DATA DESCRIPTION ACE EPAM data These ACE EPAM (Electron, Proton& Alpha Monitor) daily, spin-averaged He fluxes are given in 12 energy windows between 0.443-0.531 and 3.28-3.93 MeV/n. They were prepared and provided by T.P. Armstrong at Fundamental Technologies, LLC, and are accessible, along with equivalent C, O, Ne, Si and Fe fluxes, at http://data.ftecs.com/VHO/VEPO/ace_epam/pha/spectra/. On 2/2/2012, a newly FunTech-reprocessed version of the data, having revised fluxes and energy bin ranges, was swapped into this MSSP interface and into the FTPBrowser interface at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/ace_epam_flux_1d.html. For background, see the ACE EPAM home page at JHU/APL at http://sd-www.jhuapl.edu/ACE/EPAM/ and see the ACE EPAM web pages at FunTech at http://ace.ftecs.com/index.html ACE SIS data These ACE SIS (Solar Isotope Spectrometer; Caltech) hourly He fluxes are given in 8 energy windows between 3.4-4.7 and 28.4-41.2 MeV/n. They are from the "Level 2" data set accessible from the ACE Science Center and from CDAWeb. The L2 data set contains fluxes of 14 elements from Z=2 (He) to Z=28 (Ni). The instrument is described at http://www.srl.caltech.edu/ACE/CRIS_SIS/sis.html The data set is described at http://www.srl.caltech.edu/ACE/ASC/level2/sis_l2desc.html and references therein. ACE ULEIS data The ULEIS (Ultra Low Energy Isotope Spectrometer) on ACE measures ion fluxes over the charge range from He through Ni from about 20 keV/n to 10 MeV/n. The instrument and its diversity of available data products are extensively discussed at http://sd-www.jhuapl.edu/ACE/ULEIS/. Key Investigators are Glenn Mason, Rob Gold and George Ho at JHU/APL. ULEIS Level 2 data consist of hourly and daily averaged fluxes and statistical uncertainties of H, He3, He4, C, O, Ne-S, and Fe. These data have long been accessible from the ACE Science Center at http://www.srl.caltech.edu/ACE/ASC/level2/index.html. Descriptions of the Level 2 data are at http://www.srl.caltech.edu/ACE/ASC/level2/uleis_l2desc.html and updated release notes are at http://www.srl.caltech.edu/ACE/ASC/DATA/level2/uleis_v2/uleis_release_notes The Level 2 hourly fluxes of H (5 energy bands between 0.16 and 7.24 MeV) and He4 (15 energy bands between 0.063 and 8.67 MeV/n) have been taken from ASC for inclusion in the Multi-Source Spectral Plot (MSSP) interface and a companion FTPBrowser interface at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/ace_ule_hr.html. Separately, L2 fluxes of H, He4, C, O, and Fe are taken from ASC for a new high-Z MSSP version now in development and a companion FTPBrowser interface at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/ace_ule_all_hr.html. CAVEAT: depending on flux levels ULEIS spectra above ~1 MeV/nucleon may show turn ups which are background and should be discarded. This effect is stronger when intensities are low. GOES data Hourly fluxes of protons and alpha particles as measured by the NOAA GOES (Geostationary Operational Environmental Satellites) are taken from the NOAA/NGDC site at http://satdat.ngdc.noaa.gov/sem/goes/data/new_avg/. At 6.6 Re, the spacecraft are inside, but near (when on the day side), the Earth's magnetopause, so GOES energetic particle fluxes are representative of fluxes in the nearby interplanetary medium at all but the lowest energies measured. We have taken proton fluxes in 7 energy bins, 0.6-4.0, 4.0-9.0, ... 165-500 MeV, and alpha particle fluxes in 6 energy bins, 4-10, ... 300-500 MeV/n. All channels except the lowest-energy proton channel show little or no magnetospheric signature. As the GOES 8 and 11 data sets are described by NOAA as having the same energy bins, we have created a single data set spanning 1995-2010 from their data. Data up to 2003/168 are from GOES 8, and thereafter from GOES 11. GOES 13 energy bins are described as slightly different, so we have created a single GOES 13 data set that we will extend as new data become available. There is an 8-month overlap between the two data sets in 2010. The full hourly-averaged data sets are available with subset, plot and list functionalities from data set-specific FTPBrowser interfaces at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/goes08_11_hr.html and http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/goes13_hr.html. These interfaces display the energy bin ranges. For inclusion in the Multi-Source Spectral Plot (MSSP) interface (that otherwise includes no magnetospheric fluxes), we exclude the lowest proton energy channel fluxes due to their strong magnetospheric