HDF4 file: 32 data descriptors
library version = "HDF Version 4.2 Release 13, June 24, 2017"
data description = (text block)
| The file 'cris_level2_data_Bartels.h' is shown below, it was used to create the data in the Vgroup named 'VG_CRIS_data_Bartels'.
| 
| /* Id: cris_level2_data_Bartels.h,v 1.1 2000/08/01 23:43:00 asc Exp $ */
| 
| #include "hdfi.h"
| #include "cris_sizes.h"
| 
| struct CRIS_data_Bartels {
| 
|   /* UT time at the start of the periods */
|   int32   year;                         /* integer year */
|   int32   day;                          /* integer day of year */
|   int32   hr;                           /* hour of day */
|   int32   min;                          /* min of hour */
|   float32 sec;                          /* seconds */
|   float64 fp_year;                      /* floating point year */
|   float64 fp_doy;                       /* floating point Day of YearDOY */
|   float64 ACEepoch;                     /* UT time in sec since 1/1/96 */
| 
|   float32 flux_B[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_C[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_N[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_O[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_F[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Ne[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Na[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Mg[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Al[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Si[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_P[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_S[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Cl[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Ar[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_K[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Ca[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Sc[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Ti[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_V[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Cr[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Mn[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Fe[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Co[NUMBER_OF_ENERGY_LEVELS];
|   float32 flux_Ni[NUMBER_OF_ENERGY_LEVELS];
| 
|   float32 cnt_B[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_C[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_N[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_O[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_F[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Ne[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Na[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Mg[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Al[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Si[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_P[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_S[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Cl[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Ar[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_K[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Ca[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Sc[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Ti[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_V[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Cr[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Mn[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Fe[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Co[NUMBER_OF_ENERGY_LEVELS];
|   float32 cnt_Ni[NUMBER_OF_ENERGY_LEVELS];
| 
|   float32 livetime;
| 
| };
data description = (text block)
| The file 'cris_level2_factors_energy_levels.h' is shown below, it was used to create the data in the Vgroup named 'VG_CRIS_factors_energy_levels'.
| 
| /* Id: cris_level2_factors_energy_levels.h,v 1.1 2000/08/01 23:49:14 asc Exp $ */
| 
| #include "hdfi.h"
| #include "cris_sizes.h"
| 
| struct CRIS_factors_energy_levels {
| 
|   uint8   z_number;
|   float32 energy_min[NUMBER_OF_ENERGY_LEVELS];
|   float32 energy_max[NUMBER_OF_ENERGY_LEVELS];
|   float32 geo_factor[NUMBER_OF_ENERGY_LEVELS];
|   float32 spallation[NUMBER_OF_ENERGY_LEVELS];
|   float32 SOFT[NUMBER_OF_ENERGY_LEVELS];
| 
| };
file description = (text block)
| Created by the ACE Science Center (ASC) --
| ACE Science Center Level 2 Software Version:  1.5
| ACE Science Center Processing Date/Time: Sat Aug 15 08:50:49 2026 PDT
| For more info email us at: asc@srl.caltech.edu
| 
| Note: There are CRIS team written release notes presented in the
|       annotation section under Release Notes. These should be read.
| 
| For each Bartels Rotation (27.000 day periods):
| 
| 	Type of File		Number of Records
| 	-------------		-----------------
| 	1 hour			648
| 	1 day			27
| 	1 Bartels		1
| 
| The fluxes for the shortest time periods (256 sec for abundant species and 1024 sec
| for rare species) are calculated as follows:
| 
| 	flux = abundance * factor
| 		in units of particles/(cm^2*Sr*sec*Mev/nucleon)
| 	where
| 
| 	   abundance = counts in time period / livetime
| 
| 	   factor = 1 / ( (Energy Max - Energy Min) * (seconds in time period) *
| 		 Geometry Factor * Spallation * SOFT )
| 
| 	   counts = the total number of events during the timing period and is
| 		    unitless; from these counts, the fractional uncertainty
| 		    (0 to 1) can be calculated as 1/sqrt(counts) or the flux
| 		    uncetrainty can be calculated as flux/sqrt(counts)
| 
|    where
| 
| 	livetime = fraction of the time period that the instrument was
| 		   ready to collect data.
| 
| 	Energy Max - Energy Min = the energy range covered in MeV/nucleon
| 
| 	Geometry Factor = determined by Monte Carlo estimation in cm^2*Sr
| 
| 	Spallation = the fraction of particles expected to remain after
| 	             spallation in the detector elements (unitless).
| 
| 	SOFT = the efficiency of SOFT to recognize a particle trajectory
| 	       (unitless).
| 
| For the longer time periods (1hr, 1day, and Bartels rotation), they are averaged as:
| 
| 	Average = Sum(flux)/(Number of samples)
| 
| over the "good fluxes" during the period.
| 
| This data is for an acceptance angle of 30 degrees.
| 
| The timing data at the start of the integration period in Universal Time (UT)
| is:
| 	year	-	int32 year
| 	day	-	int32 day of year
| 	hr	-	int32 hour of day
| 	min	-	int32 minute of hour
| 	sec	-	float32 seconds (accurate to millisec)
| 	fp_year -       float64 fractional year
| 	fp_doy	-	float64 fractional day of year
| 	ACEepoch-	float64 ACE epoch time in seconds since Jan 1, 1996
| 			at 0hr UT
| 
| The average fluxes for N=7 energy ranges are listed as float32. The Energy
| Ranges (MeV/nucleon) for each element and their factors components are
| listed in a separate annotation.
