Mars Global Surveyor
Thermal Emission Spectrometer
Data Processing User's Guide
Version 1.03
May 15, 1999
Prepared by:
Philip R. Christensen
TES Principal Investigator
Arizona State University
Tempe, AZ 85287-1404
Approved:
Philip R. Christensen Date
TES Principal Investigator
Thomas Thorpe Date
Mars Global Surveyor Science Office Manager
Yolanda Fletcher Date
PDS / Mars Global Surveyor Interface Manager
1.0 OVERVIEW
INSTRUMENT DESCRIPTION
The Thermal Emission Spectrometer (TES) investigation is designed to study
the surface and atmosphere of Mars using thermal infrared (IR) spectroscopy,
together with broadband thermal and solar reflectance radiometry. The
specific objectives of the TES experiment are: (i) to determine and map the
composition of surface minerals, rocks, and ices; (ii) to study the
composition, particle size, and spatial and temporal distribution of
atmospheric dust; (iii) to locate water-ice and CO2 condensate clouds and
determine their temperature, height, and condensate abundance; (iv) to study
the growth, retreat, and total energy balance of the polar cap deposits; (v)
to measure the thermophysical properties of the martian surface materials;
and (vi) to characterize the thermal structure and dynamics of the
atmosphere. A complete description of the TES instrument is given in
(Christensen et al., 1992).
The TES instrument consists of three sub-sections, the primary one being a
Michelson interferometer that produces spectra from 1700 to 200 cm-1 (~6 to
50 microns), at a spectral sampling of either ~5 or ~10 cm-1. The instrument
cycle time, including collection of the interferogram, mirror flyback, and
electronic reset, is 2 sec for 10 cm-1 ("single scan") operation, and 4 sec
for 5 cm-1 ("double scan") operation. The interferometer includes a visible
interferometer with a monochromatic source that is used to generate fringes
which control the linear drive servo and determine position in the
interferogram. This system uses two redundant neon lamps that produce an
emission line at 703.2 nm for fringe generation and a continuum that is used
for a quasi-white-light source for determination of zero path difference.
The TES instrument returns 143 points in single-scan or 286 points in double
scan mode. The starting spectral sample point can be determined by ground
command. In single-scan mode the default PROM sequence for Detector 2 begins
at 148.6 cm-1 and ends at 1655 cm-1. This spectral range was used
throughout the aerobraking and Science Phasing Orbits. However, the first
five spectra samples in single-scan mode (first 10 in double-scan mode)
have very low instrument response and a very low signal-to-noise ratio.
Therefore, beginning with the mapping orbits the starting sample in
single-scan mode will be changed to 201.6 cm-1 (Det. 2) with an ending
sample of 1708.9 cm-1. The single-scan data are stored in a 148-point
array beginning at 148.6 cm-1 (Det. 2) in which either the first five
(mapping phase) or last five (aerobraking phase) samples are set to zero
or null. The double-scan data are stored in a 296-point array with
corresponding offsets and null values. The wavenumber positions for each
detector from sample 1 to 148 (single scan) or sample 1 to 296 (double
scan) are given in Table A1.
The finite size and off-axis position of the six detectors results in self-
apodization and a spectral shift that is a function of both distance from
the axis and optical frequency. The resulting full-width half-maximum
(FWHM) value is ~12.5 cm-1 for 10 cm-1 sampling at 200 cm-1 and 15.4 cm-1 at
1650 cm-1. For the corner detectors and at the highest frequency (shortest
wavelength) there is a significant departure from the ideal line width,
giving a worst-case degradation of a FWHM of ~24 cm-1. Because all of the
response functions have the same area there is no loss in signal when viewing
a smooth continuum scene like Mars. However, there will be a slight loss in
contrast of narrow spectral features due to broadening of the spectral width.
Because the self-apodization is considerable, the data are used without
further apodization. Separate fast Fourier transform (FFT) algorithms are
used for the center and edge detectors in order to partially compensate for
the different spectral shifts introduced into these detectors. These offsets
are discussed in Section 2.4.
