CXO Project Science:

EPHIN and ACE/EPAM do not sample identical energy bands. The closest overlap is between EPHIN SCP4GM (4.37.8 MeV) and EPAM LEMS30 P8 (1.94.75 MeV). Ideally, one would like to use EPHIN data to help signal potential high fluxes of protons at around 100 keV. Though EPHIN does not have a suitable energy band, the EPAM LEMS30 P3 (0.1120.187 MeV) channel is ideal. Thus, if a correlation can be made between the EPHIN and EPAM channels and a correlation can be made between EPAM P3 and P8 then the potential for EPHIN to predict low energy protons is improved. Here is the data available (many thanks to the Sources):
Instrument  Source  Channel  Energy  Coverage 

ACE/EPAM LEMS30  ACE/ASC  p3  0.1120.187 MeV  970814  990108 
ACE/EPAM LEMS30  ACE/ASC  p8  1.914.75 MeV  970814  990108 
ACE/EPAM LEMS30  ACE RealTime Solar Wind  p3  0.1120.187 MeV  970814  current 
ACE/EPAM LEMS30  Ed Hawkins III, JHU  p8  1.914.75 MeV  990601  990915 
Chandra/EPHIN SCP4GM  Dick Edgar, CXC  scp4gm  4.307.80 MeV  990727  current 
So, we can compare ACE/EPAM LEMS30 P3 to P8 over a 513 day baseline, but with no overlap to Chandra data (first two rows of the above table), and EPAM P8 and P3 to EPHIN SCP4GM over a portion of the Chandra mission, about 52 days to date. (Note: the NOAA realtime data, available at the SEC, includes P3 but does not include P8 and is not a level 2 product).
After scaling by the appropriate geometric factor (0.18 cm^2*str) and energy bandwidth and averaging the EPHIN data over 1 hour intervals to be consistent with the EPAM standard dataset (cts/cm2/s/str/MeV), the light curves look like this (red is EPAM P8 and green is EPHIN SCP4GM):
So there is a correlation there as expected (ignoring EPHIN data near perigee!) but this serves basically as a control since we are comparing similar energy bands. The interesting correlation, if it exists, is between EPHIN SCP4GM and EPAM P3: The pointbypoint correlation, ignoring points in the radiation belts (defined here simply as those with SCP4GM greater than 10 cts/cm2/s/str/MeV) for these two datasets is:
which shows evidence of a trend, perhaps, but Chandra has not been in orbit long enough to obtain a good sample. On the other hand, the pointbypoint correlation for EPAM P3 and EPAM P8, including all data with flux in p8.gt.1, over the period 970814990108 is more promising, as shown below. The best fit is found by fitting a power law to the data and the approximate 1sigma curves are estimated by fitting a normal distribution to the data (in log space) in three slices: p8 between 1.0 and 2.5, between 10 and 20, and between 50 and 100 cts/s/cm2/str/MeV and then plotting a straight line through the resulting +/ 1sigma points. The power law fit to the data is p3 = 355.4*(p8)**0.8
Now, since the correlation is strong between EPAM P8 and EPHIN SCP4GM and the long timeline comparison of EPAM P3 and P8 shows a correlation, it follows that EPHIN SCP4GM and EPAM P3 are, indeed correlated but we need a longer baseline to determine fit parameters with confidence.
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