| 
| The fluxes are:
|  Z number				   	          Original Designation
|    5	flux_B	- B flux for N energy ranges in			rare
| 			particles/(cm^2*Sr*sec*Mev/nucleon)
|    6	flux_C	- C flux					abundant
|    7	flux_N	- N flux					abundant
|    8	flux_O	- O flux					abundant
|    9	flux_F	- F flux					rare
|   10	flux_Ne	- Ne flux					abundant
|   11	flux_Na	- Na flux					rare
|   12	flux_Mg	- Mg flux					abundant
|   13	flux_Al	- Al flux					rare
|   14	flux_Si	- Si flux					abundant
|   15	flux_P	- P flux					rare
|   16	flux_S	- S flux					abundant
|   17	flux_Cl	- Cl flux					rare
|   18	flux_Ar	- Ar flux					rare
|   19	flux_K	- K flux					rare
|   20	flux_Ca	- Ca flux					rare
|   21	flux_Sc	- Sc flux					rare
|   22	flux_Ti	- Ti flux					rare
|   23	flux_V	- V flux					rare
|   24	flux_Cr	- Cr flux					rare
|   25	flux_Mn	- Mn flux					rare
|   26	flux_Fe	- Fe flux					abundant
|   27	flux_Co	- Co flux					rare
|   28	flux_Ni	- Ni flux					rare
| 
| The counts are:
| 	cnt_B   - B counts for the N energy ranges
| 	cnt_C	- C counts
| 	cnt_N	- N counts
| 	cnt_O	- O counts
| 	cnt_F	- F counts
| 	cnt_Ne	- Ne counts
| 	cnt_Na	- Na counts
| 	cnt_Mg	- Mg counts
| 	cnt_Al	- Al counts
| 	cnt_Si	- Si counts
| 	cnt_P	- P counts
| 	cnt_S	- S counts
| 	cnt_Cl	- Cl counts
| 	cnt_Ar	- Ar counts
| 	cnt_K	- K counts
| 	cnt_Ca	- Ca counts
| 	cnt_Sc	- Sc counts
| 	cnt_Ti	- Ti counts
| 	cnt_V	- V counts
| 	cnt_Cr	- Cr counts
| 	cnt_Mn	- Mn counts
| 	cnt_Fe	- Fe counts
| 	cnt_Co	- Co counts
| 	cnt_Ni	- Ni counts
| 
| 	livetime - The fraction of the nominal timing period (i.e. 1 hour,
| 		   1 day, or 27 day period) during which the instrument was
| 		   collecting data.
file description = (text block)
| CRIS Instrument team contact:
| 		  Rick Leske
| 	Phone:    626 395 8400
| 	Org:      California Institute of Technology
| 		  Pasadena, CA 91125
| 	Email:    ral@srl.caltech.edu
| 
| 	CRIS Co-Investigator:
| 		Christina Cohen
| 	Phone:	626-395-6614
| 	Org:	California Institute of Technology
| 	City:	Pasadena, CA 91125
| 	Email:	cohen@srl.caltech.edu
file description = (text block)
| CRIS Factors File
|                Energy Range   Recommended    Geometry                              Spallation
|      Energy   (MeV/nucleon)    Mid-Point      Factor       SOFT      Spallation    Correction
|  Z    Level   Lower   Upper    of Erange    (cm^2*sr)   Efficiency   Correction   Uncertainty
| --   ------   -----   -----   -----------   ---------   ----------   ----------   -----------
|  5      2      51.4    65.8       59.6        152.0        0.959        0.955        0.005
|  5      3      67.3    90.4       79.7        154.0        0.944        0.929        0.007
|  5      4      91.5   110.6      102.0        143.6        0.925        0.895        0.011
|  5      5     111.6   128.4      121.1        135.8        0.905        0.863        0.015
|  5      6     129.2   144.6      138.2        126.0        0.887        0.832        0.019
|  5      7     145.3   159.4      154.0        118.4        0.871        0.802        0.022
|  5      8     160.2   173.7      168.6        119.6        0.855        0.773        0.026
|  6      2      59.0    75.6       68.3        151.9        0.967        0.953        0.005
|  6      3      77.2   103.8       91.5        153.9        0.960        0.926        0.008
|  6      4     105.1   127.3      117.3        143.5        0.951        0.891        0.012
|  6      5     128.3   147.9      139.3        135.7        0.941        0.857        0.016
|  6      6     148.8   166.6      159.1        125.9        0.931        0.825        0.019
|  6      7     167.4   183.9      177.4        118.3        0.922        0.794        0.023
|  6      8     184.8   200.4      194.5        119.5        0.913        0.764        0.027
|  7      2      63.2    81.0       73.3        152.0        0.973        0.949        0.005
|  7      3      82.8   111.4       98.1        154.0        0.968        0.920        0.008
|  7      4     112.7   136.6      125.9        143.5        0.963        0.883        0.013
|  7      5     137.7   158.8      149.6        135.7        0.959        0.847        0.017
|  7      6     159.8   179.0      171.0        126.0        0.954        0.813        0.021
|  7      7     179.9   197.6      190.7        118.3        0.949        0.781        0.025
|  7      8     198.6   215.5      209.2        119.6        0.945        0.750        0.029
|  8      2      69.4    89.0       80.4        151.9        0.976        0.947        0.005
|  8      3      91.0   122.5      107.8        153.9        0.973        0.917        0.009
|  8      4     124.0   150.3      138.4        143.5        0.969        0.878        0.013
|  8      5     151.6   174.9      164.7        135.7        0.966        0.842        0.017
|  8      6     176.0   197.3      188.4        125.9        0.963        0.807        0.022
|  8      7     198.3   218.0      210.3        118.3        0.961        0.773        0.026
|  8      8     219.1   237.9      230.8        119.5        0.958        0.741        0.030
|  9      2      72.0    92.4       83.5        151.9        0.980        0.943        0.006
|  9      3      94.4   127.2      112.0        153.9        0.976        0.911        0.009
|  9      4     128.8   156.2      143.8        143.5        0.973        0.870        0.014
|  9      5     157.5   181.8      171.1        135.7        0.971        0.832        0.019
|  9      6     182.9   205.1      195.9        125.9        0.969        0.795        0.023
|  9      7     206.2   226.8      218.7        118.2        0.967        0.760        0.028
|  9      8     227.9   247.5      240.0        119.5        0.966        0.726        0.033
| 10      2      77.1    99.0       89.5        152.0        0.983        0.940        0.006
| 10      3     101.2   136.4      120.1        154.1        0.979        0.908        0.010
| 10      4     138.1   167.6      154.4        143.6        0.976        0.866        0.015
| 10      5     169.1   195.2      183.9        135.8        0.974        0.826        0.019
| 10      6     196.5   220.4      210.6        126.0        0.972        0.788        0.024
| 10      7     221.6   243.8      235.3        118.4        0.971        0.752        0.029
| 10      8     245.0   266.3      258.4        119.6        0.970        0.718        0.034
| 11      2      81.0   104.1       94.0        151.9        0.985        0.938        0.006
| 11      3     106.4   143.5      126.2        153.9        0.982        0.904        0.010
| 11      4     145.3   176.5      162.4        143.5        0.979        0.860        0.015
| 11      5     178.0   205.6      193.5        135.7        0.977        0.819        0.020
| 11      6     206.9   232.3      221.7        125.9        0.975        0.780        0.025
| 11      7     233.5   257.0      247.8        118.2        0.974        0.743        0.030
| 11      8     258.4   280.9      272.3        119.5        0.973        0.708        0.035
| 12      2      86.3   110.9      100.2        152.0        0.987        0.936        0.007
| 12      3     113.4   153.1      134.7        154.0        0.984        0.901        0.010
