PDS_VERSION_ID            = PDS3
DATA_SET_ID               = "CO-S-MIMI-4-LEMMS-CALIB-V1.0"
PRODUCT_ID                = "LCPRESS0_2004150"
STANDARD_DATA_PRODUCT_ID  = "LEMMS_PRESS_DAILY"
PRODUCT_TYPE              = "BROWSE"
PRODUCT_VERSION_ID        = "01"
PRODUCT_CREATION_TIME     = 2013-055T14:53:46

INTERCHANGE_FORMAT        = BINARY
MD5_CHECKSUM              = "2cb8709c42a3825f205cbfa0da8cf4f2"

START_TIME                = 2004-150T00:00
STOP_TIME                 = 2004-151T00:00

INSTRUMENT_HOST_NAME      = "CASSINI ORBITER"
INSTRUMENT_HOST_ID        = "CO"
TARGET_NAME               = "SATURN"
INSTRUMENT_NAME           = "MAGNETOSPHERIC IMAGING INSTRUMENT"
INSTRUMENT_ID             = "MIMI"

^DOCUMENT                 = "LCPRESS0_2004150_01.PNG"
OBJECT                    = DOCUMENT
  DOCUMENT_NAME           = "LCPRESS0_2004150_01"
  DOCUMENT_FORMAT         = PNG
  DOCUMENT_TOPIC_TYPE     = "BROWSE IMAGE"
  INTERCHANGE_FORMAT      = BINARY
  PUBLICATION_DATE        = 2013-015
  DESCRIPTION             = "This plot shows particle pressure
    spectrograms for LEMMS and CHEMS. It also shows total pressure for LEMMS
    and CHEMS, and for LEMMS, a comparable energy-time spectrogram. The
    location of the Cassini spacecraft is also shown.

    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 bwo 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."
END_OBJECT                = DOCUMENT
END