A pointing mirror capable of rotating 360 degrees provides views to space,
both limbs, and to internal, full-aperture thermal and visible calibration
targets, as well as image motion compensation. In addition to the
spectrometer, the instrument has bore sighted bolometric thermal radiance
(4.5 to ~100 microns) and solar reflectance (0.3 to 2.7 microns) channels.
Each instrument sub-section has six instantaneous fields of view (IFOV) of
~8.5 mrad that provide a contiguous strip three elements wide with a spatial
resolution designed to be 3 km from the final MGS mapping orbit altitude of
350 km. The outputs from all TES channels are digitized at 16 bits,
processed, and formatted before being sent to the spacecraft Payload Data
Subsystem (PDS). The outputs of the interferometer receive the following
processing within the instrument before transfer to the PDS: 1) selectable
apodization; 2) Fast Fourier Transformation (FFT) of data from all six
interferometer channels; 3) correction for gain and offsets; 4) data editing
and aggregation; 5) data compression; and 6) formatting for the PDS.
A separate 1.5 cm diameter reflecting telescope, collimated with the main
telescope and using the same pointing mirror, is used for the thermal and
visible bolometer channels. These channels have similar 3x2 arrays of
detectors, that are bore sighted with the spectrometer array. The optical
system consists of a single off-axis paraboloidal mirror operating at f/8.
A reflecting resonant fork chopper operating at 30 Hz is used to separate the
solar reflectance and thermal emission bands.
2.0 SPECTROMETER CALIBRATION
2.1 SPECTROMETER ALGORITHM OVERVIEW
The measured spectra can be characterized at each wavenumber by the equation:
Vt = ( Rt - Ri ) * IRF
where,
Vt is the voltage generated by the TES looking at a target
Rt is the radiance of the target
Ri is the radiance of the instrument
IRF is the instrument response function
The radiance of the target can be determined from the above equation once
the instrument radiance and the response function are known. These parameters
are determined using observations of space and the internal reference surface
at planned time intervals. These observations give two equations of the form:
Vr = ( Rr - Ri ) * IRF
Vs = ( Rs - Ri ) * IRF
where Vr and Vs are the measured voltages viewing space and reference
respectively, Rr is derived from the measured temperature of the reference
surface, and Rs is the radiance of space (~0 W cm-2 str-1 /cm-1). These
equations can be solved for the two unknown values, Ri and IRF, giving:
Ri = ( Vs*Rr - Vr*Rs ) / ( Vs - Vr )
IRF = Vr / ( Rr - Ri )
Or the equivalent:
IRF = Vs / ( Rs - Ri )
These computed values are then used to compute the radiance of the planet
using:
Rp = ( Vp / IRF ) + Ri
2.2 SPECTROMETER ALGORITHM VERSION (V.002A)
The simultaneous determination of IRF and Ri requires Space (S) and
Reference surface (R) observations spaced closely in time. Typically these
are acquired as consecutive or interleaved observations that are termed
"SR-pairs". The IRF is assumed to vary slowly, whereas Ri can vary
throughout the orbit. Thus, the SR-pairs are only acquired several times per
orbit to determine IRF, whereas Space observations are acquired approximately
every 3-5 minutes to determine Ri.
It is necessary for the calibration that the required subsets of all the
parameters are also available. For example, the spectral values for the
planet acquired from detector 5 can only be calibrated if all other
parameters are also available for detector 5. Similarly, single-scan planet
observations are calibrated using single-scan S and R observations, and
double-scan planet observations require double-scan S and R observations.
During the aerobraking and Science Phasing Orbits the thermal state of the
TES was not stable. For example, during each spacecraft roll the Sun could
directly illuminate the reference surface. Therefore, it was not possible
to use long-term averages of IRF and Ri to reduce the noise level present
in a single determination of these parameters. In this version of the
algorithm the bounding values of IRF and Ri are simply interpolated to
determine Rp. The instrument response was not averaged over multiple
SR-pairs, nor was the Ri term smoothed to reduce noise.
