Lambertian albedo, derived from visual bolometer.
See PROCESS.PDF, Section 3.0 for a description of the visible bolometer calibration algorithms.

A constraint for spectral data that has a low risk of algor phase inversions (RAD.QUALITY:ALGOR_RISK=0).
See QUALITY.TXT for a complete description of this quality issue.

Total emissivity is deconvolved using eight spectral components which represent surface, atmospheric dust, atmospheric ice, and a thermal blackbody. The atmospherically corrected emissivity is calculated by removing the atmospheric dust and ice components from the total emissivity. The correction is only applied to single scan observations over channels 9-35 and 65-100.
See Surface Endmember Array entry for components and percentages, and BANDFIELD, 2002 for more information about the deconvolution.

Atmospheric opacities are provided as scaling factors for four spectral shapes (STDSHAPES) that best fit the nadir radiance spectrum. The RMS residual between the observed and four endmember modeled spectra is also available, given in units of 1e-8 watts cm-2 steradian-1 wavenumber-1.
See ATM.FMT and PROCESS.PDF, Section 7.0 for more information.

Aerosol dust opacity (ATM.NADIR_OPACITY[1])
Aerosol water ice opacity (ATM.NADIR_OPACITY[2])
CO2 hot bands opacity (ATM.NADIR_OPACITY[3])
Reference surface emissivity (ATM.NADIR_OPACITY[4])
Opacity RMS (ATM.NADIR_OPACITY_RESIDUAL)

TES Team scientists have rated the quality of the derived opacity results and provided a constraint to select only the best results (ATM.QUALITY:ATMOSPHERIC_OPACITY_RATING=0).
See QUALITY.TXT for more information.

Temperature observed by the thermal bolometer, assuming that the target is radiating as a blackbody; in units of K.
See PROCESS.PDF, Section 4.0 for a description of the thermal bolometer calibration algorithms.

Calibrated visual bolometer radiance; given in units of (watts cm-2 steradian-1). The visual bolometer operates at 0.3 - 2.7 microns.
See PROCESS.PDF, Section 3.0 for a description of the calibration algorithms.

TES Team scientists recommend the following constraints for query results of spectra with minimal atmospheric effects.
Note: do not use this constraint when requesting only bolometric results.

ATM.QUALITY:ATMOSPHERIC_OPACITY_RATING 0 0
ATM.NADIR_OPACITY[1] -0.03 0.2 (i.e. Dust Opacity)
ATM.NADIR_OPACITY[2] -0.03 0.1 (i.e. Water Ice Opacity)

See ATM.FMT for more information.

The number of the spectrometer detector that made the observation. Detectors are numbered from 1 to 6.

A spatial detector mask was applied to every TES spectral observation prior to transmission to Earth. There are eight possible combinations [0-7] of co-adding the spectra from the six detectors, for example: mask 1 = all detectors co-added into single spectrum; mask 7 = all detectors downlinked as separate spectra.
See DETMASK.TXT for more information.

Atmospheric downwelling flux due to either CO2 (667 cm-1 band) or all atmospheric aerosols; given in watts cm-2.
See ATM.FMT and PROCESS.PDF, Section 7.0 for more information.

Angle between the spacecraft, the target point and the surface normal vector at the target. When TES is observing the surface directly below the spacecraft, the emission angle is close to 0 degrees.

Emissivity is calculated by dividing the TES calibrated radiance by a blackbody at the calculated target temperature for the observation.

There are 143 radiance channels at ~10 wavenumber spacing, and 256 radiance channels at ~5 wavenumber spacing. To restrict the returned spectral resolution, use commas to separate a list of individual channel numbers (1,2,....,n) and/or define a range of channel numbers (min:max). Example = 6,50:100,125,130:143

If SCAN_LENGTH is not constrained, then all available wavelength modes (singles and/or doubles) will be returned in the results; in this case, the value of radiance channels [144:256] will be NULL for single mode data.
See Wavelength entry for more information.

Emissivity band depths indexes and ratios are calculated as follows (all bands given in cm-1):

Hematite Index (PCT.HEM_INDEX) - emissivity band ratio = [360-391]/[286-296+466-476]
LongWave Depth Index (PCT.LW_DEPTH) - emissivity at long wavelengths 350-450
ShortWave Depth Index (PCT.SW_DEPTH) - emissivity at long wavelengths 1354-1397
LongWave Ratio (PCT.LW_RATIO) - emissivity band ratio = [425-455]/[380-390+465-475]
450 & 530 Index - not currently available

See BANDFIELD, 2003 for more information.

The time at the beginning of the observation, given in seconds since 12:00 a.m. January 1, 2000. The TES mapping mission covers the ET range -26495432 and 214295844.

