C osmic R Ay T elescope for the E ffects of R adiation CRaTER Data Products & Production Pipeline Larry Kepko Boston University Center for Space Physics CRaTER PDR

C osmic R Ay T elescope for the E ffects of R adiation Calibration  By exposing the detectors to beams of known energies, we can determine the response. Current From Detector Energy of Incident Particle

C osmic R Ay T elescope for the E ffects of R adiation Calibration  We will calibrate the detectors at 3 different beam facilities, each with different energy ranges and species. Timetable TBD  Spot-checking

C osmic R Ay T elescope for the E ffects of R adiation Calibration  88” Cyclotron, Lawrence Berkeley National Laboratory FacilityBeam Properties LIIF9-55 MeVH 19 or 32.5 MeV/nucleonHe to Ne HIIF4.5 MeV/nucleonHe to Bi 10 MeV/nucleonB to Xe MeV/nucleonC to Xe

C osmic R Ay T elescope for the E ffects of R adiation Calibration  NASA Space Radiation Laboratory at Brookhaven National Laboratory FacilityBeam Properties Boosterup to 1 GeVH Boosterup to 1 GeV/nucleonFe

C osmic R Ay T elescope for the E ffects of R adiation Calibration  Indiana University FacilityBeam Properties IUCF MeVH

C osmic R Ay T elescope for the E ffects of R adiation CRaTER Data Products Description Level 0 Unprocessed instrument data (pulse height at each detector), secondary science (discarded events), housekeeping. Level 1 Science data depacketed, 1-s resolution. Ancillary data pulled in (spacecraft attitude, calibration files, etc) Level 2 Pulse heights converted into energy deposited in each detector. Calculation of Si LET spectra. Level 3Separate out magnetotail, foreshock and ‘GCR’ data. Level 4 Calculation of TEP LET, incident energies and particle flux. Pull in GCR data from other spacecraft (e.g. ACE).

C osmic R Ay T elescope for the E ffects of R adiation Level 0 To Level 1 Processing LRO MOC Housekeeping Primary/secondary science sFTP CRaTER SOC Validation PDS L0 Archive

C osmic R Ay T elescope for the E ffects of R adiation Level 0 Data Products Level 0 Science Unprocessed instrument data (pulse height at each detector), secondary science (discarded events, etc.). Up to 25 packets of up to 48 events per second Level 0 Housekeeping Bias voltage, temperature, etc., 16-s resolution

C osmic R Ay T elescope for the E ffects of R adiation Level 1 To Level 2 Processing LRO MOC Calibration Files Orbit & Attitude sFTP Depacket, create 1-s data PDS L1 Archive CRaTER SOC

C osmic R Ay T elescope for the E ffects of R adiation Level 1 Data Products Level 1 Science Unprocessed instrument data (pulse height at each detector), depacketed. Creation of 1-s data. Secondary science placed in 1-s data header. Level 1 Housekeeping Bias voltage, temperature, etc., 16-s resolution

C osmic R Ay T elescope for the E ffects of R adiation Level 2 To Level 3 Processing Convert to energy deposited PDS L2 Archive Calculate Si LET Events of Interest QL Plots

C osmic R Ay T elescope for the E ffects of R adiation Level 2 Data Products Level 2 ScienceEnergy deposited in each detector and LET. QL PlotsTBD Events of Interest e.g., SEP events.

C osmic R Ay T elescope for the E ffects of R adiation Level 3 To Level 4 Processing Region Separation GCR Foreshock Magnetotail SEP Events

C osmic R Ay T elescope for the E ffects of R adiation Level 3 Data Products L3 Region Data separated into 3 files (or, alternately, 1 file with a data flag) identifying what data was obtained while the moon was in the a) magnetosphere, b) foreshock and c) pure GCR L3 SEP Data containing SEP events (definition TBD) are separated as well

C osmic R Ay T elescope for the E ffects of R adiation Level 4 Calculate LET in TEP Modeling Community ? Calculate Particle Flux GCR Spectrum

C osmic R Ay T elescope for the E ffects of R adiation Timetables  Level 2 data produced immediately upon verification of Level 1 data. Only involves application of pre-flight calibration curves and simple LET calculations.  GCR LET spectrum requires time The longer the better Probably something useful after 3-6 months

C osmic R Ay T elescope for the E ffects of R adiation Back-up Slides

C osmic R Ay T elescope for the E ffects of R adiation LET Calculation Linear Energy Transfer (LET) is the energy deposition in matter per unit length

C osmic R Ay T elescope for the E ffects of R adiation LET Calculation LET in the Silicon detectors can be calculated directly

C osmic R Ay T elescope for the E ffects of R adiation LET Calculation LET in the TEP requires E 0 and E f E0E0 EfEf