The following sequence of operations was carried out for spectral
calibration:
1) Read the data associated with all the observations under consideration
2) Find all of the single and double scan SR-pairs and Space observations
(S) in the given set of observations.
3) At each SR-pair, compute the temperature of the instrument (Ti) and IRF.
For each detector:
a) Average the voltage of all the Space observations having the same
scan length. This is Vs.
b) Average the voltage of all the reference observations having the
same scan length. This is Vr. Average the reference surface
thermistor temperatures (aux_temp[1-3]) to find the average
temperature of the reference surface for this SR-pair. This is Tr.
c) Compute the radiance of the reference surface (Rr) at temperature
Tr using the Planck blackbody radiance function.
d) Compute the radiance of space (Rs) at the temperature of space
(3K), using the Planck radiance function.
e) Compute the radiance of the instrument by substituting the
calculated values in the equation:
Ri = ( Vs*Rr - Vr*Rs ) / ( Vs - Vr )
f) Compute the instrument brightness temperature (Ti) at each
spectral sample by inverting the blackbody radiance function with
radiance Ri.
g) Take the average of the instrument brightness temperatures from
spectral samples 50 through 90 (single scan; samples 100-180 double
scan), to determine a single best-fit value of Ti. This is the
temperature of this particular detector.
h) Compute IRF using the equation:
IRF = Vs / ( Rs - Ri )
If IRF equals zero or infinity for a particular spectral sample,
then average the two neighboring spectral samples to compute an IRF
value for that spectral sample.
4) Store the computed values of IRF, Ri, and Ti into one packet, tag it as
an SR-pair with its starting sclk_time and pool it among other similar
packets for SR-pairs and Space observations in ascending order of their
sclk_time. This pool is called the IRF-pool.
5) Replicate the first SR-pair as an additional SR-pair in the beginning of
the given set of observations.
6) Replicate the last SR-pair as an additional SR-pair at the end of the
given set of observations.
7) At each Space observation, compute Ti. For each detector:
a) Average the voltage of all the Space spectra in a given set of
consecutive spectra having the same scan length. This is Vs.
b) Compute radiance of space (Rs) at temperature of space (3K) using
the Planck radiance function.
c) Search in the IRF-pool to find the closest SR-pair in each
direction. Interpolate over sclk_time between the Ti of the two
bounding SR-pairs to compute an initial estimate of Ti at the
sclk_time of this Space observation.
d) Interpolate over Ti between the IRF values at the Ti's of the two
bounding SR pairs to compute the IRF at the estimated Ti of this
Space observation.
e) Compute the radiance of the instrument using the value of IRF in
the equation:
Ri = Rs - ( Vs / IRF )
f) Compute the instrument brightness temperature (Ti) at each
spectral sample by inverting the blackbody radiance function with
radiance Ri.
g) Take the average of the instrument brightness temperatures from
spectral samples 50 through 90 (single scan; samples 100 to 180
double scan) to determine a new value of Ti.
h) Store the final computed values of Ti and Ri for this Space
observation into one packet. Tag this packet as an S with its
starting sclk_time and pool it in the IRF-pool in ascending order
of its sclk_time.
8) At each planet observation, determine IRF and Ri and compute Rp. For
each detector:
a) Interpolate over sclk_time between the Ti of the two bounding SR
observations to compute Ti at this planet observation.
b) Interpolate over Ti between the IRF values at the Ti's of the two
bounding SR observations to determine the IRF at this planet
observation.
c) Interpolate over sclk_time between the Ri values of the two
bounding SR or S points to determine Ri at this planet observation.
d) If this observation had a spectral mask other than full spectral
resolution, average the Ri and IRF corresponding to the mask.
e) Use IRF and Ri to compute Rp using the equation:
Rp = ( Vp / IRF ) + Ri.
9) Write the calibrated spectra to the database.
2.3 PRECISION AND ACCURACY
The TES spectrometer has a noise equivalent spectral radiance near 1.2 x 10-8
W cm-2 str-1 cm-1. This corresponds to a signal-to-noise ratio (SNR) of 490
at 1000 cm-1 (10 microns) viewing a 270K scene. Absolute radiometric accuracy
was estimated from pre-launch data to be better than 4 x 10-8 W cm-2 str-1
cm-1.
