum. The output is passed to the band-pass filters, is differenced from the original signal, then absolute value of the data is taken and averaged. The output from the low-pass filter is also sent to a second FIR filter with 2:1 decimation. This output is then fed back through the system. The process runs through 12 cascades for input at 8,192 samples/s and 13 for input at 16,384 samples/sec (EAC input only), reducing the signal and computing power by a factor 2 at each cascade. At each cascade a set of data is produced at a sampling frequency of 2^n from 2 Hz to the initial sampling frequency (frequency characteristics for each step are shown below in Table 1). The average from the Filter Bank is compressed to 8 bits with a pseudo-logarithmic encoder. The data is stored in sets of six frequency bins at 2.689 kHz, 572 Hz, 144.2 Hz, 36.2 Hz, 9.05 Hz, and 2.26 Hz. The average of the coupled E12HF signal and it's peak value are recorded over 62.5 ms windows (i.e. a 16 Hz sampling rate). Accumulation of values from signal 31.25 ms windows is performed externally. The analog signals fed into the FBK are E12DC and SCM1. Sensor and electronics design provided by UCB (J. W. Bonnell, F. S. Mozer), Digital Fields Board provided by LASP (R. Ergun), Search coil data provided by CETP (A. Roux). Table 1: Frequency Properties. Cascade Frequency content of Input Signal Low-pass Filter Cutoff Frequency Freuency Content of Low-pass Output Signal Filter Bank Frequency Band 0* 0 - 8 kHz 4 kHz 0 - 4 kHz 4 - 8 kHz 1 0 - 4 kHz 2 kHz 0 - 2 kHz 2 - 4 kHz 2 0 - 2 kHz 1 kHz 0 - 1 kHz 1 - 2 kHz 3 0 - 1 kHz 512 Hz 0 - 512 Hz 512 Hz - 1 kHz 4 0 - 512 Hz 256 Hz 0 - 256 Hz 256 - 512 Hz 5 0 - 256 Hz 128 Hz 0 - 128 Hz 128 - 256 Hz 6 0 - 128 Hz 64 Hz 0 - 64 Hz 64 - 128 Hz 7 0 - 64 Hz 32 Hz 0 - 32 Hz 32 - 64 Hz 8 0 - 32 Hz 16 Hz 0 - 16 Hz 16 - 32 Hz 9 0 - 16 Hz 8 Hz 0 - 8 Hz 8 - 16 Hz 10 0 - 8 Hz 4 Hz 0 - 4 Hz 4 - 8 Hz 11 0 - 4 Hz 2 Hz 0 - 2 Hz 2 - 4 Hz 12 0 - 2 Hz 1 Hz 0 - 1 Hz 1 - 2 Hz *Only available for 16,384 Hz sampling.

ISEE 2 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates

ISEE-2 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer 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.

VOYAGER 2 JUPITER MAGNETOMETER RESAMPLED DATA 1.92 SEC

This data set includes Voyager 2 Jupiter encounter magnetometer data that have been resampled at a 1.92 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979A Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

ACE Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates

ACE linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM 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.

MMS 3 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/.

ICE MAGNETOMETER DATA V1.0

These data were obtained from the JPL magnetometer experiment on ICE (Principal Investigator: E.J. Smith produces three, high-accuracy, triaxial measurements per second of the magnetic field strength in 8 ranges, i.e., +/-4 nT (lowest full range), 14, 42, 144, 640, 4000, 22000, and 140000 nT (highest full range) and a sensitivity of 1/256 of each full range, in a 0-3 Hz pass band. During the G-Z encounter the instrument range was switched automatically between the 4 lowest ranges depending on the field intensity, giving sensitivities of 0.015, 0.051, 0.17 and 0.57 nT respectively. The time resolution is 1/3 sec from the start of Day 253 (September 10, 1985) until Day 255 (September 12, 1985), 18:38. At that time the bit rate dropped from 1024 to 512 bps, and the time resolution decreased to 2/3 sec.