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CDAWeb Served Heliophysics Datasets Beginning with 'L'

L0_K0_MPA: LANL 1990-095 Magnetospheric Plasma Analyzer Key Parameters - D. McComas (LANL)
L0_K0_SPA: LANL 1990 Synchronous Orbit Particle Analyzer Key Parameters - Reiner Friedel (LANL)
L1_K0_GIFWALK: Links to GEOSYNC KP pre-generated survey and other plots - Polar-Wind-Geotail Ground System (NASA GSFC)
L1_K0_MPA: LANL 1991-080 Magnetospheric Plasma Analyzer Key Parameters - D. McComas (LANL)
L1_K0_SPA: LANL 1991 Synchronous Orbit Particle Analyzer Key Parameters - Reiner Friedel (LANL)
L4_K0_MPA: LANL 1994-084 Magnetospheric Plasma Analyzer Key Parameters - D. McComas (LANL)
L4_K0_SPA: LANL 1994 Synchronous Orbit Particle Analyzer Key Parameters - Reiner Friedel (LANL)
L7_H0_MPA: LANL 1997 Magnetospheric Plasma Analyzer High Resolution data - D. McComas (LANL)
L7_K0_MPA: LANL 1997 Magnetospheric Plasma Analyzer Key Parameters - D. McComas (LANL)
L7_K0_SPA: LANL 1997 Synchronous Orbit Particle Analyzer Key Parameters - Reiner Friedel (LANL)
L9_H0_MPA: LANL 1989-046 Magnetospheric Plasma Analyzer High Resolution data - D. McComas (LANL)
L9_K0_MPA: LANL 1989-046 Magnetospheric Plasma Analyzer Key Parameters - D. McComas (LANL)
L9_K0_SPA: LANL 1989 Synchronous Orbit Particle Analyzer Key Parameters - Reiner Friedel (LANL)
L0_K0_MPA doi:10.48322/b3yv-mf47
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.
Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
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L0_K0_SPA doi:10.48322/zzr5-dd89
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
Status of SOPA Instrument 1990-095:  Loss of all ion data as of July 1992
All three thin, front, D1 detectors have failed, having become intolerably
noisy.  The net result of this failure is the complete loss of proton, 
helium, carbon, nitrogen, oxygen and other high Z Key Parameter data from
the instrument.  Since all three thick, back D2 detectors are still 
operating normally, the electron measurements remain only insignificantly 
affected.
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992
Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993
Modified proton  summation to eliminate noisy channel.
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
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L1_K0_GIFWALK
Description
Pre-generated PWG plots
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
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L1_K0_MPA doi:10.48322/5jaw-x105
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.
Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L1_K0_SPA doi:10.48322/1jyx-5h51
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
Status of SOPA Instrument 1991-080:  Operating normally as of 01-Feb-1993
with the following exception.  Detector D1 on Telescope 2 is becoming noisy.
This affects proton and ion data from that telescope.  Bad data is disabled 
thru software in the ground processing and is NOT averaged into the Key 
parameter data.  Therefore, the parameters given are good but do not cover 
the same percentage of the sky.
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992
Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993
Modified proton  summation to eliminate noisy channel.
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L4_K0_MPA doi:10.48322/8y0b-0s77
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.
Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L4_K0_SPA doi:10.48322/abg8-2403
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
Status of SOPA Instrument 1994-084:  Operating normally as of 01-Jan-1996
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992
Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993
Modified proton summation to eliminate noisy channel.
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L7_H0_MPA doi:10.48322/2hyb-ms72
Description
No TEXT global attribute value.
Modification History
Created OCT 1998
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L7_K0_MPA doi:10.48322/pb5s-re17
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.
Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L7_K0_SPA doi:10.48322/51vv-e118
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
Status of SOPA Instrument LANL-97A:  Operating normally as of 01-Jul-1997
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992
Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993
Modified proton summation to eliminate noisy channel.
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L9_H0_MPA doi:10.48322/7d0a-cf96
Description
No TEXT global attribute value.
Modification History
Created OCT 1998
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L9_K0_MPA doi:10.48322/jv8m-ra10
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.
Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
L9_K0_SPA doi:10.48322/7xdy-y825
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
Status of SOPA Instrument 1989-046:  Operating normally as of 01-Feb-1993
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992
Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993
Data reduction software updated.  Temperature and 
Density algorithms implemented  15-dec-1993
Repaired some errors in the skeleton table 21-Feb-1995
Implemented updated algorithm for calculating Electron and Proton densities
 and temperatures  21-Feb-1995
 removed contribution of noisy detectors and updated text.
Dataset in CDAWeb
Data Access Code Examples written in Python and IDL®.
Back to top
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