In flight deviations are discussed in Section 6.
2.4 WAVENUMBER SAMPLE POSITION AND SPECTRAL LINE SHAPE
In an ideal interferometer with an on-axis point detector, the spectral
samples are uniformly distributed in wavenumber, and the full-width, half
maximum (FWHM) of each sample is simply determined by the optical
displacement of the Michelson mirror. The TES uses a neon bulb with a line at
0.7032 microns in the visible interferometer to sample the IR interferometer.
The ideal sample spacing of the interferometer is given by:
Sample spacing = ________1________________ (2.1)
(0.7032 x 10-4 cm)*Npts
where Npts is the number of points in the FFT.
For a large detector, the two beams of the interferometer are not in phase
over the entire areal extent of the detector, producing "self-apodization",
or widening of the instrument line shape. In addition, the path length of
the rays traveling to the off-axis portion of each detector is decreased
relative to the optical axis rays by a factor of cos theta, where theta is
the angle of the off-axis ray. As a result, the mirror must move farther to
produce interference of the off-axis rays, producing a shift of the center
frequency of each spectral sample to a higher apparent wavelength (lower
wavenumber) than its true spectral position. All six detectors are offset
from the optical axis, producing separate shifts in the spectral line
position, shape, and modulation efficiency of each detector.
The TES flight software processes the interferogram data with prime factors
FFTs that use a different number of points for the center and edge detectors
respectively. These FFT's were selected to produce a slightly different
spacing that partially compensates for the different spectral offsets due to
self-apodization between the edge and center detectors. The number of points
and sample spacing is given in Table 2-1.
Table 2-1.
Edge Detectors (1,3,4,6) Center Detectors (2,5)
Single Scan Double Scan Single Scan Double Scan
Npts in FFT 1350 2700 1344 2688
Sample Spacing 10.53 cm-1 5.267 cm-1 10.58 cm-1 5.290 cm-1
Sample 1 Position
(ideal) 147.47 cm-1 147.47 cm-1 148.13 cm-1 148.13 cm-1
Sample 148 (single;
296 double) Position
(ideal) 1695.95 cm-1 1701.22 cm-1 1703.52 cm-1 1708.81cm-1
(Note: the sample spacing used to compute the sample position of the
archived data is computed in full digital precision using 0.7032 microns in
Eq. 2.1.)
A numerical model has been developed by Co-Investigator Stillman Chase to
model the self-apodization effects and to determine the true spectral
position, FWHM, and spectral line shape of each sample. Interferogram data of
Mars were collected immediately after Mars orbit insertion, and the
atmospheric CO2 data were used to verify Chase's model of line shape and
position. Because the focal plane is symmetric in the cross-track direction
(e.g. detectors 1 and 3 are symmetrically located relative to the optical
axis), the position and FWHM are identical for detector pairs 1 and 3 and
detector pairs 4 and 6. The sample position offset was calculated for each
detector, taking into account the actual prime factor FFT used for each
detector. Examples of the offset and the actual sample position calculated
with this offset and the actual prime factors FFT used for the double-scan
samples 1 and 296 are given in Table 2-2. The full set of sample offsets for
each detector are tabulated in Table A1 in the Appendix. The sample
positions are identical for single and double scans. The modeled full-width
half-maximum values for double scan observations are tabulated in Table A2.
The full-width half-maximum values for single scan data are twice the double
scan values.
Table 2-2. Double Scan Self-Apodization
Edge Detectors (1,3) Center Detector (2)
Sample 1 Self-Apodization
Offset 1.19 cm-1 0.44 cm-1
Sample 296 Self-Apodization
Offset 14.00 cm-1 5.45 cm-1
Sample 1 (actual) 148.66 cm-1 148.57 cm-1
Sample 296 (actual) 1715.22 cm-1 1714.26 cm-1
3.0 VISIBLE BOLOMETER CALIBRATION
3.1 VISIBLE BOLOMETER ALGORITHM OVERVIEW
The in-flight calibration of the TES visible bolometer is performed for each
detector in the following stages.
