not applicable

not applicable

not applicable

not applicable

This bundle contains derived data from the Cosmic Ray Subsystem (CRS), which was designed for cosmic ray studies. It consists of two high Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET).

Pioneer 10 Cosmic-ray telescope (CRT) data from the Jupiter encounter period, covering 1973-11-26 to 1973-12-15. The data set provides 15.0 minute flux averages from 18 electron, proton, and heavy ion channels.

Voyager_1 LECP - Low_Energy_Charged_Particle - Ions Data provided to CDPP by ONERA. All information included in this report: http://amda.cdpp.eu/help/parameters/doc/ONERA_Jupiter_plasma_db_for_AMDA.pdf

Pioneer 11 Cosmic-Ray Telescope (CRT) data from the Jupiter encounter period from 1974-11-26 and 1974-12-09. The data set provides 15.0 minute flux averages from 18 electron, proton, and heavy ion channels.

This data set contains ion flux data recorded by the COSPIN High Flux Telescope (HFT) during the Ulysses Jupiter encounter 1992-Jan-25 to 1992-Feb-18

This data set contains ion flux data recorded by the COSPIN High Flux Telescope (HFT) during the Ulysses Jupiter encounter 1992-Jan-25 to 1992-Feb-18

The Cosmic Ray Subsystem (CRS) was designed for cosmic ray studies. It consists of two high Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The detectors have large geometric factors (~ 0.48 to 8 cm^2 ster) and long electronic time constants (~ 24 [micro]sec) for low power consumption and good stability. Normally, the data are primarily derived from comprehensive ([Delta]E[1], [Delta]E[2] and E) pulse-height information about individual events. Because of the high particle fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on counting rates in single detectors and various coincidence rates. In inter- planetary space, guard counters are placed in anticoincidence with the primary detectors to reduce the background from high-energy particles penetrating through the sides of the telescopes. These guard counters were turned off in the Jovian magnetosphere when the accidental anticoincidence rate became high enough to block a substantial fraction of the desired counts. Fortunately, under these conditions the spectra were sufficiently soft that the background, due to penetrating particles, was small.

This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 48.0 second rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period).

• Data Set Overview
• =================

+------------------------------------------------------------------------------------------+

| Data Set Characteristics | Value |

| Instrument Principal Investigator | Rochus E. Vogt | | Data Supplier | National Space Science Data Center | | Data Sampling Rate | Variable (1 hr for FPHA Data, 15 min for all others) | | Data Set Start Time | 1979-02-28T00:00:00.000Z | | Data Set Stop Time | 1979-03-21T23:45:00.000Z | +------------------------------------------------------------------------------------------+

The following Description has been adapted from NSSDC CRS, 1979:

As its Name implies, the Cosmic Ray Subsystem (CRS) was designed for Cosmic Ray Studies (Stone et al., 1977b). It consists of two High Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The Detectors have large Geometric Factors (about 0.48 cm^2 sr to 8 cm^2 sr) and long Electronic Time Constants (∼24 µs) for low Power Consumption and good Stability. Normally, the Data are primarily derived from comprehensive (δE[1], δE[2] and E) Pulse-Height Information about individual Events. Because of the high Particle Fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on Counting Rates in single Detectors and various Coincidence Rates. In Interplanetary Space, Guard Counters are placed in Anticoincidence with the Primary Detectors to reduce the Background from High-Energy Particles penetrating through the Sides of the Telescopes. These Guard Counters were turned off in the Jovian Magnetosphere when the accidental Anticoincidence Rate became high enough to block a substantial Fraction of the desired Counts. Fortunately, under these Conditions the Spectra were sufficiently soft that the Background, due to penetrating Particles, was small.

