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ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental and Isotopic Density, Speed, Thermal Speed, Charge State, and Ratio Parameters, Level 2 (L2), Daily Data

This ACE SWICS/SWIMS Data Set contains the He/O, C/O, N/O, Ne/O, Mg/O, Si/O, S/O, Fe/O Abundance Ratios, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. 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. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

VOYAGER 2 SAT LOW ENERGY CHARGED PARTICLE CALIB. 15MIN

THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as su

ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental and Isotopic Density, Speed, Thermal Speed, Charge State, and Ratio Parameters, Level 2 (L2), 1 h Data

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, Fe/O Abundance Ratio, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. 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. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

VOYAGER 1 SAT LOW ENERGY CHARGED PARTICLE CALIB. 15MIN

THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 1 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as su

restrictedus-pdApr 2025View details →

VOYAGER 2 SAT LOW ENERGY CHARGED PARTICLE CALIB. BR 15MIN

THIS BROWSE DATA CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. FOR THIS BROWSE DATA SET ONLY SCAN AVERAGE DATA IS GIVEN (NO ANGULAR INFORMATION). THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.

Voyager 1 Low-Energy Charged Particle (LECP) Background-Corrected Electron Differential Fluxes, Daily Data in CDF Format

This data set contains data from the LECP instrument on the Voyager 1 spacecraft. Each record in a file contains 1-day (24-hour) scan-averaged fluxes and flux uncertainties of electrons in two contiguous energy channels that cover the energy range 26-70 keV. The period 2002/001 through 2012/240 includes electrons measured upstream of the termination shock and in the heliosheath up though ~2 days after the heliopause crossing. The Voyager 1 LECP instrument steps through eight, 45 deg full-angle sectors, spending 192 sec in each sector, yielding a full scan through 360 deg every 25.6 min. The LECP scan plane is nearly parallel to RT-plane of the heliospheric RTN coordinate system. The electron data are averaged over the seven active sectors S1-S7; S8 is behind the sun-shield and not included in the average.-- Electron channels designated EB01 and EB02-- Data have been corrected to remove background due to penetrating cosmic ray ions-- Electron fluxes and uncertainties (one st. dev.) in units: (cm^2 s sr MeV)^-1-- Data are 5-point running averages of daily values-- Values -9.900e+01 used for missing or nonphysical data-- Negative year indicates filled data for the associated doy

VOYAGER 1 JUP LOW ENERGY CHARGED PARTICLE CALIB. BR 15MIN

THIS BROWSE DATA CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 1 WHILE THE SPACECRAFT WAS IN THE VICINITY OF JUPITER. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. FOR THIS BROWSE DATA SET ONLY SCAN AVERAGE DATA IS GIVEN (NO ANGULAR INFORMATION). THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.

restrictedus-pdApr 2025View details →

VOYAGER 2 JUP LOW ENERGY CHARGED PARTICLE CALIB. BR 15MIN

THIS BROWSE DATA CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF JUPITER. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. FOR THIS BROWSE DATA SET ONLY SCAN AVERAGE DATA IS GIVEN (NO ANGULAR INFORMATION). THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS U HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.

restrictednotspecifiedAug 2025View details →

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPC Ion Charge Flux Distributions, Electrical Current versus Time and Energy-per-Charge, Level 2 (L2), 0.2185 s Data

