urn:nasa:pds:cassini-mimi-chems-cal:browse-cspgm:cspgm_opp_2012140_2012160 1.0 1.20.0.0 Product_Browse Vandegriff, Jon 2024 CHEMS MIMI This file contains Cassini Magnetospheric Imaging Instrument (MIMI) Charge Energy Mass Spectrometer (CHEMS) 20-day energy per charge spectrogram for O++, (water group ions such as H2O+, OH+, and O+) during the Extended-Extended Mission from 2012-05-19T00:00:00.000Z to 2012-06-08T00:00:00.000Z. 2024-05-13 1.0 This product, CSPGM0_OPP_2012140_2012160_00.PDF, was originally released as part of the PDS3 CO-S-MIMI-4-CHEMS-CALIB-V1.0 data set. The metadata have been migrated to PDS4. The data themselves are unchanged. 2012-05-19T00:00:00.000Z 2012-06-08T00:00:00.000Z Science Calibrated Cassini MIMI CHEMS Energy per Charge O++ Browse Heliosphere Magnetosphere Particles Ions Energetic Cassini-Huygens Mission urn:nasa:pds:context:investigation:mission.cassini-huygens browse_to_investigation Cassini Orbiter Host urn:nasa:pds:context:instrument_host:spacecraft.co is_instrument_host Magnetospheric Imaging Instrument for Cassini Orbiter Instrument urn:nasa:pds:context:instrument:mimi.co is_instrument MIMI Charge/Energy Mass Spectrometer Instrument urn:nasa:pds:context:instrument:mimi-chems.co is_instrument Saturn Planet urn:nasa:pds:context:target:planet.saturn browse_to_target Titan Satellite urn:nasa:pds:context:target:satellite.saturn.titan browse_to_target Titan Satellite urn:nasa:pds:context:target:satellite.saturn.titan browse_to_target Extended-Extended Mission 1716079913.000 1717807923.000 1 166 167 3 220 Ions Pulse Height Analysis Heavy urn:nasa:pds:cassini-mimi-chems-cal:data-cpavg:cphaflx_t1_opp_2012140_2012160::1.0 browse_to_data urn:nasa:pds:cassini-mimi-chems-cal:data-cpavg:cphaflx_t2_opp_2012140_2012160::1.0 browse_to_data urn:nasa:pds:cassini-mimi-chems-cal:data-cpavg:cphaflx_t3_opp_2012140_2012160::1.0 browse_to_data urn:nasa:pds:cassini-mimi-chems-cal:data-cpavg:cphaflx_ta_opp_2012140_2012160::1.0 browse_to_data CO-S-MIMI-4-CHEMS-CALIB-V1.0:CSPGM0_OPP_2012140_2012160_00:CSPGM0_OPP_2012140_2012160_00.PDF data_to_calibrated_source_product 10.17189/1519606 PDS Planetary Plasma Interactions Node This is the first version converted to PDS4. The DOI references the source PDS3 data set. CSPGM0_OPP_2012140_2012160_00.PDF 2013-01-24T16:46:26 1203442 b54f69ec1b83b233a5052883aaa8c956 CSPGM0_OPP_2012140_2012160_00 0 PDF PDF file containing CHEMS 20-day energy per charge Spectrograms for O++. Pixels are 15 percent in energy per charge by 60 minutes and are based on CHEMS PHA data. The bottom axis is time covering a 20 day interval. Also given is the position of the Cassini spacecraft in SZS (Saturn equatorial) coordinates is given along the x-axis. The coordinates are radial distance from the center of Saturn in Saturn radii, latitude in degrees, and local time in decimal hours (sunward = 12.0, anti-sunward = 0.0). The y-axis is energy per charge (keV/e). The color represents the differential intensity for this species, and the units are particles per (cm^2 sec sr keV/e). No background has been subtracted. There are 4 horizontal panels in the plot. The top panel contains the average intensity from all three CHEMS telescopes combined (full 4 degrees x 159 degrees FOV). Each panel below is for an individual telescope (4 degrees x 53 degrees FOV) (1, 2, and 3 respectively). The intensities are derived from triple coincidence events (TOF + SSD energy) at high energies and from double coincidence events (TOF only) plus (relatively rare) triple coincidence events at low energies. The energy ranges for the 32 E/Q steps are defined in the CHEMS energy per charge average file LBL files which were used to create these products. For O++ the transition occurs at 25.6 keV/e. Because of the large drop in number of PHA events (sometimes to zero or one event in one hour) at the transition from doubles + triples to triples only, an apparent discontinuity is sometimes observed in the intensity at the transition energy. When statistics are abundant the transition should be smooth. Below 25.6 keV/e, only mass/charge is determined, not mass and charge separately. Therefore at lower energies, this channel will include any species in the m/q=8 range. O++ generally dominates. Background is expected to be lower for the triples only events.