The Data on Proton and Ion Fluxes at Jupiter were obtained with the LET. The Thicknesses of individual Solid-State Detectors in the LET and their Trigger Thresholds were chosen such that, even in the Jovian Magnetosphere, Electrons made, at most, a very minor Contribution to the Proton Counting Rates (Lupton and Stone, 1972). Dead Time Corrections and accidental Coincidences were small (<20%) throughout most of the Magnetotail, but were substantial (>50%) at Flux Maxima within 40 Rj Of Jupiter. Data have been included in this Package for those Periods when the Corrections are less than ∼50% and can be corrected by the User with the Dead Time appropriate to the Detector (2 δs to 25 δs). The high Counting Rates, however, caused some Baseline Shift which may have raised Proton Thresholds significantly. In the Inner Magnetosphere, the L[2] Counting Rate was still useful because it never rolled over. This Rate is due to 1.8 MeV to 13 MeV Protons penetrating L1 and >9 MeV Protons penetrating the Shield (8.4 cm^2 sr). For an E^-2 Spectrum, the two Groups would make comparable Contributions, but in the Magnetosphere, for the E^-3 to E^-4 Spectrum above 2.5 MeV (McDonald et al., 1979), the Contribution from Protons penetrating the Shield would be only 3% to 14%.

The LET L[1]L[2]L[4] and L[1]L[2]L[3] Coincidence-Anticoincidence Rates give the Proton Flux between 1.8 MeV and 8 MeV and 3 MeV to 8 MeV with a small Alpha Particle Contribution (~10^-3). Corrections are required for Dead Time Losses in L[1], accidental L[1]L[2] Coincidences and Anticoincidence Losses from L[4]. Data are given only for Periods when these Corrections are relatively small. In addition to the Rates listed in the Table, the Energy lost in Detectors L[1], L[2] and L[3] was measured for individual Particles. For Protons, this covered the Energy Range from 0.42 MeV to 8.3 MeV. Protons can be identified positively by the δE versus E Technique, their Spectra obtained and accidental Coincidences greatly reduced. Because of Telemetry Limitations, however, only a small Fraction of the Events could be transmitted, and Statistics become poor unless Pulse-Height Data are averaged over a Period of one Hour.

HET and LET Detectors share the same Data Lines and Pulse-Height Analyzers. Thus, the Telescopes can interfere with one another during Periods of high Counting Rates. To prevent such an Interference and explore different Coincidence Conditions, the Experiment was cycled through four Operating Modes, each 192 s long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] Coincidence Requirements. The TET was cycled through various Coincidence Conditions, including Singles from the Front Detectors. At the Expense of some Time Resolution, this Procedure permitted us to obtain significant Data in the Outer Magnetosphere and excellent Data during the long Passage through the Magnetotail Region.

Some of the published Results from this Experiment required extensive Corrections for Dead Time, accidental Coincidences and Anticoincidences (Vogt et al., 1979a, Vogt et al., 1979b, Schardt et al., 1981, Gehrels, 1981). These Corrections can be applied only on a case-by-case Basis after a careful Study of the Environment and many Self-Consistency Checks. They cannot be applied on a systematic Basis and we have no Computer Programs to do so. Therefore, Data from such Periods are not included in the Data Center Submission. The Scientists on the CRS Team will, however, be glad to consider special Requests if the desired Information can be extracted from the Data.

• Description of the Data
• =======================

(1) LD1 RATE gives the nominal >0.43 MeV Proton Flux (cm^2 s sr)^-1. This Rate includes all Particles which pass through a 0.8 mg/cm^2 Aluminum Foil and deposits more than 220 keV in a 34.6 µm Silicon Detector on Voyager 1 (209 keV, 33.9 µm on Voyager 2) Therefore, Heavy Ions, such as Oxygen and Sulfur are also detected, however, their Contribution is believed to be relatively small. Only a small Percentage of the Pulses in this Detector are larger than the maximum Energy that can be deposited by a Proton. Heavy Ions would produce such large Pulses, unless their Energy Spectra were much steeper than the Proton Spectrum. The true Flux, F(t), can be calculated from the Data:

F(t) = F/(1-1.26x10^-4 F)

and Corrections are small for F<1000 (cm^2 s)^-1.

(2) The LD2 RATE is not suitable for an Absolute Flux Determination and is given in counts per second. The Detector responds to Protons and Ions that penetrate either (a) 0.8 mg/cm^2 Aluminum plus 8.0 mg/cm^2 Silicon and lose at least 200 keV in a 35 µm Si Detector (1.8 MeV to 13 MeV) or (b) pass through >140 mg/cm^2 Aluminum. For an E^-2 Proton Spectrum, the Contributions from (a) and (b) would be about equal, however, the Proton Spectrum is substantially softer throughout most of the Magnetosphere and the Detector should respond primarily to (a). Dead Time Corrections are given by

R(t) = R/(1-2.55x10^-5 R)

where R is the Count Rate in counts per second. Thus, Correction to the supplied data are small for R<4000 counts per second, but become so large in the middle Magnetosphere that the Magnitude of even relative intensity Changes becomes uncertain.