signature. Helios 1&2 E6 data. These data were originally provided to NSSDC by Principal Investigator Horst Kunow, U. Kiel. These are nominally 1-hour resolution differential fluxes, and Poisson uncertainties associated with each, for protons in 4 energy bands (4-13, 13-27, 27-37, 37-51 MeV) plus an integral proton channel (>51 MeV), for alpha particle fluxes and uncertainties in 5 energy bands (2-4, 4-13, 13-27, 27-37, and 37-48 MeV/n) plus an integral channel>48 MeV/n, and finally for electrons in the two energy bands 0.3-0.8 and 0.8-2 MeV. The data are further described at ftp://spdf.gsfc.nasa.gov/pub/data/helios/ helios1/particle/e6_kunow/h-a-cr.txt and references therein. Manipulations carried out on the data to facilitate usage are described at ftp://omniweb.gsfc.nasa.gov/helios1/flux/ helios_e6_flux_descr.txt. Helios 1&2 E7 data. These datasets were recently created by Dr. Nand Lal of the original PI's team (PI: James Trainor, NASA/GSFC) These are 30-min resolution differential fluxes, and uncertainties associated with each, for protons in 7 energy bands (3.4-6.05, 6.05-11.1, 11.1-21.6, 24.52-28.82, 32.0-46.3, 46.3-57.22, 135.2-206.5 MeV), and for alpha particle fluxes and uncertainties in 6 energy bands (3.2-4.98, 4.98-11.50, 11.5-21.6, 24.51-31.12, 31.12-45.53, 45.53-57.53 MeV/n). The data set also includes many additional count rates including two for electrons in the energy bands 2-4 and 4-8 MeV. Creation of a subsetted data set containing just the fluxes and rates mentioned above intended to facilitate usage are described at ftp://omniweb.gsfc.nasa.gov/helios1/flux/ helios_e7_flux_descr.txt. IMP 8 CRNC data (U.Chi./UNH) This data set consists of hourly fluxes of protons, electrons and alpha particles in three species-specific subdirectories, and of hourly count rates of "heavies" in a fourth subdirectory The fluxes are based on count rates pulled to GSFC/SPDF from UNH in 2011 and converted by the equation F = CR / [2.05 * (E2-E1)], where 2.05 is the geometric factor relevant to all the rates and fluxes and E1,E2 are the bounds of the relevant energy band. See ftp://ulysses.sr.unh.edu/WWW/Simpson/IMPData/hourly.html for the UNH-resident version. The count rates at UNH are based on the folding together of telescope coincidence-mode count rates and pulse height analysis data. The data at UNH and at SPDF are ASCII formatted. The data at UNH are in monthly files and at SPDF are in annual files The proton and alpha particle fluxes are each given in 9 energy bands in the 11-95 MeV/n range, and the electron fluxes are given in 0.7- 2.0, 2-12 and 12-50 MeV bands. The "heavies" rates are of both heavy nuclei (CNO>80,<80 MeV/n; Z>8 low and high energy) and of all penetrating particles (including protons with E> 106 MeV). The species-specific subdirectories have readme files that identify the energy bands relevant to each species, as given in the UNH-resident monthly files' headers. The fill value for all fluxes and rates is 9.999E+05 in the SPDF-resident files. IMP 8 GME data These data are based on 30-min PHA-based proton and alpha particle fluxes determined from the IMP 8 GME (Goddard Medium Energy) experiment. Fluxes for every other one of the CDAWeb-accessible 30 proton energy channels, and 21 alpha particle energy channels, are folded into this interface as providing sufficient spectral resolution for our purposes. (CDAWeb is at http://cdaweb.gsfc.nasa.gov/sp_phys if you want to access fluxes for the in-between channels.) Because the dE/dx - E boxes used with pulse height data for deriving fluxes of particles in specific species and energy bands were optimized for energetic solar particle events, quiet time cosmic ray fluxes must be used carefully, especially at the high energy end of the Low Energy Detector range (i.e., ~6-20 MeV/n). For further detail, see the home page of the IMP 8 GME team at http://spdf.gsfc.nasa.gov/imp8_GME/GME_home.html Pioneer 10 &11 CRT The GSFC/UNH Cosmic Ray Telescope (CRT) flown on the Pioneer-10 and -11 spacecraft, and the ~3-300 MeV/n proton and alpha particle flux data made accessible through this multi-source spectral plot interface, are extensively described at ftp://spdf.gsfc.nasa.gov/pub/data/pioneer/pioneer10/ particle/crt/ip_6hour_ascii/p10crt6h_voldesc.sfdu SOHO ERNE Data The SOHO ERNE (Energetic and Relativistic Nuclei and Electron experiment) data accessible through this MSSP interface consist of 2-hour-averaged proton and alpha particle fluxes for the period February, 1996 to August, 2008. The 2-hour flux data were pulled from the U. Turku site at