1) Use observations of the internal TES reference calibration lamp and space
to determine the instrument response function (IRF) and the zero-level
radiance (background).
2) Convert each target observation to calibrated radiance using the IRF and
background.
3) Compute the Lambert albedo using the calibrated radiance, the Sun-Mars
distance, and the incidence angle.
3.2 VISIBLE BOLOMETER ALGORITHM VERSION V.002A
1)Read the data associated with all the observations to be calibrated. For
each observation this includes:
sclk_time Spacecraft Clock Time
pnt_view Pointing Angle View
det_mask Detector mask
scan_len Scan length
solar_distance Solar distance
aux_temps[1-3] Temperature of the reference surface
temps[1] Temperature of the detector array
detector Detector Number
vbol Raw voltages from visible bolometer
incidence Solar incidence angle at the target
latitude Latitude of the target
2) Separate the data into single and double scan modes. Each mode is
calibrated separately.
3) Sort the data on ascending sclk_time.
4) Find all distinct groups of space observations (S) in the given set of
observations. To improve on noise-reduction, only space observations with
three or more consecutive space spectra are used; other space views with
fewer than three space spectra are discarded.
At each set of Space observations for each detector:
a) Average the visible bolometer voltage (vbol) of all space
observations in this set. This is called the background.
b)Store the background value with the beginning sclk_time of this
set in one packet. Tag it as an S, and pool it among similar packets
in ascending order of its sclk_time.
5) Find all distinct groups of consecutive visible bolometer reference
observations (REFAn) within the given set of observations, where n refers to
the calibration lamp number 1 or 2.
At each REFAn for each detector:
a) Compute the IRF for each internal lamp observation:
i) Average the vbol for all consecutive observations within
this set of lamp observations.
ii) Correct vbol for the background signal by subtracting the
background from the nearest Space observation to give the
lamp_voltage.
iii) Average the temperature of the detector array (temps[1])
to yield detector temperature (det_temp) in degrees C.
iv) Average the three reference surface temperatures
(aux_temps[1-3]) to yield lamp temperature (lamp_temp).
v) Choose the lamp absolute radiance at 28.2 C
(lamp_absolute) for this lamp and scan length (single or
double) using the values in the TES Calibration Report.
vi) Select the RL/T for the lamp that was observed.
vii) Compute the actual lamp radiance (RL)(TL)cal for each
detector at the lamp temperature using lamp_absolute, the
variation in lamp radiance (RL) with temperature (dRL/dTL,)
from the TES Calibration Report, and the difference (TL)
between lamp_temp and the internal lamp absolute calibration
temperature (28.2 degrees). The lamp radiance equation is:
lamp_radiance = lamp_absolute +(dRL/dT * (lamp_temp -28.2)))
vii) Compute IRF using the equation:
IRF = lamp_voltage / lamp_radiance
b) Store the IRF, the background voltage, and the detector
temperature in one packet. Tag it as a REFAn packet and pool it
among other REFAn packets In ascending order of their beginning
sclk_time.
6) Replicate the first REFAn as an additional REFAn in the beginning of the
given set.
7) Replicate the last REFAn as an additional REFAn at the end of the given
set.
8) At each target (planet) observation, compute the calibrated visible
bolometer radiance (cal_vbol). The visible bolometer response function must
be corrected at each planet observation to account for changes in the
detector temperature between the lamp and planet observations. In order to
avoid discrete jumps at each lamp observation, it is necessary to interpolate
IRF and the detector temperature between successive lamp views. This
baseline IRF is then corrected to the actual IRF at each planet observation
using df/dTD, and d2f/dTD2, along with the coefficients in the TES
Calibration Report and the detector temperature difference between the
baseline lamp observations and the planet observations.
This is done by:
a) Search the pool of REFAn observations to find the two bounding
observations.
b) Search the pool of Space observations to find the two bounding
observations.
