PDS_VERSION_ID            = PDS3
DATA_SET_ID               = "CO-S-MIMI-4-LEMMS-CALIB-V1.0"
PRODUCT_ID                = "LPHASPGM0_2011038_00"
STANDARD_DATA_PRODUCT_ID  = "LEMMS_PHA_SPGM_DAILY"
PRODUCT_TYPE              = "BROWSE"
PRODUCT_VERSION_ID        = "00"
PRODUCT_CREATION_TIME     = 2013-017T16:42:45.000

INTERCHANGE_FORMAT        = BINARY
MD5_CHECKSUM              = "12e8d3c72a286eb597f472bab1a95a31"

START_TIME                = 2011-038T00:00
STOP_TIME                 = 2011-039T00:00

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

^DOCUMENT                 = "LPHASPGM0_2011038_00.PNG"
OBJECT                    = DOCUMENT
  DOCUMENT_NAME           = "LPHASPGM0_2011038_00"
  DOCUMENT_FORMAT         = PNG
  DOCUMENT_TOPIC_TYPE     = "BROWSE IMAGE"
  INTERCHANGE_FORMAT      = BINARY
  PUBLICATION_DATE        = 2013-015
  DESCRIPTION             = "This plot shows energy-time spectrograms for
    the LEMMS PHA electron data (top panel) and LEMMS PHA ion data (second
    panel). The ions are almost always protons, and these come from channels 8
    through 62 in the LEMMS PHA data. For protons, these channels have an
    energy range of 25 to 780 keV. The electrons (the lower of the two data
    panels) come from the LEMMS PHA E channels 15 through 62 and the LEMMS PHA
    F1 channels (26 through 59) and have energy ranges of 20 to 410  (for E
    channels) and 205 to 1700 keV (for F1 channels). Note that there is some
    overlap. Also note that in the data, it is usually possible to see the
    transition region from the lower energy E channels to the higher energy F1
    channels. This is because the efficiencies adn geometric factors used work
    for most situations, but in some environments, the detectors have
    different responses and this causes a visible seam in the data.

    The thin plot between the two data panels is a status panel indicating
    when sunlight contamination may be present in the data. This status panel
    is color coded such that green indicates the data is likely free of
    sunlight problems. Red indicates a likely contamination problem. 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.

    There is also a panel showing angles between the LEMMS Low Energy
    Telescope (LET) and various other vectors. The green line is the SZS
    longitude of the LET boresight. The black line is the latitude of the LET
    boresight in the SZS frame. The blue line is the Sun angle - the angle
    between the LET boresight and the Cassini-Sun line. This is the angle used
    to determine possible sunlight contamination.

    The X axis is labeled with the time of day and the local time (in SZS),
    and also the radial distance of Cassini to the center of Saturn.

    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 following frame definitions are used. Fpr 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.

    For the SZS frame, +Z points along the Saturn spin axis. +Y is +Z crossed
    into the Saturn-Sun line. +X is then +Y cross +Z."
END_OBJECT                = DOCUMENT
END