(3) LD L[1].L[2].L[4]. SL COINCIDENCE RATE gives the total Proton Flux (cm^2 s sr)^-1 between 1.8 MeV and 8.1 MeV with a small Admixture of Alpha Particles. Accidental Coincidences become subst

This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 2 while the spacecraft was within the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >13 keV electrons and >24 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period).

This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Jupiter far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period).

This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Jupiter far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period).

This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 2 while the spacecraft was within the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >13 keV electrons and >24 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period).

This data set provides energetic (MeV) ion fluxes for a variety of different Z values (carbon, oxygen, sulfur) derived from the Heavy Ion Counter (HIC) instrument on the Galileo spacecraft. The data set includes all recorded intervals at Jupiter.

Data Set Overview

• Data Set Description
• ===================

This Near Encounter Step Data Set consists of Electron and Ion Counting Rate and Flux Data from the Low Energy Charged Particle (LECP) Experiment on Voyager 1 while the Spacecraft was within the very close Vicinity of Jupiter.

The LECP Instrument measures the Intensities of in situ Charged Particles (>15 keV Electrons and >30 keV Ions) with various Levels of Discrimination based on Energy Range and Mass Species. A Subset of almost 100 LECP Channels are included in this Data Set. The LECP Data are globally calibrated to the extent possible (see below).

During the Jupiter Near Encounter, the Low Energy Magnetospheric Particle Analyzer (LEMPA) subsystem was turned on for Data Collection. Particles include low Energy Electrons, Protons, Alpha Particles, medium Energy Protons and Ions, high Energy and high Intensity protons, Electrons, Alpha Particles, and Z≥2 Nuclei. The Near Encounter Data are 48 s Rate and Flux Measurements within one eighth of the LECP instrumental Motor Rotation Period (the angular Scanning Periods or Step Period).

The LECP Instrument has a rotating Head for obtaining angular Anisotropy Measurements of the medium Energy Charged Particles. A gear-drive Motor steps through eight equal angular Sectors per Revolution for Data Collection. The Cycle Time for the Rotation is 25.6 min or 48 min during Cruise Mode, and 48 s or 192 s during the Planetary Encounter.

The Data were originally collected in the Form of "Rate" Data which were not always 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 the Background. Both the Mass Species and the 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. The Background is to be determined from context and from making use of Sector 8 Rates (Sector 8 is covered by a 2 mm Aluminium Sunshield and is used for Data Calibration).
• 2) Divide the Background-corrected Rate by the Geometric Factor of the Channel and by the Energy Bandpass of the Channel.

To determine the Energy Bandpass, one must judge the Mass Species of the detected Particles (for Ions but not for Electrons). The Energy Bandpasses are given in the Entries MINIMUM_INSTRUMENT_PARAMETER and MAXIMUM_INSTRUMENT_PARAMETER in Table FPLECPENERGY, and are given in the Form of "Energy per 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 the Entries for MINIMUM_INSTRUMENT_PARAMETER and MAXIMUM_INSTRUMENT_PARAMETER in Table FPLECPCHANZ, which give the Minimum and Maximum "Z" Value accepted. Note that 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., (1979a)). The final Product of these Instructions will be the Particle Intensity in Units of counts/(cm^2 s sr keV). LECP Data can also be in the Form of Flux, whose Units are (cm^2 s sr)^-1.

• Near Encounter Channel Definitions for Voyager 1 LECP
• =====================================================

+-----------------------------------------------------------------------------------------------------------------+

| CH Num | CH Name | Low (MeV/n) | High (MeV/n) | Mean (MeV/n) | Geometric Factor (cm^2 sr) | CH Logic Definition |