http://www.srl.utu.fi/erne_data/main_english.html. There are proton and alpha particle fluxes each in 5 energy bins between 1.8-3.3 MeV/n end 25.8-50.7 MeV/n. In the data at U.Turku, zero fluxes have been replaced by fill values to avoid problems in plotting on a logarithmic scale. However, because our MSSP interface enables the building of fluxes as averaged over user- specified durations, often significantly longer than two hours, and because we handle the plotting of zero fluxes differently (cf. http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/spectral_interface.txt), we have replaced all U.Turku fill values in the downloaded files with zeroes. Adjustments to settings of the sensor contributing to the higher energy fluxes prior to May 7, 1996, resulted in unreliable fluxes. This is why the H and He fluxes for two highest energy channels have our fill values from launch through May 7, 1996. ERNE was a contribution of the group at U. Turku, Finland. Dr. J. Torsti was the original Principal Investigator, and Dr. Eino Valtonen has subsequently assumed that role. The ERNE instrument is described at Torsti et al, Solar Physics, 162, 505-531, 1995. STEREO-A and -B IMPACT/LET The Low Energy Telescope (LET; Co-I Edward Stone, Caltech) flown on the STEREO-A and -B spacecraft is a part of the In-situ Measurements of Particles and CME Transients (IMPACT) investigation (PI: Janet Luhmann, UCB). LET data made accessible through this multi-source spectral plot interface, 1.8-12.0 MeV proton fluxes and 2.2-15.0 MeV/n alpha particle fluxes, spin averaged and in 4 energy windows each, were pulled from, and represent a very small subset of the data accessible through, the Caltech/LET interfaces at http://www.srl.caltech.edu/STEREO/DATA/Level1/Public/ahead/Hourly/ and http://www.srl.caltech.edu/STEREO/DATA/Level1/Public/behind/Hourly/. See http://www.srl.caltech.edu/STEREO/docs/LET_Level1.html#level1docs for further details. STEREO-A & -B IMPACT/SIT data The SIT (Suprathermal Ion Telescope) on the STEREO-A and -B spacecraft is a component of the overall IMPACT (In-Situ Measurements of Particles and CME Transients). SIT measures the heavy ion composition (H, He, C, O, Fe) from suprathermal energies (few 10's keV/n) to several MeV/n). The IMPACT Co-Investigator for SIT is Glenn Mason, JHU/APL. The hourly fluxes taken from from CDAWeb (which also provides statistical flux uncertainties) and accessible through this Multi-Source Spectral Plot (MSSP) interface consist of: H 0.320 - 10.24 MeV in 10 bins He 0.113 - 10.24 MeV/n in 13 bins [The MSSP-2 interface at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/flux_spectr_m2.html contains SIT fluxes for H, He, C, O, Fe.] A companion FTPBrowser interface at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/sta_sit_all_hr.html lists ranges for each energy bin for each element, and enables time-series plotting of any combination of elements and energy bins. The SIT instrument and measurements are described at http://sprg.ssl.berkeley.edu/impact/SSR/MasonetalSSR.pdf and at http://epact2.gsfc.nasa.gov/STEREO/SIT_description_V_2-9.pdf. An important page with caveats on data usage is at http://stereo.ssl.berkeley.edu/sit/caveats_2011_10_07.pdf. Ulysses COSPIN data These daily-averaged fluxes are from the LET (Low Energy Telescope; R.G. Marsden, ESTEC) and HET (High Energy Telescope; R.B. McKibben, UNH) components of the COSPIN (COsmic ray and Solar Particle INvestigation; R.B. McKibben, UNH) package flown on the Ulysses spacecraft. For instrument details, see: COSPIN: http://ulysses-ops.jpl.esa.int/ulysses/archive/cospin.html LET: http://helio.estec.esa.nl/ssd/public/let.html HET: http://ulysses.sr.unh.edu/WWW/Simpson/UlyDocs/HET.html. There are 5 LET proton fluxes in energy bins ranging from 2-4 to 16-20 MeV and two HET proton fluxes at 39-70 and 71-94 MeV. There are 3 LET alpha particle fluxes in energy bins ranging from 4-6 to 11-20 MeV/n and two HET alpha particle fluxes at 39-70 and 71-95 MeV/n. The fluxes are derived by convolving pulse height data and telescope coincidence more count rates. The data are further described, and are ftp-accessible, at LET: ftp://spdf.gsfc.nasa.gov/pub/data/ulysses/particle/cospin/let/let_pha_flux_h_he_1day/ and HET: ftp://spdf.gsfc.nasa.gov/pub/data/ulysses/particle/cospin/het/het_pha_flux_h_he_1day/ Ulysses HISCALE data These daily-averaged He fluxes are from the HISCALE (Heliosphere Instrument for Spectrum, Composition and Anisotropy at Low Energies; L.J. Lanzerotti, P.I. and T.P. Armstrong, Co-I and Data product creator) flown