| 12      4     155.0   188.4      173.4        143.5        0.981        0.857        0.016
| 12      5     190.1   219.7      206.8        135.7        0.979        0.815        0.021
| 12      6     221.1   248.4      237.1        125.9        0.978        0.775        0.026
| 12      7     249.7   275.0      265.2        118.3        0.977        0.737        0.031
| 12      8     276.4   300.7      291.5        119.6        0.976        0.701        0.036
| 13      2      89.4   115.0      103.8        151.9        0.989        0.933        0.007
| 13      3     117.5   158.8      139.6        153.9        0.986        0.897        0.011
| 13      4     160.8   195.5      179.8        143.5        0.983        0.851        0.016
| 13      5     197.2   228.1      214.5        135.7        0.981        0.808        0.022
| 13      6     229.5   257.9      246.1        125.9        0.980        0.767        0.027
| 13      7     259.2   285.6      275.3        118.3        0.979        0.728        0.032
| 13      8     287.1   312.4      302.8        119.5        0.978        0.691        0.038
| 14      2      94.8   121.9      110.1        151.9        0.990        0.932        0.007
| 14      3     124.7   168.6      148.2        153.9        0.988        0.895        0.011
| 14      4     170.7   207.8      191.1        143.5        0.985        0.848        0.017
| 14      5     209.6   242.6      228.1        135.7        0.983        0.804        0.022
| 14      6     244.1   274.5      261.8        125.9        0.982        0.763        0.027
| 14      7     275.9   304.2      293.1        118.3        0.981        0.724        0.033
| 14      8     305.7   332.9      322.6        119.5        0.980        0.686        0.038
| 15      2      97.1   124.9      112.7        151.9        0.991        0.929        0.007
| 15      3     127.7   172.8      151.8        153.9        0.989        0.891        0.012
| 15      4     175.0   213.0      195.9        143.5        0.987        0.843        0.017
| 15      5     214.9   248.8      233.9        135.7        0.985        0.797        0.023
| 15      6     250.4   281.6      268.6        125.9        0.984        0.754        0.029
| 15      7     283.1   312.2      300.8        118.2        0.983        0.714        0.034
| 15      8     313.8   341.7      331.1        119.5        0.982        0.676        0.040
| 16      2     101.6   130.8      118.2        152.2        0.993        0.928        0.008
| 16      3     133.7   181.2      159.4        154.2        0.991        0.889        0.012
| 16      4     183.4   223.5      205.8        143.7        0.989        0.840        0.018
| 16      5     225.4   261.2      245.9        135.9        0.988        0.794        0.023
| 16      6     262.8   295.8      282.5        126.1        0.986        0.751        0.029
| 16      7     297.3   328.1      316.6        118.5        0.985        0.710        0.035
| 16      8     329.8   359.3      348.7        119.7        0.985        0.671        0.041
| 17      2     103.2   133.0      120.2        152.2        0.994        0.925        0.008
| 17      3     136.0   184.3      162.1        154.2        0.992        0.885        0.012
| 17      4     186.6   227.4      209.4        143.7        0.991        0.834        0.018
| 17      5     229.4   265.8      250.3        135.9        0.989        0.787        0.024
| 17      6     267.5   301.1      287.7        126.1        0.988        0.742        0.030
| 17      7     302.7   334.0      322.4        118.5        0.987        0.700        0.036
| 17      8     335.8   365.9      355.1        119.8        0.987        0.660        0.042
| 18      2     107.7   138.8      125.0        151.7        0.992        0.922        0.008
| 18      3     141.9   192.4      168.8        153.7        0.991        0.881        0.013
| 18      4     194.9   237.7      218.1        143.3        0.989        0.830        0.019
| 18      5     239.7   278.0      260.9        135.5        0.988        0.782        0.025
| 18      6     279.8   315.1      300.0        125.7        0.987        0.737        0.031
| 18      7     316.7   349.7      336.4        118.1        0.987        0.694        0.037
| 18      8     351.6   383.3      370.8        119.4        0.986        0.654        0.043
| 19      2     110.0   141.8      127.9        152.0        0.994        0.920        0.008
| 19      3     145.0   196.8      172.8        153.9        0.993        0.878        0.013
| 19      4     199.3   243.1      223.4        143.5        0.991        0.826        0.019
| 19      5     245.3   284.5      267.4        135.7        0.990        0.776        0.026
| 19      6     286.3   322.5      307.5        125.9        0.989        0.730        0.032
| 19      7     324.2   358.1      344.9        118.3        0.989        0.687        0.038
| 19      8     360.0   392.6      380.3        119.5        0.988        0.646        0.045
| 20      2     113.3   146.2      131.6        151.7        0.993        0.917        0.009
| 20      3     149.5   203.1      177.9        153.6        0.992        0.874        0.013
| 20      4     205.6   251.0      230.1        143.2        0.991        0.821        0.020
| 20      5     253.2   293.9      275.6        135.4        0.990        0.771        0.026
| 20      6     295.8   333.3      317.1        125.7        0.989        0.724        0.033
| 20      7     335.1   370.2      355.9        118.0        0.988        0.681        0.039
| 20      8     372.2   406.0      392.4        119.3        0.988        0.639        0.046
| 21      2     114.7   148.1      133.5        151.9        0.995        0.915        0.009
| 21      3     151.4   205.8      180.5        153.9        0.994        0.871        0.014
| 21      4     208.4   254.4      233.7        143.5        0.993        0.817        0.020
| 21      5     256.7   297.9      279.9        135.7        0.992        0.765        0.027
| 21      6     299.9   338.0      322.2        125.9        0.991        0.718        0.034
| 21      7     339.8   375.5      361.6        118.2        0.991        0.673        0.040
| 21      8     377.5   411.9      398.8        119.5        0.990        0.631        0.047
| 22      2     117.8   152.1      137.1        152.0        0.995        0.913        0.009
| 22      3     155.5   211.5      185.5        153.9        0.994        0.869        0.014
| 22      4     214.1   261.6      240.3        143.5        0.993        0.813        0.021
| 22      5     263.9   306.5      287.9        135.7        0.993        0.761        0.028
| 22      6     308.5   347.9      331.6        125.9        0.992        0.713        0.034
| 22      7     349.7   386.6      372.3        118.3        0.991        0.667        0.041
| 22      8     388.7   424.2      410.8        119.6        0.991        0.625        0.048
| 23      2     120.2   155.3      139.9        152.0        0.995        0.911        0.009
| 23      3     158.8   216.0      189.5        153.9        0.994        0.866        0.015
| 23      4     218.8   267.4      245.5        143.5        0.994        0.809        0.021
| 23      5     269.8   313.4      294.3        135.7        0.993        0.756        0.028