| 1 | EB01 | 0.015 | 0.037 | 0.020 | 0.00600 | | | 2 | EBD1 | 0.015 | 0.500 | 0.020 | 0.00012 | | | 3 | EB02 | 0.037 | 0.061 | 0.045 | 0.00600 | | | 4 | EBD2 | 0.037 | 0.500 | 0.045 | 0.00012 | | | 5 | EB03 | 0.070 | 0.112 | 0.090 | 0.00600 | | | 6 | EBD3 | 0.070 | 0.500 | 0.090 | 0.00012 | | | 7 | EB04 | 0.130 | 0.183 | 0.120 | 0.00600 | | | 8 | EBD4 | 0.130 | 0.500 | 0.120 | 0.00012 | | | 9 | EB05 | 0.200 | 0.500 | 0.200 | 0.00600 | | | 10 | EBD5 | 0.200 | 0.500 | 0.200 | 0.00012 | | | 11 | EG06 | 0.252 | 2.000 | 0.250 | 0.00200 | | | 12 | EG07 | 0.480 | 2.000 | 0.500 | 0.00200 | | | 13 | EG08 | 0.853 | 2.000 | 0.900 | 0.00200 | | | 14 | EG09 | 2.100 | 5.000 | 2.000 | 0.00200 | | | 15 | E44 | 0.350 | 1.500 | 0.500 | 1.31000 | | | 16 | E45 | 2.500 | 100.000 | 2.000 | 1.31000 | | | 17 | E37 | 6.000 | 100.000 | 6.000 | 1.31000 | | | 18 | PL01 | 0.030 | 0.053 | 0.025 | 0.04020 | | | 19 | PL02 | 0.053 | 0.085 | 0.050 | 0.04020 | | | 20 | PL03 | 0.085 | 0.139 | 0.100 | 0.04020 | | | 21 | PL04 | 0.139 | 0.200 | 0.150 | 0.04020 | | | 22 | PL05 | 0.200 | 0.550 | 0.250 | 0.04020 | | | 23 | PL06 | 0.540 | 1.050 | 0.600 | 0.04020 | | | 24 | PL07 | 1.050 | 2.030 | 1.000 | 0.04020 | | | 25 | PL08 | 2.030 | 4.010 | 2.500 | 0.04020 | | | 44 | AL01 | 0.980 | 1.770 | 1.000 | 0.04020 | | | 45 | AL02 | 1.770 | 4.220 | 2.500 | 0.04020 | | | 77 | ESA0 | 2.500 | 99.999 | 2.500 | 0.49350 | A-B Coincidence | | 78 | ESB0 | 8.500 | 99.999 | 8.500 | 0.94620 | B 4π sr | | 79 | AB10 | 8.500 | 99.999 | 8.500 | 0.05040 | A-B Coincidence | | 80 | DP09 | 0.285 | 5.020 | 0.250 | 0.00084 | Delta' | | 81 | DP10 | 0.480 | 2.580 | 0.600 | 0.00084 | Delta' | | 82 | DP11 | 0.725 | 1.640 | 1.000 | 0.00084 | Delta' | | 83 | PD09 | 0.285 | 5.250 | 0.250 | 0.00260 | Delta | | 84 | PD10 | 0.480 | 2.720 | 0.600 | 0.00260 | Delta | | 85 | PD11 | 0.725 | 1.580 | 1.000 | 0.00260 | Delta | | 86 | AB12 | 54.000 | 87.300 | 50.000 | 0.05040 | A-B Coincidence | | 87 | AB13 | 87.300 | 152.000 | 100.000 | 0.05040 | A-B Coincidence | | 88 | PSA1 | 15.800 | 158.000 | 15.000 | 0.49350 | A 2π sr | | 89 | PSA2 | 15.800 | 49.000 | 25.000 | 0.49350 | A 2π sr | | 90 | PSA3 | 16.300 | 26.200 | 25.000 | 0.49350 | A 2π sr | | 91 | PSB1 | 54.000 | 174.000 | 50.000 | 0.94620 | B 4π sr | | 92 | PSB2 | 54.000 | 87.300 | 50.000 | 0.94620 | B 4π sr | | 93 | PSB3 | 54.000 | 59.000 | 50.000 | 0.94620 | B 4π sr | | 94 | DA03 | 0.480 | 2.450 | 0.600 | 0.00084 | Delta' | | 95 | DA04 | 0.780 | 1.410 | 1.000 | 0.00084 | Delta' | | 96 | DZ01 | 0.405 | 18.800 | 0.600 | 0.00084 | Delta' | | 97 | AD03 | 0.480 | 2.580 | 0.600 | 0.00260 | Delta | | 98 | AD04 | 0.780 | 1.480 | 1.000 | 0.00260 | Delta | | 99 | ZD01 | 0.400 | 19.800 | 0.600 | 0.00260 | Delta | +-----------------------------------------------------------------------------------------------------------------+

• Near Encounter Data are stored in Files for Channels from different Rate Groups indicated by the File Name
• ==========================================================================================================

+-----------------------------------------+ |

• Data Set Overview

• =================

• Data Set Description

• ====================

This Far Encounter Step Data Set consists of Electron and Ion Counting Rate and Flux Data from the Low Energy Charged Particle (LECP) Experiment on Voyager 2 while the Spacecraft was within the Vicinity of Jupiter.