on the Ulysses spacecraft. The He fluxes are in 12 energy bands between 0.314-0.388 MeV/n to 3.17-3.91 MeV/n These fluxes were taken from a multi-species HISCALE data set (He, C, O, Ne, Si, Fe) accessible in EXCEL spreadsheet format from http://data.ftecs.com/VHO/VEPO/ace_epam/pha/spectra/. The fluxes result from the convolution of pulse height data and coincidence mode count rate data. On 2/2/2012, a newly FunTech-reprocessed version of the data, having revised fluxes and energy bin ranges, was swapped into this MSSP interface and into the FTPBrowser interface at http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/uly_hisc_flux_1d.html For instrument and data product details, see the Ulysses Data Analysis Handbook (and referenced therein) at http://hiscale.ftecs.com/uly-handbk-oview.html. For fluxes of all measured species, see http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/flux_spectr_m2.html Voyager 1&2 LECP data These data sets flow into NSSDC and its nssdcftp server routinely from the ftp site of the Voyager Low Energy Charged Particle team at the Applied Physics Laboratory. See http://sd-www.jhuapl.edu/VOYAGER/v1_data/v1_1h/v1_prot_1h/v1_%Y_prot_flux_1h.txt and ftp://spdf.gsfc.nasa.gov/pub/data/voyager/voyager1/particle/lecp/v1_prot_1hour/. The data consist of hourly proton fluxes and their uncertainties in the energy ranges 0.57-1.78, 3.40-17.6, and 22.0-31.0 MeV. See http://voyager.ftecs.com/default.htm and ftp://spdf.gsfc.nasa.gov/pub/data/voyager/voyager1/ particle/lecp/v1_prot_1day/read_me_v1_prot_flux_1d.txt for further detail. Owing to the significant interest in Voyager data as Voyager travels in the vicinity of the Heliosphere's boundary with the interstellar medium, we have today (11/20/2012) added LECP ion fluxes to the interfaces. These fluxes are dominantly protons, with an admixture of helium and higher-Z ions. The ion fluxes are in eight energy bins in the range 0.040-0.053 MeV/n to 2-4 MeV/n. Spectra for these fluxes are shown with spectra of protons from other sources upon the specification of Species = Protons on the interface page. The data are as taken from http://sd-www.jhuapl.edu/VOYAGER/v1_data/v1_1h/v1_ion_1h/ and http://sd-www.jhuapl.edu/VOYAGER/v2_data/v1_1h/v2_ion_1h/ Plots and lists of subsets of the fluxes and their uncertainties are available from http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/v1_lecp_ion_flux_1h.html and http://omniweb.sci.gsfc.nasa.gov/ftpbrowser/v2_lecp_ion_flux_1h.html Voyager 1&2 CRS data The Cosmic Ray Subsystem (CRS) investigations on Voyagers 1 and 2 were provided by a collaboration of Caltech personnel (Stone et al., Low Energy Telescope - LET) and GSFC personnel (McDonald et al., High Energy Telescope - HET). The team's web site, with much detail, is at http://voyager.gsfc.nasa.gov/. The 6-hour-resolution CRS data have many proton and alpha particle fluxes, which are not identically the same on the two Voyagers. For Voyager 1, there are eight proton energy bins (1.9-2.6 MeV to 132-242 MeV) and 11 alpha particle energy bins (1.8-2.6 MeV/n to 193-480 MeV/n). For Voyager 2, there are 11 proton energy bins (1.9-2.6 MeV to 171-225 MeV) and 14 alpha particle energy bins (1.8-2.6 MeV/n to 191-457 MeV/n). See the "Data home page" links on the spectral plot interface page for a listing of the individual energy bins for each spacecraft and species. The CRS fluxes made available through this multi-spacecraft spectral plot interface represent a data subset intended to eliminate much of the energy overlap of the underlying data. Only six of the eight or eleven energy channels per species are used, as shown when one selects the "Listing of spectral function points..." option from the spectral plot page. Some bins overlap due to energy overlap between LET and HET and others overlap in association with multiple count rate coincidence conditions. For further detail, see the CRS team web site cited above and see ftp://spdf.gsfc.nasa.gov/pub/data/voyager/voyager1/ particle/crs/six_hour/vy1crs_6h_fmt.txt. Wind EPACT LEMT data These EPACT/LEMT (Energetic Particles:Acceleration, Composition and Transport/Low Energy Matrix Telescope) data consist of hourly omnidirectional fluxes of helium in 6 energy bins spanning 2.0 to 12.7 MeV/n. They may also be found for solar particle event intervals, along with fluxes of higher-Z elements, at http://vho.nasa.gov/mission/wind/epact/omni/. See the EPACT web page at http://epact2.gsfc.nasa.gov/don/epact.htm for further detail. ----------------------------------------------------------------