2.0.1 spase://vspo/numericalData/P_ACE_HDR_CRIS_L2_1D ACE CRIS L2 1-day Z=3-28 flux data 2007-06-01T00:00:00 ACE CRIS L2 1-day Z=3-28 flux data at ASC spase://SMWG/Person/Richard.A.Mewaldt GeneralContact spase://SMWG/Person/Richard.Leske TechnicalContact spase://SMWG/Repository/ACE_SC Online Open ACE Science Center http://www.srl.caltech.edu/ACE/ASC/level2/lvl2DATA_CRIS.html ACE/CRIS L2 data in HDF via ftp ftp://mussel.srl.caltech.edu/pub/ace/level2/cris/ CDAWeb http://cdaweb.gsfc.nasa.gov in CDF via ftp from CDAWeb ftp://cdaweb.gsfc.nasa.gov/pub/istp/ace/cris_h3 Text CALIBRATED spase://SMWG/Instrument/ACE/CRIS EnergeticParticles IonComposition 1997-08-14T00:00:00 -P21D Data are presently ~2-3 weeks delayed PT86400S Heliosphere.NearEarth spase://SMWG/Observatory/ACE ACE Advanced Composition Explorer 1997-045A Explorer 71 2009-05-20T20:00:12Z The objective of the Advanced Composition Explorer (ACE) is to collect observations of particles of solar, interplanetary, interstellar, and galactic origins, spanning the energy range from that of KeV solar wind ions to galactic cosmic ray nuclei up to 600 MeV/nucleon. Definitive studies will be made of the abundances of essentially all isotopes from H to Zn (Z = 1-30), with exploratory isotope studies extending to Zr (Z = 40). The ACE payload includes six high resolution spectrometers, each designed to provide the optimum charge, mass, or charge-state resolution in its particular energy range. Each spectrometer has a geometry factor optimized for the expected flux levels, so as to provide a collecting power greater by a factor of 10-1000 times that of previous or planned experiments. The payload also includes three additional instruments of standard design to monitor energetic electrons, H and He ions, and a magnetometer. The ACE spacecraft is based on the design of the Charge Composition Explorer, built at JHU/APL for the Active Magnetospheric Particle Tracer Explorer (AMPTE) program. The spacecraft spin axis is pointed towards the Sun to within +/- 20 degrees, and it occupies a halo orbit about the L1 Earth-Sun libration point. Powered by solar cells, the spacecraft has a design life of at least five years, and it returns data in daily tape recorder dumps, received through NASA JPL's Deep Space Network and initially processed at NASA-GSFC. The average data telemetry rate is 6.7 Kbs. spase://SMWG/Person/Edward.C.Stone.Jr PrincipalInvestigator ACE Home Page http://www.srl.caltech.edu/ACE/ ACE mission home page at Caltech with data download NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1997-045A Information about the ACE mission spase://vspo/observatory/2 Heliosphere.NearEarth Heliosphere.Inner spase://SMWG/Instrument/ACE/CRIS Cosmic Ray Isotope Spectrometer (CRIS) CRIS 2009-05-20T21:10:13Z The Cosmic Ray Isotope Spectrometer (CRIS) provides measurements with significant statistics of galactic cosmic ray nuclei from He to Zn (Z=2 to 30) at energies of 100 to 600 MeV/nucleon. CRIS makes more exploratory measurements of ultra-heavy nuclei from Ga (Z=31) to Zr (Z=40). The detector system consists of a Scintillating Optical Fiber Telescope (SOFT) hodoscope and four identical stacks of large-area silicon solid-state detectors. SOFT uses the optical fiber scintillation to provide position information in three x-y planes (H1, H2, H3) for trajectory measurement, while also providing a trigger counter (T) with two signals from the x-trigger and y-trigger fibers for the CRIS coincidence logic. Each detector stack includes eight four-inch diameter lithium-drifted (LiD) silicon solid-state detectors (SSD), designated as E1 to E8. Detectors E1 - E3 are 3-mm thick, while E3 - E8 are 6-mm thick and each consisting of a pair of 3-mm detectors. All detectors except E9 are pulse-height analyzed. Detectors E2 - E8 have a central active area surrounded by an annular integral guard ring used in anti-coincidence to elimiate side-penetrating events. Penetration of the entire stack is signaled by an E9 detector trigger. The total geometric factor for all four stacks is about 200 cm2-sr, dependent on energy, with a 45-degree conical (half-angle) field of view. Mass resolution for isotope analysis is at or below 0.25 amu. Most of the CRIS telemetry is devoted to event data, about 224 bits per analyzed event, while only 16 bps are needed for rate and housekeeping data. Since all analyzed events cannot be recorded during large solar flare events, a priority system ensures that the most significant events are selected for readout. In order of descending priority these are stopping heavy nuclei (Z > 2), penetrating heavies, stopping hydrogen and helium, and penetrating hydrogen and helium. Under all interplanetary conditions CRIS can then record most accumulated heavy nuclei events. spase://SMWG/Person/Alan.C.Cummings CoInvestigator spase://SMWG/Person/Richard.A.Mewaldt CoInvestigator spase://SMWG/Person/Richard.Leske TechnicalContact Instrument description http://www.srl.caltech.edu/ACE/CRIS_SIS/cris.html Description of the ACE CRIS instrument, with links to data NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1997-045A&ex=6 Information about the Cosmic Ray Isotope Spectrometer (CRIS) experiment on the ACE mission. spase://SMWG/instrument/1997-045A-06 ParticleDetector Cosmic Ray Isotope Spectrometer (CRIS) on ACE spase://SMWG/Observatory/ACE spase://SMWG/Repository/ACE_SC SRL ACE Science Center ASC 2008-06-18T06:07:48Z ACE Science Center Please acknowledge the ACE instrument teams and the ACE Science Center in publications and presentations that use these data spase://SMWG/Person/Andrew.J.Davis PrincipalInvestigator GeneralContact ACE Science Center http://www.srl.caltech.edu/ACE/ASC spase://SMWG/Person/Richard.A.Mewaldt Dr. Richard A. Mewaldt California Institute of Technology spase://SMWG/Person/Richard.Leske 2007-11-27T19:24:48Z Dr. Richard Leske California Institute of Technology ral@srl.caltech.edu spase://SMWG/Person/Alan.C.Cummings Dr. Alan C. Cummings California Institute of Technology spase://SMWG/Person/Andrew.J.Davis Dr. Andrew J. Davis California Institute of Technology spase://SMWG/Person/Edward.C.Stone.Jr 2001-04-02T00:00:00Z Prof. Edward C. Stone, Jr. California Institute of Technology ecs@srl.caltech.edu +1-626-395-8321