The LECP Instrument measures the Intensities of in situ Charged Particles (>13 keV Electrons and >24 keV Ions) with various Levels of Discrimination based on Energy Range, Mass Species, and angular Arrival Direction. A Subset of almost 100 LECP Channels are included in this Data Set. The LECP Data are globally calibrated to the extent possible (see below).

During the Jupiter Far Encounter, the entire Low Energy Particle Telescope (LEPT) and Part of the Low Energy Magnetospheric Particle Analyzer (LEMPA) Subsystem were turned on for Data Collection. Particles include Electrons, Protons, Alpha Particles, and Light, Medium, and Heavy Nuclei Particles. The Far Encounter Data are 3.2 min Rate and Flux Measurements within one eighth of the LECP instrumental Motor Rotation Period (the angular Scanning Period or Step Period).

The LECP Instrument has a rotating Head for obtaining angular Anisotropy Measurements of the Medium Energy Charged Particles. A gear-drive Motor steps through eight equal angular Sectors per Revolution for Data Collection.

The Cycle Time for the Rotation is 25.6 min or 48 min during Cruise Mode, and 48 s or 192 s during the Planetary Encounter.

The Data were originally collected in the Form of "Rate" Data which were not always 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 the Background. Both the Mass Species and the 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. The Background is to be determined from context and from making use of Sector 8 Rates (Sector 8 is covered by a 2 mm Aluminium Sunshield and is used for Data Calibration).
• 2) Divide the Background-corrected Rate by the Geometric Factor of the Channel and by the Energy Bandpass of the Channel.

The Geometric Factor is found in the Entry for CHANNEL_GEOMETRIC_FACTOR as associated with the CHANNEL_ID of each Channel.

To determine the Energy Bandpass, one must judge the Mass Species of the detected Particles (for Ions but not for Electrons). The Energy Bandpasses are given in the Entries MINIMUM_INSTRUMENT_PARAMETER and MAXIMUM_INSTRUMENT_PARAMETER in Table FPLECPENERGY, and are given in the Form of "Energy per 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 the Entries for MINIMUM_INSTRUMENT_PARAMETER and MAXIMUM_INSTRUMENT_PARAMETER in Table FPLECPCHANZ, which give the Minimum and Maximum "Z" Value accepted. Note that 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., (1979a)). The final Product of these Instructions will be the Particle Intensity in Units of counts/(cm^2 s sr keV). LECP Data can also be expressed in the Form of Flux, whose Units are (cm^2 s sr)^-1.

• Far Encounter Channel Definitions for Voyager 2 LECP
• ====================================================

+-----------------------------------------------------------------------------------------------------------------+

| CH Num | CH Name | Low (MeV/n) | High (MeV/n) | Mean (MeV/n) | Geometric Factor (cm^2 sr) | CH Logic Definition |

