cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.48322/8fc4-fq16
title: PSP FIELDS Fluxgate Magnetometer (MAG) Magnetic Field Vectors, Spacecraft, SC, Coordinates, Full Resolution, Level 2 (L2), 3.413 ms Data

description: 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
DOI: 10.48322/pq4w-8z67
title: PSP FIELDS Fluxgate Magnetometer (MAG) Magnetic Field Vectors, Spacecraft, SC, Coordinates, 4 samples/cycle, Level 2 (L2), 3.413 ms Data

description: 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
DOI: 10.48322/7hrp-ya88
title: PSP FIELDS Fluxgate Magnetometer (MAG) Magnetic Field Vectors, Spacecraft, SC, Coordinates, Level 2 (L2), 1 min Data

description: 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
DOI: 10.48322/7r0d-mp78
title: PSP FIELDS Fluxgate Magnetometer (MAG) Magnetic Field Vectors, (VS) Venus Solar Orbital Coordinates, Level 2 (L2), 7 s Data

description: PSP FIELDS Fluxgate Magnetometer data. Time resolution varies with instrument mode, ranging from 2.3-292.9 samples/sec, corresponding to 2-256 samples per 0.874 seconds (0.874 = 2^25 / 38.4 MHz, see reference [2]).
The Magnetometer has 4 ranges - +/-1024, +/-4096, +/-16,384, +/-65,536 nT, selected by the ranging algorithm, based on the ambient magnetic field. Precision is +/- 15 bits, based on the 16-bit 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
DOI: 10.48322/baqw-yt37
title: PSP FIELDS Merged Searchcoil Magnetometer, SCM, and Magnetometer, MAG, (SCAM) Waveform, Level 3 (L3), 7 s Data

description: PSP FIELDS Merged Search Coil Magnetometer and Fluxgate Magnetometer (SCaM), SCaM data.
Merged SCaM data is composed of SCM and MAG data from the FIELDS experiment on the Parker Solar Probe spacecraft [1]. For a full description of the FIELDS experiment, see [2]. The SCM is sampled by the Digital Fields Board (DFB), discussed in ref. [3]. For an overview of FIELDS/MAG calibration see ref. [4].
SCaM data consists of continuous time-series data from the SCM and MAG sensors. Merged SCaM data is a Level 3 (l3) product derived from the direct sum of weighted and time corrected l1 MAG and SCM data [4]. The weighting coefficients are designed to optimize the SCaM signal to the integrated instrumental noise floor.
The Level 3 SCaM product uses SCM data which has been calibrated for (i) DFB in-band gain, (ii) DFB analog filter gain/phase response, (iii) DFB digital filter gain/phase response, and (iv) the SCM preamplifier gain/phase response. The SCM data is empirically gain-matched to the MAG, with correction factors included in the metadata [4]. Information on SCM sample rate is provided at a 1 min cadence.
The Level 3 SCaM product uses orthogonalized MAG data with spacecraft zero offsets removed. Spacecraft zero offset data, along with the native MAG range and sample-rate meta-data is provided at a 1 minute cadence.
The Level 3 SCaM data product in this file may be in spacecraft coordinates (e.g. X,Y,Z), RTN coordinates (R,T,N), or SCM sensor coordinates (U,V,W). For large parts of the PSP mission, anomalous performance of the SCM sensor-X axis (in the U direction) precludes merging in SC or RTN coordinates. In these cases data is only provided for the SCM sensor coordinate system (V,W).
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. (2016) JGR Space Physics, 121, 5088-5096. https://doi.org/10.1002/2016JA022344
4. Bowen, T.A., Bale, S.D., Bonnell, J.W., Dudok DeWit, T. et al. (2020) JGR Space Physics, https://doi.org/10.1029/2020JA027813
DOI: 10.48322/gf9t-4082
title: Parker Solar Probe, FIELDS Radio Frequency Spectrometer, RFS, High Frequency Receiver, HFR, Spectra, Level 2 (L2), 7 s and 56 s Data

description: 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
DOI: 10.48322/re4h-tk40
title: Parker Solar Probe, FIELDS Radio Frequency Spectrometer, RFS, Low Frequency Receiver, LFR, Spectra, Level 2 (L2), 7 s and 56 s Data

description: 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
DOI: 10.48322/41s1-hx58
title: Parker Solar Probe Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data

description: Heliocentric trajectories for Parker Solar Probe in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, Coordinates

The original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth.

The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch" which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage:

+---------------------------------------------------------------------+
| Method Name  | FPA Longitude Definition                             |
|---------------------------------------------------------------------|
| B1950.0      | the actual FPA at 22:09 UT on December 31, 1949      |
| J2000.0      | the smoothed FPA at 12:00 UT on January 1, 2000      |
| True of Date | the actual FPA at 00:00 UT on the date of interest   |
| Mean of Date | the smoothed FPA at 00:00 UT on the date of interest |
+---------------------------------------------------------------------+

The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method.

More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.

Citation: Szabo, A. (2020). Parker Solar Probe Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/41s1-hx58
DOI: 10.48322/6b2f-mx69
title: PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 10 s Data

description: Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.

The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).

Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.

The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:

Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).

Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 10 s Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/6b2f-mx69
DOI: 10.48322/ahkk-d044
title: PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 1 h Data

description: Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.

The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).

Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.

The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:

Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).

Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 1 h Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/ahkk-d044
DOI: 10.48322/7gr7-1791
title: PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 1 min Data

description: Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.

The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).

Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.

The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:

Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).

Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 1 min Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/7gr7-1791
DOI: 10.48322/jwkm-bn55
title: PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 5 min Data

description: Parker Solar Probe, PSP, Integrated Science Investigation of the Sun, IS☉IS, Energetic Particle Instrument, EPI-Hi, High Energy Telescope, HET, Rates: The Epoch time tags indicate midpoint of integration. For information concerning use of the IS☉IS data please refer to the Energetic Particle Data User Guide available from the PSP IS☉IS Science Operations Center, SOC, web site hosted by the University of New Hampshire. The energetic particle pitch angle calculations are made possible via use of magnetic field data provided by the PSP FIELDS team.

The public data reflect current instrument calibration as determined by the IS☉IS science team. Calibration efforts are ongoing and the public data will be updated over the course of the mission based on improved understanding of instrument response to the near-Sun energetic particle environment. IS☉IS visualization tools are provided as a quicklook utility for the community to better access the IS☉IS data and are also under continual development. While we make every effort to ensure their accuracy, the IS☉IS team cannot guarantee that they are error-free. For questions regarding the use of IS☉IS data, please contact Colin Joyce (cjjoyce@princeton.edu).

Refer to the following web site concerning the Rules of use for the IS☉IS energetic particle data: https://spp-isois.sr.unh.edu/ISOIS_Terms_of_Use.html.

The PSP IS☉IS effort is funded as part of the NASA Parker Solar Probe mission under contract NNN06AA01C. Use of any PSP IS☉IS data in publications or presentations should include the following text for acknowledgement and also cite the PSP IS☉IS instrument suite publication:

Acknowledgement: Thanks to the Integrated Science Investigation of the Sun (IS☉IS) Science Team (PI: D. J. McComas, Princeton University).

Citation: McComas, D. J. (2020). PSP Integrated Science Investigation of the Sun, Energetic Particle Instrument-Hi (ISOIS EPI-Hi) High Energy Telescope (HET) Rates, Level 2 (L2), 5 min Data [Data set]. NASA Space Physics Data Facility.