urn:nasa:pds:cassini-mimi-lemms-cal:browse-lcpress:lcpress_2016183 1.0 1.20.0.0 Product_Browse Vandegriff, Jon 2024 LEMMS MIMI This file contains Cassini Magnetospheric Imaging Instrument (MIMI) Calibrated CHEMS and LEMMS particle pressure spectrograms. Also shown is the total pressure and for LEMMS, comparable energy-time spectrogram all given the location of the Cassini spacecraft for 2016-07-01T00:00:00.000Z to 2016-07-02T00:00:00.000Z. 2024-05-13 1.0 This product, LCPRESS0_2016183_02.PNG, was originally released as part of the PDS3 CO-S-MIMI-4-LEMMS-CALIB-V1.0 data set. The metadata have been migrated to PDS4. The data themselves are unchanged. 2016-07-01T00:00:00.000Z 2016-07-02T00:00:00.000Z Science Calibrated Cassini MIMI LEMMS Calibrated Particle Pressure Spectrogram 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 MIMI Low Energy Magnetospheric Measurement Sensor for Cassini Orbiter Instrument urn:nasa:pds:context:instrument:mimi-lemms.co is_instrument Saturn Planet urn:nasa:pds:context:target:planet.saturn browse_to_target 237 237 25 59 Ions Energy Flux Proton urn:nasa:pds:cassini-mimi-lemms-cal:data-pha-full:lphafull_2016183::1.0 browse_to_data CO-S-MIMI-4-LEMMS-CALIB-V1.0:LCPRESS0_2016183:LCPRESS0_2016183_02.PNG data_to_calibrated_source_product 10.17189/1519608 PDS Planetary Plasma Interactions Node This is the first version converted to PDS4. The DOI references the source PDS3 data set. LCPRESS0_2016183_02.PNG 2017-06-28T12:32:11 152057 558d4cf85083e8415195920ad2ef90e3 The top panel shows a spectrogram of CHEMS particle pressure. The source for this data are the 32 energy steps (3 to 230 keV) for the BR0 and BR3 summed channels of just Telescope 2. This telescope was chosen because it points most closely to the now-fixed look direction of LEMMS. The intensities are averaged into 5 minute bins before converting to pressure. The units are dyne/cm^2. Note that in the magnetosphere of Saturn, the CHEMS pressures can only be trusted outside of L values around 4. The next panel is particle pressure based on LEMMS PHA ions, presumed to be protons. Channels A08 through A62 are used and cover an energy range of 25 to 780 keV. These data are averaged into 120 second bins before calculating the pressure. The units are the same as for the CHEMS data in the top panel. Note that in the magnetosphere of Saturn, the LEMMS pressures can only be trusted outside of L values around 6. Inside this distance, background levels become significant and cause the reported pressure to be too high. There is essentially very little particle pressure in this region anyway. The next panel shows the total pressure, as computed by summing the LEMMS and CHEMS pressure spectrograms in the above panels. The units for the pressure are still the same. The next panel is a LEMMS energy-time spectrogram based on these LEMMS A and P channels: A0 through A7 and P2 through P8 excluding P4. These channels cover an energy range of 27 keV to 59 MeV and are averaged into 120 second bins. The units are particles/sec/cm^2/ster/keV. Directly below this LEMMS spectrogram is a thin panel showing times of potential light contamination for LEMMS. Red indicates times when the angle between the LET boresight and the Cassini-Sun vector is less than 60 degrees. Black and gray both indicate that attitude data could not be obtained to make a determination. The Cassini MIMI Data User Guide discusses LEMMS light contamination in more detail. The bottom three panels show the position of Cassini relative to Saturn in the KSM frame. The first plot is a top view, with the Sun to the left. The blue trace is the projection of the bow shock into the X-Y plane, and the brown line is the magnetopause projection. The equation for the bow shock was obtained from Went, et al, 2011, A new semiempirical model of Saturn's bow shock based on propagated solar wind parameters, DOI: 10.1029/2010JA016349. The magnetopause used is from Kanani et al, 2009, A new form of Saturn's magnetopause using a dynamic pressure balance model, based on in situ multi-instrument Cassini measurements DOI: 10.1029/2009JA014262. In each of the trajectory plots, Saturn is in the middle, and the actual orbit of Titan is shown (centered on the time of the data, but extendeing several days before and after so that the whole orbit can be seen). The location of Titan at the middle of the day of the data plots is indicated with a small red circle. The trajectory of Cassini is shown in black, and the part of the trajectory covered by the data is shown with a thicker blue line. The position of Cassini at the start of the data plot is indicated by a red X. In the KSM YZ projection, the magnetopause and bow shock are shown projected into the plane containing the spacecraft. Note that if the spacecraft is far enough inside or outside, these boundaries may not appear. The KSM frame is defined as follows: KSM, +X points from Saturn to the Sun. +Y is the Saturn dipole axis crossed into the +X axis. (In practice, the spin axis of Saturn is used in place of the dipole axis.) The +Z axis is then +X cross +Y. LCPRESS_2016184 0 PNG