The TES Team scientists have noted that the motions of either the antenna or the panels induce microphonics which adversely affect the quality of the observed spectra. Use this constraint to obtain spectral data collected at a time when the High Gain Antenna was not moving (RAD.QUALITY:HGA_MOTION=1) or when the Solar Panels were not moving (RAD.QUALITY:SOLAR_PANEL_MOTION=1).
See QUALITY.TXT for a complete description of this quality issue.

TES Team scientists recommend the following constraints so that query results only contain the highest quality bolometric data:

BOL.QUALITY:BOLOMETRIC_INERTIA_RATING 0 1
BOL.QUALITY:BOLOMETER_LAMP_ANOMALY 0 0

See QUALITY.TXT and BOL.FMT for more information on these fields.

TES Team scientists recommend the following constraints so that query results only contain the highest quality spectral data:

RAD.QUALITY:MAJOR_PHASE_INVERSION 0 0
RAD.QUALITY:ALGOR_RISK 0 0
OBS.DETECTOR_MASK 7 7
RAD.TARGET_TEMPERATURE 250 300
OBS.IMC_COUNT 0 0

See QUALITY.TXT, PROCESS.PDF, Section 8.0, and DETMASK.TXT for more information on these fields

The number of two-second intervals that have elapsed since the start of the orbit. The two-second interval is the smallest time unit defined by the TES instrument and equals the time to complete a single length scan. There are approximately 3530 icks per TES orbit.

TES was originally designed to improve the quality of the collected spectra by mechanically compensating for the MGS orbital motion using Image Motion Compensation (IMC); however, due to issues during aerobraking, the MGS orbit was modified and the TES IMC was infrequently used. The IMC_COUNT can be used to constrain data based on the use of the IMC:

IMC Off selects only spectral data where OBS.IMC_COUNT = 0
IMC On selects only spectral data where OBS.IMC_COUNT > 1

Angle between the sun, the target point, and the surface normal vector at the target.
TES day observations have an incidence angle between 0 and 90 degrees; TES night observations have an incidence angle between 90 and 180 degrees.

TES calibrated radiances are convolved to Viking IRTM band resolution for the five primary data channels. Original IRTM channels, with wavelength ranges, are generated from the TES (double scan) channels as follows:

T7 (6.1 - 8.3 um) = (184 - 284)
T9 (8.3 - 9.8 um) = (154 - 234)
T11 (9.8 - 12.5 um) = (118 - 186)
T20 (17.7 - 30.0 um) = (36 - 90)
T15* (14.56 - 15.41 um) = (92 - 104)

Areocentric latitude of target point; given in degrees.
All derived surface geometry values are computed on the IAU-1994 Mars ellipsoid.

Local time at target, in decimal Martian hours. The Martian day is divided into 24 equal hours.

Originally, TES data was released with Areocentric WEST longitude coordinates of observed point, based on the IAU-1994 Mars ellipsoid. TES longitudes are now also available in Areocentric EAST coordinates, based on the IAU-2000 Mars ellipsoid. All longitudes are given in degrees.

To translate between IAU-1994 (west) and IAU-2000 (east) coordinate systems:

EAST_LONGITUDE = 360 - WEST_LONGITUDE + 0.271
with the appropriate adjustments made at the 0/360 boundary.

Distance in KM from the spacecraft to the sub-spacecraft point on the planet surface.

A constraint for spectral data that does not contain major phase inversion (RAD.QUALITY:MAJOR_PHASE_INVERSION=0).
See QUALITY.TXT for a complete description of this quality issue.

The angle the TES scanning mirror was pointing during the observation, measured in degrees away from nadir. Mirror angles between -90 and +65 view Mars and space.

A coarse data constraint based on the following observation criteria:

Surface = OBS.OBSERVATION_TYPE D D
Warm Surface = OBS.OBSERVATION_TYPE D D & RAD.TARGET_TEMPERATURE 250 300
Limb = OBS.OBSERVATION_TYPE L L
EPF = OBS.OBSERVATION_CLASSIFICATION:{INTENDED_TARGET 1 1 & TES_SEQUENCE 6 6}

Sequential count of the number of orbital revolutions since orbit insertion; unique throughout the entire MGS mission. This number is identical to the MGS project orbit number up until the beginning of the Mapping Phase (ock=1684) when the MGS Project reset its orbit count to 1. For your convenience, an approximate orbit timetable is available here.

Calibrated spectral radiance; given in units of (watts cm-2 steradian-1 wavenumber-1).
See PROCESS.PDF, Section 2.0 for a description of the calibration algorithms.