| 23      6     315.4   355.8      339.1        125.9        0.993        0.707        0.035
| 23      7     357.7   395.5      380.8        118.3        0.992        0.661        0.042
| 23      8     397.6   434.1      420.3        119.5        0.992        0.618        0.049
| 24      2     123.4   159.6      144.0        152.2        0.996        0.910        0.010
| 24      3     163.2   222.2      195.1        154.2        0.996        0.864        0.015
| 24      4     225.0   275.2      253.0        143.7        0.995        0.807        0.022
| 24      5     277.6   322.6      303.5        135.9        0.994        0.753        0.029
| 24      6     324.8   366.5      349.8        126.1        0.994        0.703        0.036
| 24      7     368.4   407.6      393.0        118.5        0.994        0.657        0.043
| 24      8     409.8   447.5      434.0        119.8        0.993        0.614        0.050
| 25      2     126.0   163.0      146.8        152.0        0.995        0.907        0.010
| 25      3     166.7   227.0      199.1        153.9        0.995        0.861        0.015
| 25      4     230.0   281.3      258.3        143.5        0.994        0.802        0.022
| 25      5     283.9   330.0      309.9        135.7        0.994        0.748        0.029
| 25      6     332.2   375.0      357.3        125.9        0.993        0.698        0.037
| 25      7     377.0   417.2      401.6        118.3        0.993        0.651        0.044
| 25      8     419.4   458.2      443.5        119.5        0.993        0.607        0.051
| 26      2     129.1   167.0      150.4        152.0        0.995        0.906        0.010
| 26      3     170.8   232.9      204.1        153.9        0.995        0.859        0.015
| 26      4     235.9   288.7      265.0        143.5        0.994        0.799        0.023
| 26      5     291.3   338.9      318.1        135.7        0.994        0.744        0.030
| 26      6     341.1   385.2      366.9        125.9        0.994        0.693        0.037
| 26      7     387.3   428.7      412.6        118.3        0.994        0.646        0.045
| 26      8     431.0   471.0      455.9        119.5        0.993        0.602        0.052
| 27      2     131.7   170.6      153.6        152.0        0.995        0.904        0.010
| 27      3     174.5   238.0      208.5        153.9        0.995        0.856        0.016
| 27      4     241.0   295.2      270.9        143.5        0.995        0.796        0.023
| 27      5     297.9   346.6      325.3        135.7        0.994        0.740        0.031
| 27      6     348.9   394.1      375.4        125.9        0.994        0.689        0.038
| 27      7     396.3   438.8      422.3        118.3        0.994        0.641        0.045
| 27      8     441.1   482.2      466.7        119.5        0.994        0.596        0.053
| 28      2     136.2   176.5      158.9        152.0        0.995        0.904        0.010
| 28      3     180.5   246.4      215.9        153.9        0.995        0.855        0.016
| 28      4     249.6   305.9      280.7        143.5        0.995        0.795        0.023
| 28      5     308.7   359.4      337.3        135.7        0.995        0.739        0.031
| 28      6     361.8   408.9      389.5        125.9        0.994        0.687        0.038
| 28      7     411.2   455.5      438.4        118.3        0.994        0.639        0.046
| 28      8     458.0   500.8      484.7        119.5        0.994        0.595        0.053
file description = (text block)
| CRIS Level 2 Data Release Notes
| =========================================================================
| 
| January 23, 2013  Kelly Lave
| REANALYSIS OF THE FULL CRIS DATASET
| 
| The CRIS Level 2 data product has been re-evaluated following changes made to
| the data cuts and the calculation of the geometry factors and SOFT hodoscope
| efficiencies.  Bugs in the positioning and thicknesses of the silicon detector
| stacks and the calculation of the depth of incident particles have been
| corrected.  This resulted in a small change in the geometry factors (less than
| ~1%).  Note that the geometry factors tabulated for the user are slightly
| different for each species in a given energy level.  This is expected since we
| first calculate the differential geometry factor per unit energy and then
| integrate over the energies of the particles stopping in the given energy
| level.  The isotopic composition used for this calculation comes from the
| values posted in the contributed CRIS level 3 data product
| (www.srl.caltech.edu/ACE/ASC/DATA/level3/cris/isotopic_composition.html). The
| tabulated elemental geometry factors are a weighted average of the isotopic
| geometry factors.
| 
| The corrections described above also change the number of events accepted in
| each energy level.  For abundant species (i.e. carbon, oxygen, silicon, and
| iron) the number of events change by less than ~1%; rarer species (i.e.
| phosphorus, chlorine, and scandium) changed by less than ~3%; cobalt, which
| has limited statistics, changed by less than ~5%.
| 
| The calculation of the SOFT efficiencies now implements the work of de Nolfo,
| et. al (2006).  These efficiencies are parameterized by the energy loss in
| silicon at the top of the instrument for particles stopping in each of the
| four stacks of silicon detectors; they have been reproduced in Lave (2012a,
| 2012b).  The boron efficiencies change by up to 1.5%, while heavier species
| change by less than 0.7%; the heaviest species, such as iron, change by less
| than 0.2%.
| 
| The available documentation
| (www.srl.caltech.edu/ACE/ASC/DATA/level2/cris/cris_factors.txt) now includes
| additional information previously unavailable.  In addition to the energy
| bands, recommended central energies, and geometry factors, we now include the
| SOFT efficiencies, spallation correction factors, and the uncertainties on the
| spallation factors.  THIS NEW FACTORS FILE SHOULD BE USED WITH THE NEW LEVEL 2
| DATA!  The uncertainties on the spallation correction factors are determined
| by assuming a 10% uncertainty on the total interaction cross sections.  Note
| that the spallation factors assume that all particles interacting in the CRIS
| instrument are identified and removed from the analysis; although there is
| reasonable certainty that the efficiency of rejection is high, this has not
| yet been confirmed.
| 
| The appropriate systematic uncertainties on the CRIS intensities should be
| calculated for each charge and energy bin.  Combine in quadrature the
| contributions due to the geometry factors (2%), the SOFT efficiencies (2%),
| and the spallation (given by the absolute uncertainties in the data file
| discussed above).
| 
| For supplemental information regarding the calculation of the CRIS
| intensities, please refer to George, et al. (2009) and Lave (2012a, 2012b).
| 
| References:
| G. A. de Nolfo, et. al. Adv. Sp. Res., Vol. 38, pg 1558, 2006.
| J. S. George, et al. ApJ 698, pg 1666, 2009.
| 
| K. A. Lave.  "The Interstellar Transport of Galactic Cosmic
| Rays", Ph. D. Thesis, Washington University in St. Louis,
| http://openscholarship.wustl.edu/etd/707, 2012a.