For each detector:
i) Interpolate linearly on sclk_time between this
observation and two bounding REFAn times to compute the
baseline IRF.
ii) Interpolate linearly on sclk_time between this
observation and two bounding REFAn times to get the baseline
detector temperature and the background for this observation.
iii) Determine dIRF/dT and d2IRF/dT2 using the calibration
coefficients determined pre-launch and the equations:
dIRF/dT = 3*af*(detector_temp)2 + 2*bf*detector_temp + cf
d2IRF/dT2 = 6*af*detector_temp + 2*bf
where,
af = 'alpha' of the visual bolometer from the TES
Calibration Report.
bf = 'beta' of the visual bolometer from the TES
Calibration Report.
cf = 'chi' of the visual bolometer from the TES
Calibration Report.
iv) Get the actual detector temperature (temps[1]) for this
observation.
v) Calculate delta T by subtracting the baseline detector
temperature value from the actual value.
vi) Correct IRF for this detector temperature value by the
equation:
Corr_IRF = IRF + dIRF/dT *deltaT + d2IRF/dT2 * deltaT2 / 2!
vii) Compute cal_vbol using the equation:
cal_vbol = ( vbol - background ) / Corr_IRF
9) Compute Lambert albedo.
a) Extract incidence angle and solar distance from the database.
Convert solar_distance to Astronomical Units.
b) Compute albedo using the equation:
lambert_alb = cal_vbol / (( Sun_absolute / solar_distance2)
*cos(incidence_angle))
where Sun_absolute is the solar radiance at 1 A.U. integrated over
the TES visible bolometer relative spectral response, and is equal to
1.666 x 10-2 W cm-2 str-1
Note: The cos(incidence_angle) in the denominator can lead to division by
small numbers (including zero), generating highly inaccurate values for the
albedo. To avoid this problem, the Lambert albedo is not computed for
incidence angles >88 degrees.
10) Write cal_vbol and lambert_alb to the database.
3.3 PRECISION AND ACCURACY
The precision, zero-level offset, and absolute accuracy of the in-flight
calibration was determined using data from cruise (test tes_c2a and tes_c9a)
and orbits P3 through P460.
The in-flight precision (noise level) of the calibrated radiance measurements
was determined using observations of deep space acquired away from Mars
during spacecraft rolls prior to and after periapsis.. The internal lamp was
not used because its temperature increases if left on for an extended period
of time, which changes its brightness level. The data used were acquired on
orbits P95 through P100 (no data were available for orbit P99) at a Mars-Sun
distance of 2.068*10-8 km (1.382 A.U.). Only observations well away from
Mars, selected by constraining the height of the tangent point of the
observation to be >2000 km above the martian surface, were included. The
sigma values of the calibrated radiance of the space observations are given
in Table 3-1.
Table 3-1
Detector Sigma (Radiance) Mean Zero-level Radiance
(x10-6 W cm-2 str-1) (x10-6 W cm-2 str-1)
1 3.62 0.914
2 3.74 1.03
3 3.77 1.07
4 3.73 0.676
5 3.67 0.942
6 3.59 1.00
The 1 sigma variation in the zero-level radiance is ~3.75 x10-6 W cm-2 str-1
for all six detectors. This value is consistent with the variation in the
internal lamp brightness measured pre-flight (1-6 x10-6 W cm-2 str-1; Table
4-6). A Lambertian surface with a reflectivity of 1.0 would have a radiance
of 8.718 x10-3 W cm-2 str-1 at the Mars-Sun distance of these observations,
measured at normal incidence angle. The 1 sigma precision of the visible
bolometer calibrated radiance corresponds to a noise-equivalent delta
reflectivity (NE_R) of 0.0004, and is equivalent to an SNR of 2100 for a
surface with unit reflectivity.
