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PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Cross Spectra, v-component, w-component, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data

PSP FIELDS Digital Fields Board (DFB), SCMvlfhg ⨯ SCMwlfhg cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) 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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523

Ottawa (OTT) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Ottawa, ON, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (OTT), Station Location: (GEO Latitude 45.4, Longitude 284.4), NRCan Network

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MEX: MARSIS ELECTRON PLASMA DENSITY AND MAGNETIC FIELD DATA

This data set tabulates local electron densities and local magnetic field strengths magnetic field strengths obtained from Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) Active Ionospheric Sounding (AIS) mode ionograms. The electron density is obtained by measuring the increment in frequency between the plasma frequency harmonics, visible as bright vertical lines at low frequency and delay time in many MARSIS ionograms. Similarly, the local magnetic field strength is found by measuring the difference in delay time between electron cyclotron echoes, visible as bright horizontal lines at low frequency on many ionograms. Both the measured quantity and the derived result are included in the archive product. We also include a data quality flag giving the impression of the archivist as to how reliable each result is. This archive product includes only data from the nominal mission, which starts about orbit 1850 and ends on orbit 2539.

Ekati (EKAT) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Ekati, NT, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (EKAT), Station Location: (GEO Latitude 64.7, Longitude 249.3), THEMIS GBO/UCLA Network

Sanikiluaq (SNKQ) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Sanikiluaq, NU, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (SNKQ), Station Location: (GEO Latitude 56.5, Longitude 280.8), THEMIS GBO/Carisma Network

Schefferville (SCHF) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Schefferville, QC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (SCHF), Station Location: (GEO Latitude 54.8, Longitude 293.2), AUTUMNX Network

Fort Simpson (FSIM) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Fort Simpson, NT, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (FSIM), Station Location: (GEO Latitude 61.8, Longitude 238.8), THEMIS GBO/Carisma Network

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MEX: MARSIS ELECTRON PLASMA DENSITY AND MAGNETIC FIELD DATA

STEREO-B 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-B in Spacecraft, SC, coordinates.

Richardson (RICH) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Richardson, TX, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (RICH), Station Location: (GEO Latitude 33.0, Longitude 263.2), McMAC Network

PSP FIELDS Digital Fields Board (DFB) DC-coupled Searchcoil Magnetometer, SCM, Cross Spectra, d-component, e-component, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data

PSP FIELDS Digital Fields Board (DFB), SCMXlfhg ⨯ SCMXlfhg cross spectra 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 cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) 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 units for phase are degrees.The Level 2 voltage 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 cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [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]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB DC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB DC cross spectra is typically 30 NYseconds [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* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523

Goose Bay (GBAY) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Goose Bay, NL, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (GBAY), Station Location: (GEO Latitude 53.3, Longitude 299.5), THEMIS GBO/UCLA Network

MMS 2 Flux Gate Magnetometer (FGM) DC Magnetic Field, Level 2 (L2), Survey Mode, 8 or 16 Sample/s, v4/5 Data

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a traditional Analog Fluxgate Magnetometer (AFG) and a Digital Fluxgate magnetometer (DFG). The dual magnetometers are operated as a single instrument providing a single intercalibrated data product. Range changes occur at different times on the two instruments so the gains checked each periapsis can be carried out unambiguously to apoapsis. Cross correlation of calibration parameters can separate causes of the any apparent calibration changes. Use of Electron Drift Instrument (EDI) to determine the field along the rotation axis allows accurate monitoring of the zero levels along the rotation axis. Prior to launch the magnetometers were calibrated at the Technical University, Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were calibrated at UCLA. Both sets of sensors are operated for the entire MMS orbit, with slow survey (8 samples per second) outside of the Region of Interest (ROI), and fast survey (16 samples per second) inside the ROI. Within the ROI, burst mode data (128 samples per second) are also acquired. A detailed description of the MMS fluxgate magnetometers, including science objectives, instrument description, calibration, magnetic cleanliness program, and data flow can be found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 10.1007/s11214-014-0057-3). Additional information can also be found at http://www-spc.igpp.ucla.edu/ssc/mms (UCLA), and http://www.iwf.oeaw.ac.at/de/forschung/erdnaher-weltraum/mms/dfg (IWF, Graz). For the purpose of creating a unified FGM Level 2 data product, burst mode data is taken from DFG and survey mode data is taken from AFG. Because AFG and DFG are cross-calibrated on an orbit-averaged basis, small differences in offset may be observed between Level 2 burst and survey mode data. Consequently, any differences are within the error of the measurement. Based on preliminary analysis of the data, the absolute error within the Region of Interest (ROI) is estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the spin-axis and 0.2 nT in total magnitude.

Glyndon (GLYN) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Glyndon, MN, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (GLYN), Station Location: (GEO Latitude 46.9, Longitude 263.5), McMAC Network

Radisson (RADI) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Radisson, QC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (RADI), Station Location: (GEO Latitude 53.8, Longitude 282.4), AUTUMNX Network

Shawano (SWNO) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Shawano, WI, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (SWNO), Station Location: (GEO Latitude 44.8, Longitude 271.4), THEMIS EPO/UCLA Network

Meanook (MEA) Ground-based Vector Magnetic Field (L2) 1.0 s Data

Meanook, AB, Ground-based Vector Magnetic Field Level 2 Data, 1.0 s Time Resolution, Station Code: (MEA), Station Location: (GEO Latitude 54.6, Longitude 246.7), NRCan Network

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

PSP FIELDS Digital Fields Board, DFB, SCMwlfhg 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

Prince George (PGEO) Ground-based Vector Magnetic Field (L2) 0.5 s Data

Prince George, BC, Ground-based Vector Magnetic Field Level 2 Data, 0.5 s Time Resolution, Station Code: (PGEO), Station Location: (GEO Latitude 53.8, Longitude 237.2), THEMIS EPO/UCLA Network

PSP FIELDS Digital Fields Board (DFB) DC-coupled Single Ended Voltage Waveform, Monopole Mode, Level 2 (L2), PT0.027306S Data

PSP FIELDS Digital Fields Board, DFB, Single Ended Voltage 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].The DFB continuous waveform data consist of time series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3].The Level 2 data products contained in this data file have been calibrated for:* 1) DFB in-band gain* 2) DFB analog filter gain and phase response* 3) DFB digital filter phase response* 4) The search coil preamplifier gain and phase response, when applicableCalibrations for the DFB digital filter gain response have not been implemented, but the required convolution kernel is provided in this file. It was decided not to apply the digital filter gain response calibration to these Level 2 data because the application of the calibrations can introduce non-physical power 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 voltage sensor preamplifiers have not been implemented as the preamplifier response is flat and equal to one throughout the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to the voltage sensor data. 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. Likewise, all magnetic field quantities when present in these Level 2 data products are expressed by using units of nanoTelsas.The Level 2 data products contained in this data file are in spacecraft coordinates (e.g. x,y,z) or in sensor coordinates (e.g. dV12, dV34 for voltage measurements and [u,v,w] for the searchcoil magnetometer.The time resolution of the DFB continuous waveform data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB continuous waveform data cadence is typically 256 samples/NYsecond [2].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