| 
| K. A. Lave.  Thesis Erratum,
| www.srl.caltech.edu/ACE/ASC/DATA/level3/cris/Erratum_11-20-122.pdf, 2012b.
| 
| 
| 
| 
| - Apr 2, 2010 Rick Leske
|   NEW CRIS Level 2 Data
| 
| The CRIS Team has re-evaluated the production of CRIS Level 2 data,
| implementing several changes that were incorporated in the analysis
| presented in George et al., ApJ 698, 1666 (2009).  These include
| revisions to the hodoscope grammage, interaction probabilities, and
| data cuts and geometry factors for events stopping deep in the
| instrument.  In addition, a bug in the maps of the SOFT hodoscope has
| been repaired, slightly changing the calculation of trajectories, and
| the parsing of the data telemetry stream has been made more robust,
| which results in the recovery of a small number (~0.1%) of additional
| events.  The overall effect of these changes is typically to reduce the
| absolute intensities by a small amount, by up to a few percent.  Together
| these changes have some effect on the width and centers of the CRIS
| energy bins; PLEASE USE THE NEW ENERGY VALUES (available at
| http://www.srl.caltech.edu/ACE/ASC/DATA/level2/cris/cris_energy_bands.txt)
| WITH THESE NEW DATA!
| 
| 
| ***CAUTION*** CRIS DATA ARE OUT OF CALIBRATION BETWEEN 28 AUGUST 1997
| AND 4 DECEMBER 1997.  Early in the mission the camera discriminator
| in the SOFT hodoscope was adjusted several times.  Between 28 Aug and
| 4 Dec 1997 the discriminator settings were not optimal, resulting in
| a bias against heavily-ionizing particles in the hodoscope.  For species
| below about Si (Z=14) we do not notice any problems, but the intensities
| reported in the CRIS level 2 data (both in this new release and in all
| previous versions) are too low during this period for heavier species,
| by ~10% for Fe (Z=26) to as much as ~30% for Ni (Z=28).  This fact was
| overlooked in the George et al. paper cited above and will be addressed
| in an upcoming erratum.  We are working to determine the appropriate
| correction factors and will implement them in a future level 2 release
| when they are available.
| 
| =========================================================================
| - Mar 3, 2010 Rick Leske
|   Unintended Data Change
| 
| The CRIS Team has re-evaluated the production of CRIS Level 2 data,
| implementing several changes that were incorporated in the analysis
| presented in George et al., ApJ 698, 1666 (2009).  These include
| revisions to the hodoscope grammage, interaction probabilities, and
| data cuts and geometry factors for events stopping deep in the
| instrument.  In addition, a bug in the maps of the SOFT hodoscope has
| been repaired, slightly changing the calculation of trajectories, and
| the parsing of the data telemetry stream has been made more robust,
| which results in the recovery of a small number (~0.1%) of additional
| events.  The overall effect of these changes is typically to reduce the
| absolute intensities by a small amount, by up to a few percent.  At
| present we are evaluating the effects of these changes on our energy
| bins (which are expected to be at the few percent level), and once
| this is completed in a few weeks we will release the new data.
| 
| Unfortunately, test files using this new analysis were inadvertently
| placed on the CRIS level 2 site on Feb 24, 2010, 2:40pm PST, replacing
| the older files there; also data from Bartels Rotations 2407 and 2408
| were generated using the new analysis.  CRIS DATA FILES DOWNLOADED
| BETWEEN FEB 24 and MAR 3 2010, OR ANYTHING FROM BR 2407 DOWNLOADED
| PRIOR TO MAR 3, SHOULD NOT BE USED WITHOUT THE APPROPRIATE CHANGES TO
| THE ENERGY BINS, WHICH WE ARE STILL WORKING ON.  For the time being, we
| are restoring the old files to the site until we have finished
| evaluating the new ones.
| 
| We thank the users who called this issue to our attention, and we
| apologize for any inconvenience this may have caused.
| 
| =========================================================================
| - Nov 7, 2003 Rick Leske
|   Energy Band Information Update
| 
| Up until now the energy band info included only the minimum energy and
| maximum energy for each element for each detector range.  These values
| are for the characteristic energy band which is defined as the minimum
| and maximum energy required to stop in each range at the median zenith
| angle for that range.  The incorporation of this characteristic energy
| band into the flux and geometry factor calculations is described in more
| detail below in the entry for Level 2 Software, Version 1.0   July 26,
| 1999.  None of the geometry factors, energy intervals, or fluxes have
| changed.  However, we now add to the energy band documentation file a
| recommended central energy point, which is defined as the arithmetic
| average of the (isotope-weighted) absolute min and max calculated energies
| for each range.  Note that this is NOT the average of the upper and lower
| values of the characteristic energy band.
| 
| =========================================================================
| - Aug 16, 2002, Jeff George
|   Quiet Time Criteria Update
| 
| The CRIS quiet time criteria defined below for Level 2 data was found
| to allow periods of solar activity in which SOFT is partially
| saturated with triggers from low energy particles.  The criteria
| removed periods in which the SOFT trigger rate was essentially zero
| but did not remove the transitions from normal operation to the fully
| saturated state.  This became very apparent during the July 22, 2002
| SEP event in which the particle fluxes kept the SOFT trigger rate in
| this intermediate state for several days.  These periods need to be
| removed as the instrument is not operating in a nominal state.
| 
| We have corrected the problem by adding one additional test to the
| quiet time criteria for basic instrument operation.  Now the average
| of the four E1 detector rates is required to be below 300 Hz.  This
| has no effect on normal operation when the rate is typically 10-20
| Hz.  The 300 Hz level corresponds well to the point at which the SOFT (0 AND
| 1) trigger rate begins to saturate.  The new criterion rejects periods
| with normal SOFT rates but high E1 rates, exactly the transition
| conditions that were a problem.  The new condition removes a total of
| 5.8 days (0.3%) from the full mission to date.  Nearly 2 days
| corresponds to the July 22, 2002 event alone.  All of the other
| rejected periods come from short transitions of a few hours each
| scattered throughout the mission.  There is no effect on the data for
| periods outside these transitions during SEP events.
| 
| All CRIS Level 2 data available from the ACE Science Center was
| reprocessed using this additional quiet time criterion on Aug 16,
| 2002.  Data is currently reported through Bartels Rotation 2306.
| 
| 
| 
| =========================================================================
| - Level 2 Software, Version 2.0
|   (updated Mar 20, 2002 by Jeff George)
|   (all CRIS Level 2 data available from the ACE Science Center was
|    reprocessed using this new code on Mar 21, 2002)
| 
| This new version of the Level 2 processing software is a complete
| rewrite of Nathan Yanasak's original code to make the procedure much
| more modular, efficient, and readable.  It corrects several minor
| errors in matching event and rate data.  We also took advantage of the
| need for reprocessing the data to implement a new, objective criterion
| for selecting periods during which the instrument is operating at full
| performance and there is little possibility that the galactic cosmic
| ray spectra are contaminated by solar energetic particle events.