SPC Level 2 Ion Data--------------------File Naming Format: psp_swp_spc_l2i_yyyymmdd_v01.cdfSolar Probe Cup, SPC, charge flux distributions comprise electrical current as a function of time and energy-per-charge, with appropriate instrument response elements considered and calibrations applied. This data product contains measurements of ion flux as a function of energy organized into spectra. The SPC instrument measures one-dimensional distributions with a wide field of view. Please refer to the instrument paper for details.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation.The MODE_FLAG variable contains information about the type of spectrum being measured. "Ion Full Scan" spectra are marked with MODE_FLAG.DAT = 1. These spectra comprise a broad energy range typically with lower signal-to-noise than the more frequent "Ion Peak Tracking" spectra, which are marked with MODE_FLAG.DAT equal to zero. In the most frequent operating mode, ion full scans are executed about once every 30 s or whenever the peak signal from the solar wind is poorly defined.SPC Encounter 1 Remarks-----------------------Data quality is very good for the duration of the encounter. The solar wind flow was within the optimal field of view for the SPC instrument for nearly the entire encounter. See the data flags for specific exceptions. As with all encounters, signal-to-noise is higher during ingress than egress, which is reflected in the typically smaller uncertainties and less frequent "primary peak low signal" flag events.SPC Cruise Phase Remarks------------------------Measurements recorded during cruise phase are not all transmitted to Earth. The typical return is one spectrum out of every 32.SPC Encounter 2 Remarks-----------------------Due to an erroneous setting in the operating mode for this encounter, ion full scan spectra and certain spectra immediately following ion full scans are of reduced quality. In the affected full scan spectra, the energy steps over an initial portion of the measurement spectra have zero width, i.e. the Level 2 ion variables MV_LO.DAT = MV_HI.DAT, and the corresponding measurements are purely noise. In some cases, this results in a poor determination of the proton "primary peak" energy, which renders additional subsequent full scans that follow subject to the same incompleteness. In other cases, the energy range for the subsequent "ion peak tracking mode" scan is not ideal. The affected Level 3 ion measurements have been flagged with DQF.DAT[22]=1, which stands for "energy ranging/peak tracking error" and/or set to fill. The operating mode has been revised such that future encounters will not be so affected.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

restrictedus-pdApr 2025View details →

VOYAGER 1 SAT LOW ENERGY CHARGED PARTICLE CALIB. BR 15MIN

THIS BROWSE DATA CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 1 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. FOR THIS BROWSE DATA SET ONLY SCAN AVERAGE DATA IS GIVEN (NO ANGULAR INFORMATION). THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.

Voyager 2 Low-Energy Charged Particle (LECP) Background-Corrected Electron Differential Fluxes, Daily Data in CDF Format

This data set contains data from the LECP instrument on the Voyager 2 spacecraft. Each record in a file contains 1-day (24-hour) scan-averaged fluxes and flux uncertainties of electrons in two contiguous energy channels that cover the energy range 22-61 keV. The period 2006/001 through 2018/304 includes electrons measured upstream of the termination shock and in the heliosheath up to heliopause crossing. The voyager 2 LECP instrument steps through eight, 45 deg full-angle sectors, spending 192 sec in each sector, yielding a full scan through 360 deg every 25.6 min. The LECP scan plane is nearly parallel to RT-plane of the heliospheric RTN coordinate system. The electron data are averaged over the seven active sectors S1-S7; S8 is behind the sun-shield and not included in the average.-- Electron channels designated EB01 and EB02-- Data have been corrected to remove background due to penetrating cosmic ray ions-- Electron fluxes and uncertainties (one st. dev.) in units: (cm^2 s sr MeV)^-1-- Data are 5-point running averages of daily values-- Values -9.900e+01 used for missing or nonphysical data-- Negative year indicates filled data for the associated doy

ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental and Isotopic Density, Speed, Thermal Speed, Charge State, and Ratio Parameters, Level 2 (L2), 2 h Data

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, He/O, C/O, Ne/O, Mg/O, Si/O, Fe/O Abundance Ratios, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. 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. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

VOYAGER 1 JUP LOW ENERGY CHARGED PARTICLE CALIB. 15MIN

THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 1 WHILE THE SPACECRAFT WAS IN THE VICINITY OF JUPITER. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as s

restrictednotspecifiedAug 2025View details →

SOHO Charge, Element, and Isotope Analysis System (CELIAS) Proton Monitor (PM) 5-minute Solar Wind Data in CDF Format

The data include 5-minute proton speed, density, most probable thermal speed, and arrival direction, as well as predicted alpha-particle speed. Also included are the SOHO spacecraft predicted positon in GSE coordinates, Heliocentric Range, Heliographic Latitude and Longitude, and Earth Carrington Rotation Number. This CDF dataset was converted from the original ASCII dataset at the SOHO Archive https://soho.nascom.nasa.gov/data/archive.html. Description of the CELIAS-PM instrument and scientific scope can be found on the CELIAS instrument home page http://www2.physik.uni-kiel.de/SOHO-CELIAS/ and on the SOHO mission home page https://sohowww.nascom.nasa.gov/. CELIAS Instrument Publication: Hovestadt, D., Hilchenbach, M., Bürgi, A. et al. CELIAS - Charge, Element and Isotope Analysis System for SOHO, Sol Phys 162, 441–481 (1995), https://doi.org/10.1007/BF00733436.

VOYAGER 2 JUP LOW ENERGY CHARGED PARTICLE CALIB. 15MIN

THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF JUPITER. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as s