Start Time: 
        UTC time at the start of the search period.
        This is the earth receive time taken from the 
        FITS header.
        Formation rule: YYYY-MM-DDThh:mm:ss[.fff]

        Cautionary Note: A small number of files have 
        incorrect times in the FITS header.


End Time:   
        UTC time at the end of the search period.
        This is the earth receive time taken from the 
        FITS header.
        Formation rule: YYYY-MM-DDThh:mm:ss[.fff]

        Cautionary Note: A small number of files have 
        incorrect times in the FITS header.

Solar Longitude Year:
        Options -- map year, martian year
        Both Mars and the TES mapping years begin at Ls = 0, and the difference 
        between them is 23 years.
                                                           Mars Year 24
        End of TES year-1 mapping (Ls 360)       May 31, 2000
        Start of TES year-2 mapping (Ls 0)       June 01, 2000
                                                           Mars Year 25
        End of TES year-2 mapping (Ls 360)       April 18, 2002
        Start of TES year-3 mapping (Ls 0)       April 19, 2002
                                                           Mars Year 26
        End of TES year-3 mapping (Ls 360)       March 05 2004
        Start of TES year-4 mapping (Ls 0)       March 06, 2004
                                                           Mars Year 27
        End of TES year-4 mapping (Ls 360)       January 21, 2006
        Mars Year 1 began on April 11, 1955.

        Mapping Year range: 1 to 4
        Martian Year range 24 to 27 



Central Meridian Longitude (CML):
        Sub-observer longitude in System III West, 0-360 degrees. 
	The search range will cover the CML +/- the Longitude Range.


Longitude Range:
	Half-width of the Central Meridian Longitude search box in
	degrees. The search range will cover the CML +/- the Longitude
	Range.


Drift rate:
	Drift rate in degrees per day with respect to System III West.
	Enter a drift rate to track a feature that drifts at a known
	rate. The Central Meridian Longitude to be search at any given
	time is calcuated using:

        CML(t) = ( CML_start + drift_rate * ( t - t_start ) ) Modulo 360

        Default is 0 degrees per day.


Orton 1.58:
	This narrow band filter is centered at 1.58 microns, FWHM 0.013
	microns and was designed to detect sunlight reflected from the
	NH3 clouds in the absence of significant gaseous absorption; it
	is also sensitive to cloud particle albedos.


Spencer 2.3:
	This filter, centered at 2.28 microns, FWHM 0.17 microns, was
	designed to detect sunlight reflected from particles at the
	100-mbar level and above through a strong methane absorption
	band.


Circular variable filter, 3.533 micron:
	The center wavelength of 3.533 microns, FWHM 0.07 microns was
	chosen for the CVF to detect H3+ auroral emission near
	Jupiter's poles in a very strong methane absorption band.


L' or L'_MK:
	These filters, centered at 3.78 and 3.74 microns, FWHM 0.59 and
	0.70 microns, respectively, were used to detect sunlight
	reflected from particles at the 1-bar level and above, as well
	as some H3+ emission through a weak methane band.


nb-M or M'_MK:
	Centered at 4.78 and 4.68 microns, FWHM 0.23 and 0.24 microns,
	respectively, these filters were chosen to detect thermal
	emission from clouds in the absence of significant gaseous
	absorption.

Calibration Data:
	Select Stars and/or Flats to retrieve calibration files taken
	on the same night(s) as the Jupiter data.