| 
| The new software package processes a single Bartels rotation at a
| time, improving the speed and reducing the memory requirements. A Perl
| script automatically extracts event, rate, and housekeeping data.  All
| CRIS data are reported to the ground in 256 second instrument cycles
| stamped with a spacecraft clock time for each cycle.  In keeping with
| this format, the new code works with an efficient mask for selecting
| valid data periods on a cycle by cycle basis.  Any mask index which
| cannot be addressed by a valid clock time in the rate data is declared
| missing.  Because rate and event data are physically reported in
| different cycles in the spacecraft telemetry, the index immediately
| following a missing cycle is also rejected.  Instrument performance
| and solar activity criteria flags (described below) are also applied
| directly to the mask array.  A single loop through the mask array
| indices generates fluxes only for known valid periods and applies -999
| fill values for the remainder.  This procedure makes it extremely
| difficult to erroneously report fluxes for invalid periods.
| 
| Data provided to the public will continue to be averaged on hourly,
| daily, and 27-day timescales.  In addition, the factors used to
| calculate the fluxes from the instrument counts remain identical to
| those used in the previous Yanasak code and described in previous
| releases.
| 
|     Instrument Performance and Quiet Time Criteria:
| 
| Data from any given instrument cycle must pass a set of minimum
| criteria to be considered "valid":
|    1)  Spacecraft telemetry frames for both the event and rate data
|        	must exist and have been received without error on the ground.
|    2)  The SOFT multi-channel plate (MCP) high voltage must on and at
| 	normal values.  During high rate periods (i.e., during solar
| 	energetic particle events) the current limits on the SOFT MCP
| 	trip off and the instrument must be manually commanded back on
| 	when the event is over.
|    3)  The SOFT trigger rate (the logical AND of the two trigger
| 	planes)	must not exceed 5kHz.  The SOFT trigger is
| 	edge-detected and at high rates there is so much ambient light
| 	in the fibers that the trigger level generally remains high
| 	and few if any event triggers are generated.
|    4)  The fractional livetime for Z>2 particles must be above 60%.
| 	CRIS livetime is typically over 80% and the instrument is
| 	capable of performing even when the available livetime is
| 	low.  Such periods introduce a large correction to the flux
| 	calculation, however, so we prefer to simply reject them.
| 
| These criteria define the minimum requirements for valid data and
| remove only ~7% of all time since launch. The purpose of the Level 2
| data, however, is to provide a clean sample of galactic cosmic-ray
| data.  As such, we impose an additional tighter restriction on the
| SOFT trigger rate to avoid even the possibility of contamination by
| solar energetic particles.
| 
|    5)  The SOFT trigger rate (logical AND of the two trigger planes)
| 	must not exceed 500Hz.
| 
| Each of these criteria are applied individually to each instrument
| cycle and with 5), remove about 13% of the time in the full
| mission-to-date.   By contrast, the previous code used a very
| conservative and somewhat subjective criterion that rejected entire
| days.  That code rejected ~43% of the full mission data up to this point.
| 
| 
| 	Event and Rate matching errors corrected in this release
| 
| Rate data for a given instrument cycle is physically reported in the
| telemetry for the next instrument cycle.  Because of this, the
| previous Level 2 code version matched events from one spacecraft clock
| timestamp with the fractional livetime reported with the next
| timestamp.  We recently realized that this correction is already being
| made in the Level 1.1 processing where the timestamps for the rate
| data are corrected to match those of the cycle which contains the
| events for which the rates are being reported.  This also affects
| which cycles are rejected due to missing rates.  CRIS data are
| normally quite stable and the rates do not typically vary quickly so
| this is expected to have little impact on the previously reported
| fluxes.  Nevertheless, the error is corrected in this release.
| 
| 
| =========================================================================
| - Level 2 Software, Version 1.3	(updated February 1, 2001 by Nathan Yanasak)
| 
| No major structural changes were made in the V1.2 programs listed above.
| However, two errors in the data processing were discovered.  The first error
| occured as a result of switching from ce1 to ce2 data (see V1.2 discussion).
| A general cut applied to data from CRIS eliminates particles which pass
| close to the outside edges of the active detector region.  The intent of this
| cut is to eliminate particles which exit the detector through the sides.
| During the switch from ce1 to ce2 data, the routine in the data extraction
| software which handles this cut was altered, decreasing the size of the cut.
| The calculated geometry factor assumed the older cut from the V1.0 and V1.1
| data set, which was inappropriate for the new cut in V1.2.  After correcting
| the geometry factor so that it corresponded to a larger active volume in the
| detector, the flux for level 2 data from V1.3 software decreased by
| approximately 4-5%.
| 
| The second error is associated with the calculation of the event median angle.
| Comparison of the median angle calculated in the V1.2 factors.pro program with
| angles calculated by another independent program revealed an error in the V1.2
| code responsible for the angle calculation.  With the error corrected, the new
| values of the median theta are given below:
| 
| instrument range | median theta
| =================================
|        2	 |    20.1
|        3	 |    19.9
|        4 	 |    19.7
|        5         |    19.3
|        6	 |    18.9
|        7	 |    18.9
|        8	 |    18.6
| 
| The increase in the values of median theta give slightly increased average
| values for the corrected energy bands.  This increase depends on the depth of
| the reported energy band in the detector, ranging from ~0% for range 2 to
| ~1.5% for range 8.
| 
| The systematic uncertainties reported above at the end of the section entitled
| "General Information"--15% for low-Z elements and 10% for higher-Z elements--
| need to be re-evaluated in light of the changes which took place in V1.1, V1.2,
| and V1.3 of the level 2 code.  The primary sources of uncertainty in the flux
| calculation for level 2 data are as follows:
| 
| 	1) statistical
| 
| 	2) uncertainty in average energy of a band -- flux data are reported
| 	for an energy band, and the spectra depend on which energy the data
| 	are plotted.
| 
| 	3) geometry factor uncertainties
| 
| 	4) SOFT efficiency
| 
| 	5) correction for fragmentation in the detector -- factors.pro uses the
| 	expression of Westfall et al. (PRC, V19, p1309, 1979) instead of a
| 	more complex, energy-dependent cross-section code.