There are 143 radiance channels at ~10 wavenumber spacing, and 256 radiance channels at ~5 wavenumber spacing. To restrict the returned spectral resolution, use commas to separate a list of individual channel numbers (1,2,....,n) and/or define a range of channel numbers (min:max). Example = 6,50:100,125,130:143

If SCAN_LENGTH is not constrained, then all available wavelength modes (singles and/or doubles) will be returned in the results; in this case, the value of radiance channels [144:256] will be NULL for single mode data.
See Wavelength entry for more information.

The value of the spacecraft clock at the beginning of the observation, given in seconds since 12:00 a.m. January 1, 1980. The TES mapping mission covers the SCLK range 604699726 and 845491040.

A spectral mask was applied to every TES spectral observation prior to transmission to Earth. There are 21 masks defined which either select, reject, or average the data from each spectral sample; mask 00 selects all spectral samples.
See SPECTMASK.TXT for more information.

The MGS spacecraft postion vector relative to Mars in the J2000 reference frame; derived from the MGS-SPICE kernels. Returns a 3-item array of values given in units of KM.

The MGS spacecraft pointing quaternion in the J2000 reference frame; derived from the MGS-SPICE kernels. Returns a 4-item array of values given as a "SPICE-syle" quaternion.

Planetocentric longitude of the sun, used to measure the Martian seasons:

0 = start of Northern spring/Southern autumn
90 = start of Northern summer/Southern winter
180 = start of Northern autumn/Southern spring
270 = start of Northern winter/Southern summer

The Sun postion vector relative to Mars in the J2000 reference frame; derived from the MGS-SPICE kernels. Returns a 3-item array of values given in units of KM.

Results from Bandfield's atmospheric correction routine available as an array of the eight percentage concentrations and the RMS error. In order, the array contains:

PCT.PERC_BAS1 - concentration of Acidalia Type surface endmember (andesite)
PCT.PERC_BAS2 - concentration of Syrtis Type surface endmember (basalt)
PCT.PERC_HEM - concentration of hematite endmember
PCT.PERC_DUST1 - concentration of low CO2 dust endmember
PCT.PERC_DUST2 - concentration of high CO2 dust endmember
PCT.PERC_ICE1 - concentration of high latitude water ice cloud endmember
PCT.PERC_ICE2 - concentration of low latitude water ice cloud endmember
PCT.PERC_BB - concentration of blackbody endmember
PCT.RMS_ERROR - RMS error between measure and modeled spectra

See BANDFIELD, 2002 for more information.

Atmospheric pressure at the surface of Mars, given in mbar x1000. It is calculated from the altitudes given by the MOLA 1/4 degree x 1/4 degree topographic map, the hydrostatic law assuming a 10 km scale height, and an adjustment for the seasonal CO2 sublimation cycle. Proper normalization is obtained by fitting the pressures observed by the Viking and Pathfinder landers.
See PROCESS.PDF, Section 7.0 for more information.

Derived temperature of the observed target; given in units of K.
See PROCESS.PDF, Section 5.0 for a description of the surface temperature algorithm.

Array of atmospheric temperatures from nadir observations corresponding to 38 pressure levels (16.58152 to 0.00159 mbars), given in degrees-K x100. The NULL value (444.4) is used either when (a) the temperature retrieval fails, or (b) the pressure either exceeds the local surface pressure, or is less than 0.1 mbar.
See ATM.FMT and PROCESS.PDF, Section 7.0 for more information.

TES Team scientists have rated the quality of the pressure-temperature profile and provided a constraint to select only the best results (ATM.QUALITY:TEMPERATURE_PROFILE_RATING=0).
See QUALITY.TXT for more information.

Thermal inertia, derived from thermal bolometer; given in units of (J m-2 s-1/2 K-1). When selecting this field, consider applying the Highest BOLOMETRIC Quality constraint.
See PROCESS.PDF, Section 6.0 for a description of the thermal inertia algorithms.

Vanilla is a tool that treats PDS standard tables as a hierarchical database and allows simple queries across one or more tables. For TES specific example queries, see the Vanilla User Guide.

Wavelength of scan; for complete wavenumber tables, organized by detector and channel (see links):

single length scans (~10 wavenumber spacing)
double length scans (~5 wavenumber spacing)

TES Team Scientists highly recommend defining a SCAN_LENGTH constraint if any Spectral Bands (Radiance, Emissivity, or Atmospherically Corrected Emissivity) are selected. Constraining SCAN_LENGTH by "None" has the effect of allowing both wavelength modes (single and/or double) to be returned when available, so it should only be used ...

... IF the query returns only TES bolometer data;
... or IF the query returns fields not derived from TES spectral data;
... or IF either SCAN_LENGTH is acceptable in the query results.

When the wavelength mode is unconstrained, consider adding SCAN_LENGTH (under Additional OBS Fields) to the Field Selection List for clarity during analysis.