| 1 | EB01 | 0.013 | 0.035 | 0.020 | 0.00200 | | | 2 | EBD1 | 0.013 | 0.035 | 0.020 | 0.00200 | | | 3 | EB02 | 0.035 | 0.061 | 0.045 | 0.00200 | | | 4 | EBD2 | 0.035 | 0.061 | 0.045 | 0.00200 | | | 5 | EB03 | 0.061 | 0.112 | 0.090 | 0.00200 | | | 6 | EBD3 | 0.061 | 0.112 | 0.090 | 0.00200 | | | 7 | EB04 | 0.112 | 0.183 | 0.120 | 0.00200 | | | 8 | EBD4 | 0.112 | 0.183 | 0.120 | 0.00200 | | | 9 | EB05 | 0.183 | 0.500 | 0.200 | 0.00200 | | | 10 | EBD5 | 0.183 | 0.500 | 0.200 | 0.00200 | | | 11 | EG06 | 0.252 | 2.000 | 0.250 | 0.00200 | | | 12 | EG07 | 0.480 | 2.000 | 0.500 | 0.00200 | | | 13 | EG08 | 0.853 | 2.000 | 0.900 | 0.00200 | | | 14 | EG09 | 2.100 | 5.000 | 2.000 | 0.00200 | | | 15 | E44 | 0.350 | 1.500 | 0.500 | 1.31000 | | | 16 | E45 | 2.000 | 100.000 | 2.000 | 1.31000 | | | 17 | E37 | 6.000 | 100.000 | 6.000 | 1.31000 | | | 18 | PL01 | 0.024 | 0.048 | 0.025 | 0.12000 | | | 19 | PL02 | 0.048 | 0.080 | 0.050 | 0.12000 | | | 20 | PL03 | 0.080 | 0.137 | 0.100 | 0.12000 | | | 21 | PL04 | 0.137 | 0.215 | 0.150 | 0.12000 | | | 22 | PL05 | 0.215 | 0.540 | 0.250 | 0.12000 | | | 23 | PL06 | 0.540 | 0.990 | 0.600 | 0.12000 | | | 24 | PL07 | 0.990 | 2.140 | 1.000 | 0.12000 | | | 25 | PL08 | 2.140 | 3.500 | 2.500 | 0.12000 | | | 26 | P32 | 0.330 | 0.610 | 0.350 | 0.09750 | E0E2(E3) | | 27 | P1 | 0.520 | 1.450 | 0.600 | 0.44100 | E1E2(E3) | | 28 | P10 | 4.400 | 11.400 | 5.000 | 0.53900 | E2E3(E4) | | 29 | P11 | 11.400 | 20.000 | 12.000 | 0.53900 | E2E3(E4) | | 30 | P16 | 3.040 | 17.000 | 5.000 | 1.50000 | E5E4(E3) | | 31 | P23 | 22.000 | 30.000 | 25.000 | 1.31000 | E5E4E3(E2) | | 32 | P27 | 37.000 | 89.000 | 50.000 | 1.20000 | E5E4E3E2 | | 33 | P31 | 213.000 | 1000.000 | 250.000 | 1.31000 | E4E3 | | 34 | A39 | 0.091 | 0.233 | 0.100 | 0.09750 | E0(E2) | | 35 | A33 | 0.230 | 0.480 | 0.350 | 0.09750 | E0E2(E3) | | 36 | A46 | 0.147 | 2.000 | 0.600 | 0.44100 | 'D1F1,CA' | | 37 | A3 | 0.420 | 1.700 | 0.600 | 0.44100 | E1E2(E3) | | 38 | A4 | 1.800 | 4.000 | 2.500 | 0.44100 | E1E2(E3L12) | | 39 | A12 | 4.200 | 7.800 | 5.000 | 0.53900 | E2E3(E4L23) | | 40 | A13 | 7.800 | 20.000 | 15.000 | 0.53900 | E2E3(E4L23) | | 41 | A17 | 3.000 | 58.000 | 5.000 | 1.50000 | E5E4(E3L54) | | 42 | A24 | 22.000 | 30.000 | 25.000 | 1.31000 | E5E4E3(E2) | | 43 | A28 | 31.000 | 56.000 | 50.000 | 1.20000 | E5E4E3E2 | | 44 | AL01 | 1.040 | 1.850 | 1.000 | 0.12000 | CALC. | | 45 | AL02 | 1.850 | 3.700 | 2.500 | 0.12000 | CALC. | | 46 | M34 | 0.230 | 0.440 | 0.200 | 0.09750 | E0E2 | | 47 | L5 | 0.710 | 5.600 | 1.500 | 0.44100 | E1E2(E3L12) | | 48 | L14 | 5.800 | 28.000 | 6.000 | 0.53900 | E2E3(E4L23) | | 49 | L18 | 3.900 | 20.000 | 5.000 | 1.50000 | E5E4(E3L54) | | 50 | M38 | 0.060 | 0.200 | 0.100 | 0.09750 | E0(E2) | | 51 | M35 | 0.200 | 0.340 | 0.250 | 0.09750 | E0E2(E3) | | 52 | M47 | 0.124 | 14.300 | 0.250 | 0.44100