| 
| The uncertainty for item #2 was estimated in the following manner.  An average
| spectral shape (f=log(flux)~A*log(E)^2+Blog(E)+C) can be found for all species
| by plotting flux data at energies in the center of the energy bands.  Using
| this shape, one can examine how much the flux should change over the range of
| energies in a given band.  Assuming ad hoc that the reported flux value given
| for an energy band Elo < E < Ehi can lie anywhere between Elo+0.25*delE and
| Elo+0.75*dele (here, delE=Ehi-Elo), the largest variation in flux in any given
| energy band is 5%.
| 
| The geometry factor has been verified by three independent codes to a level of
| 5%.  The precision of the factor calculated in factors.pro is statistically
| significant to the level of 1.5%, but 5% should be used as an upper limit at
| the time of this version release.
| 
| The improved SOFT efficiencies for V1.2 and later versions are precise to 3%
| for Z=4 and 2% for other elements.
| 
| Differences between the total fragmentation cross sections from Westfall et al.
| (1979) (used by factors.txt) and measured total cross sections have been
| estimated using the formulae of Tripathi et al. (NASA/TP-1999-209726, 1999).
| The formulae from Tripathi et al. are fine-tuned to match an extensive set of
| cross-section data, and they include an energy dependence as well.  The amount
| of fragmentation depends on the depth at which the cosmic rays stop in CRIS,
| and the depth is also a function of the particle energy.  So, the amount of
| variation between the formulae of Westfall et al. and Tripathi et al. is a
| function of the particle species and energy.  The low-Z and Fe,Ni-group nuclei
| show the largest difference between these formulae (ranging from 0% for
| stopping depths near the top of the CRIS SI detector stacks to 5% at the
| bottom of the stack), and species around Z=11-15 show the least amount of
| difference (<2% over the full range).  To be conservative, we suggest an
| uncertainty of 5% in the fragmentation correction.
| 
| Adding all of the systematic uncertainties listed above in quadrature, we find
| a global uncertainty for level 2 data of ~9% for all elements.
| 
| Data from CRIS during periods of high solar activity are "flagged" with a
| value of -999.9 because the instrument was not designed for optimal
| operation during these condition
| (see http://www.srl.caltech.edu/ACE/ASC/level2/cris_l2desc.html on the ACE
| Science Center website for a full description of the CRIS level 2 data).  These
| periods are the most conservative estimates of days during which CRIS
| performance may be affected.  Currently, the criteria for determining periods
| of high activity are being re-evaluated so that more days can be included in
| the level 2 data.  These criteria will be applied at a future data release and
| documented in the release notes.
| 
| 
| =========================================================================
| - Level 2 Software, Version 1.2	(updated May 22, 2000 by Nathan Yanasak)
| 
| No major structural changes were made in the four V1.1 programs listed above.
| However, three minor changes were made.
| 
| Change #1: Discrepancies between the two different methods for calculating the
| average geometry factor (mentioned above) have been resolved, and the average
| geometry factor calculated by factors.pro has changed to reflect this
| agreement.  The maximum amount of discrepancy between the geometry factor in
| older versions of factors.pro and version 1.2 is a 7.5% increase in the
| corrected geometry factor, and the average amount of discrepancy is
| approximately 6.7%.  Calculation of the median theta for the zenith angle
| described above is dependent on the geometry factor code, and the new values of
| median theta for version 1.2 are presented below:
| 
| instrument range | median theta
| =================================
|        2	 |    18.4
|        3	 |    18.4
|        4 	 |    17.5
|        5         |    16.7
|        6	 |    15.9
|        7	 |    15.4
|        8	 |    14.6
| 
| Change #2: Version 1.2 uses ce2 data as input instead of the ce1 data used as
| input for previous versions.  ce2 data is slightly different from ce1, using a
| different algorithm to determine SOFT trajectories.  The improved algorithm
| results in a higher SOFT efficiency on average for any GCR species
| (~ +1.5% average increase from ce1 data), with much greater efficiency at
| lower Z (~ +18% for Be).  SOFT efficiencies calculated by the version 1.2
| factors.pro are appropriate level 2 data processed from ce2 data.
| 
| Change #3: In our calculation of particle energies, we have switched from an
| older range-energy IDL procedure to a newer one based on Anderson and Ziegler.
| Particle energy values decrease by 1-2% for particles stopping near the top of
| range 2 using the newer method, and the energy values experience a negligible
| decrease for particles stopping deeper within the stack.
| 
| Finally, the IDL procedure eleplot.pro has been replaced by another procedure
| which has two versions with differing names: frsteleplot.pro and
| itereleplot.pro.  The first version, frsteleplot.pro, is identical to
| eleplot.pro and should be used if one wants to reprocess level 2 data from
| the beginning of the mission.  The second version, itereleplot.pro, is similar
| to eleplot.pro, but it uses output from previous runs of frsteleplot.pro or
| itereleplot.pro instead of reprocessing data from the beginning of the mission.
| 
| 
| =========================================================================
| - Level 2 Software, Version 1.1	(updated October 26, 1999 by Nathan Yanasak)
| 
| No significant changes were made in the four V1.0 programs listed above;
| however, a different version of code was used to extract the raw ce1 data which
| acts as an input to the statflux.pro code.  A slight discrepancy concerning the
| coordinates of the detector telescope elements was discovered.  The pre-level
| 2 processing of raw event files makes certain geometric cuts appropriate to
| the geometry factor used for level 2, which serve to eliminate data which
| traverse SOFT near its edge or pass very close to the guard rings in the
| detector telescopes.  Some of these geometric cuts were affected by this
| discrepancy, and a set of positional offsets was applied to correct these in
| pre-level 2 processing.  Consequently, the number of raw events which are
| being processed by statflux.pro has increased by approximately 1.3%, which
| increases the particle fluxes found using V1.0 code by some fraction of this
| 1.3%.  The input section of statflux.pro was altered accordingly to reflect
| this increase.
| 
| 
| =========================================================================
| Level 2 Software, Version 1.0	July 26, 1999
| N. Yanasak
| Programs:
| 	1) statflux.pro
| 	   Language: IDL
| 	   General description: This program applies the data cuts to raw
| 		ce1 data.
| 
| 	2) eleplot.pro
| 	   Language: IDL
| 	   General description: This program associates the data to the
| 		appropriate values of the instrument livetime.
| 
| 	3) lvl2gen.pro
| 	   Language: IDL
| 	   General description: This program is responsible for formatting the
| 		data into the level 2 format and placing it into the
| 		appropriate files.
| 
| 	4) factors.pro
| 	   Language: IDL
| 	   General description: This program calculates the necessary factors
| 		for converting the event rates given in the output files of
| 		lvl2gen.pro into particle differential fluxes (in units of
| 		# of events/(MeV/nuc)/seconds/(cm^2 sr) ).
