ACE Solar Isotope Spectrometer (SIS) hourly intensities and count rates, for each of 14 elements (He,C,N,O,Ne,Na,Mg,Al,Si,S,Ar,Ca,Fe,Ni).in each of 8 energy bins. Overall energy ranges covered go from 3.4-41 MeV/n for helium to 10.5-168 MeV/n for iron. These are calibrated science quality data. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. The "parameter keys" given below are as used by CDAWeb.

ACE Solar Isotope Spectrometer (SIS) 256-sec intensities and count rates, for each of 14 elements (He,C,N,O,Ne,Na,Mg,Al,Si,S,Ar,Ca,Fe,Ni). in each of 8 energy bins. Overall energy ranges covered go from 3.4-41 MeV/n for helium to 10.5-168 MeV/n for iron. These are calibrated science quality data. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. The "parameter keys" given below are as used by CDAWeb.

ACE Cosmic Ray Isotope Spectrometer (CRIS) intensities and counts, for each of 7 energy bins for each of 24 elements (Z=5, boron, to Z=28, nickel) at 1-hour time resolution. Overall energy ranges coveredgo from 49-172 MeV/n for boron to 130-496 MeV/n for nickel. Calibrated science quality data. Parameter segments below address intensities but not alsothe count rates included in the data set. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. Daily averaged L2 fluxes and rates are also available from these access paths. The "parameter keys" given below are as used by CDAWeb.

ACE Cosmic Ray Isotope Spectrometer (CRIS) intensities and counts, for each of 7 energy bins for each of 24 elements (Z=5, boron, to Z=28, nickel) at 1-hour time resolution. Overall energy ranges covered go from 49-172 MeV/n for boron to 130-496 MeV/n for nickel. Calibrated science quality data. Parameter segments below address intensities but not also the count rates included in the data set. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. Daily averaged L2 fluxes and rates are also available from these access paths. The "parameter keys" given below are as used by CDAWeb.

Daily-averaged species-separated energy spectra derived from the Pulse Height Analyzer. Data consist of counts and fluxes of each of six species (He, C, O, Ne, Si, Fe) in each of 12 energy bins.

The Ultra Low Energy Isotope Spectrometer measures Ion Fluxes over the Charge Range from H through Ni from about 20 keV/nucleon to 10 MeV/nucleon, thus covering both Suprathermal and Energetic Particle Energy Ranges. Exploratory Measurements of Ultra-Heavy Species (Mass Range above Ni) will also be performed in a more limited Energy Range near 0.5 MeV/nucleon. ULEIS will be studying the Elemental and Isotopic Composition of Solar Energetic Particles, and the Mechanisms by which these Particles are energized in the Solar Corona. ULEIS will also investigate Mechanisms by which Supersonic Interplanetary Shock Waves energize Ions. To avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for Erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication.

This ACE SWICS/SWIMS Data Set contains the He/O, C/O, N/O, Ne/O, Mg/O, Si/O, S/O, Fe/O Abundance Ratios, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for Erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, He/O, C/O, Ne/O, Mg/O, Si/O, Fe/O Abundance Ratios, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for Erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, Fe/O Abundance Ratio, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for Erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

Daily-averaged and spin-averaged count rates from all detectors.