| 
| General Information:
| 
| 	Software used for the generation of level 2 CRIS data outputs
| data grouped into two categories: more abundance elemental species
| (C,N,O,Ne,Mg,Si,Fe), and species of lesser abundance (all other elements not
| listed, between Z=5-28).  Data for the more abundant species are
| reported for each 256-second window in time, and the less abundant species
| are reported for 1024-second windows.  There are two types of output data
| files, with each type corresponding to one of the two categories described
| above.  Each file holds data reported during one Bartles rotation.
| 
| 	Data are reported as the rate of particles observed to stop in each of
| the 7 instrumental ranges.  These ranges correspond to different vertical
| stopping depths in the instrument.  Because the particle zenith angle for this
| reported data lies between 0 and 30 degrees, a unique vertical depth will give
| a spread in particle stopping energies.  This means that the energy bands which
| characterize particles of a given species stopping in each instrument range
| will overlap in particle energy.  To define characteristic energy bands for
| each instrument range, we have used the minimum and maximum energy required to
| stop in that range at the median zenith angle.  The different median angles for
| each range are as follows:
| 
| instrument range | median theta
| =================================
|        2	 |    18.6
|        3	 |    18.6
|        4 	 |    17.9
|        5         |    17.2
|        6	 |    16.4
|        7	 |    15.9
|        8	 |    15.2
| 
| The differential flux of cosmic rays reported at the level 2 site is inversely
| proportional to the product of the energy band for a given instrumental range
| with the geometry factor appropriate to that band.  A proper calculation of the
| flux requires using the true energy band (with overlapping boundaries) instead
| of the characteristic band for a given instrumental range.  To account for this
| difference, an adjustment was made to the geometry factor for each instrumental
| range to keep the product of the energy band and geometry factor the same.
| 
| 	Data are required to pass a very loose charge consistency cut to
| eliminate possible contamination of less abundant species by abundant species
| which fragment in the instrument and are misidentified.  Charge consistency
| is defined as the number of standard deviations off of the mean value of
| the charge ratios ZEST_LAST/ZEST and ZEST/ZEST_E1 for a particle stopping at a
| particular vertical depth.  Here, ZEST, ZEST_LAST, and ZEST_E1 are event
| charges calculated using different detector combinations to compute dE, E'
| (for a description of particle identification using the dE/dx vs. total E
| method, see Stone, et al, 1998, Space Sci. Rev., 98, 285-356):
| 
| 	ZEST      -- E'=stopping detector, dE=all previous detectors
| 	ZEST_E1   -- E'=second and all subsequent detectors, dE=first detector
| 	ZEST_LAST -- E'=stopping detector, dE=next to last detector
| 
| We applied a charge consistency cut on the data to include events with less
| than 10 standard deviations off of the mean charge ratio value.  Because of
| the presence of dead layers in the instrument telescope elements, events
| stopping fairly close to the top and bottom surfaces of individual detector
| elements will record substantially lesser values of E' for ZEST and ZEST_LAST
| than is actually deposited.  This will cause the mean charge consistency for
| particles stopping near dead layers to change quite rapidly as a function of
| vertical stopping depth.  To simplify the difficulty in identifying particles
| stopping near dead layers, a cut on particles stopping 160 microns from the
| dead layer surfaces was implemented.
| 
| 	To convert the particle rates to fluxes, the level 2 site divides rates
| by the geometry factor and correction factors associated with the efficiency
| of the SOFT hodoscope and the expected amount of loss from fragmentation in
| the stack to yield particle fluxes.  Flux uncertainties reported in the level
| 2 site are based on the number of counts reported for a particular window of
| time.
| 
| 	Additional systematic uncertainties related to these factors must
| also be considered by the level 2 data user who uses version 1.0 data.  The
| average geometry factor for CRIS has been calculated by two independent
| methods, and there is a discrepancy of ~5% between the two for a maximum
| zenith angle of 30 degrees.  In addition, the trigger efficiency of the SOFT
| hodoscope was calculated using two different methods.  The difference in the
| results between the methods is ~5% for elements with higher Z (>10), and for
| elements of lesser charge where the light output of the SOFT varies more
| significantly with dE/dx, the discrepancy is somewhat larger (~10%).
| Considering these systematic discrepancies, we recommend adding an additional
| 10% to the statistical uncertainties of higher Z elements and 15%
| for lower Z elements to reflect the geometry factor and SOFT
| efficiency indeterminancy more accurately.  These systematics will be
| improved in future versions.
data description = (text block)
| The file 'level2_record_doy.h' is shown below, it was used to create the data in the Vgroup named 'VG_level2_record_doy'.
| 
| /* Id: level2_record_doy.h,v 1.1 2000/08/02 00:47:11 asc Exp $ */
| 
| #include "hdfi.h"
| 
| /* record year/DOY association */
| struct level2_record_doy {
| 
|   int32   record_number;             /* record number */
|   int32   year;                      /* integer year */
|   int32   day;                       /* integer day of year */
|   int32   days_jan_1_1996;           /* days since January 1, 1996 UT 0 hr*/
| 
| };
vgroup "VG_CRIS_data_Bartels" class "VG_CRIS_LEVEL2_DATA_BARTELS"
	vdata "CRIS_data_Bartels" class "CRIS data Bartels": fields year, day, hr, min, sec, fp_year, fp_doy, ACEepoch, flux_B, flux_C, flux_N, flux_O, flux_F, flux_Ne, flux_Na, flux_Mg, flux_Al, flux_Si, flux_P, flux_S, flux_Cl, flux_Ar, flux_K, flux_Ca, flux_Sc, flux_Ti, flux_V, flux_Cr, flux_Mn, flux_Fe, flux_Co, flux_Ni, cnt_B, cnt_C, cnt_N, cnt_O, cnt_F, cnt_Ne, cnt_Na, cnt_Mg, cnt_Al, cnt_Si, cnt_P, cnt_S, cnt_Cl, cnt_Ar, cnt_K, cnt_Ca, cnt_Sc, cnt_Ti, cnt_V, cnt_Cr, cnt_Mn, cnt_Fe, cnt_Co, cnt_Ni, livetime; 1 records
vgroup "VG_CRIS_factors_energy_levels" class "VG_CRIS_LEVEL2_FACTORS_ENERGY_LEVELS"
	vdata "CRIS_factors_energy_levels" class "CRIS factors_energy_levels": fields z_number, energy_min, energy_max, geo_factor, spallation, SOFT; 28 records
vgroup "VG_level2_record_doy" class "VG_LEVEL2_RECORD_DOY"
	vdata "level2_record_doy" class "level2_record DOY table": fields record_number, year, day, days_jan_1_1996; 1 records