The zero-level radiance as a function of time is determined by the
calibration algorithm using periodic observations of space and the internal
lamps to correct for detector response and offset drifts. Table 3-1 gives the
mean zero-level radiance of the space observations. This radiance is a
factor of nearly four lower than the 1 sigma variation of the data,
indicating that there are no measurable systematic biases introduced into the
data by incorrectly removing the variations in detector response and lamp
brightness with time and temperature. In addition, no systematic offsets,
trends, or discrete changes in value at space or lamp observations were
observed in the calibrated radiance of space. From these data it is concluded
that the calibration algorithm is accurately accounting for variations in
detector response and lamp brightness with time and temperature at the noise
level of the instrument. The 3 sigma accuracy of the zero-level radiance is
approximately +/- 1*10-5 W cm-2 str-1 for all six detectors, consistent with
the values in Table 3-1.
The data given in Table 3-1 were acquired of a black target (space) with zero
signal and therefore do not provide a measure of the true absolute
calibration for bright surfaces. This can only be determined by observations
of a bright source with known radiance. No surfaces of known brightness exist
on Mars to verify the absolute radiance. In addition, because the internal
calibration lamps are used in the calibration, they do not provide an
independent test of the absolute radiance. However, it is possible to
estimate changes in the lamp output with time by comparing the measured lamp
voltage, corrected for background, with the pre-flight measurements as a
function of lamp and detector temperature.
The pre-flight thermal vacuum tests (albm tests) and the in-flight data from
cruise (tests tes_c2 and tes_c9, and orbits 12, 15, 95-98, 100, 222, and 460)
indicate a 0-~3% increase in the measured signal for detector temperatures of
~10-15 degrees C, and an increase of ~3-6% near 0 C relative to the
pre-flight measurements. This change can be due to a combination of: 1) a
change in the alignment of the lamp relative to the detectors; 2) an increase
in lamp 1 brightness; 3) a change in the chopper alignment or timing; or
4) an increase in detector response. Of these, a change in alignment is
least likely because no decrease in lamp signal was observed for any
detector. A possible change in lamp 1 brightness was investigated using the
ratio of lamp 1 to lamp 2 for pre-flight and in-flight data. Lamp 2 was
observed once during cruise (test tes_c9) and once in orbit early in the
mission (orbit P59). The lamp ratio, adjusted for lamp temperature, is
unchanged for detectors 3 and 6, is ~1% higher for detectors 1, 4, and 5,
and is ~1% lower for detector 2. The change in lamp 1 relative to lamp 2,
averaged for all detectors, is ~0.7%, and is essentially constant with
temperature. Based on experience at SBRS on the Galileo PPR instrument, the
stability of these lamps is estimated to be +/- 0.5% on a long-term (years)
basis and +/- 0.15% on a short term (hours) basis. The ratio of the two TES
lamps is consistent with these stability values. Furthermore, both lamps
would have to have increased in brightness to account for changes in the
lamp 1 signal levels. It is therefore concluded that the changes in lamp 1
signal level are not associated with changes in lamp output.
It is more likely that either the detector response with temperature has
varied in flight, which would account for both the variations between
detectors and the relatively large changes over temperature, or that the
chopper alignment or timing has changed slightly. Neither of these cases
will affect the absolute calibration because the detector views both Mars and
the lamps with the same chopper and detector characteristics. Indeed, the
on-board calibration lamps are specifically intended to remove these effects.
It is concluded that the absolute calibration is most likely ~1% relative to
the pre-flight calibration of the internal lamps. The relative accuracy from
orbit P15 to P460 is ~0.5%.
4.0 THERMAL BOLOMETER CALIBRATION
4.1 THERMAL BOLOMETER ALGORITHM OVERVIEW
The measured integrated radiance can be characterized by the following
equation:
Vt = ( Rt - Ri ) * IRF
where,
Vt is the voltage generated by the TES looking at a target
Rt is the integrated radiance of the target
Ri is the integrated radiance of the instrument
IRF is the instrument response function
The integrated radiance of the target is determined from the above equation
once the instrument radiance and the response function are known. These
parameters are determined using observations of space and the internal
reference surface at planned time intervals. These observations give two
equations of the form:
Vr = ( Rr - Ri ) * IRF
Vs = ( Rs - Ri ) * IRF
where Vr and Vs are the measured voltages viewing space and reference
respectively, Rr is derived from the measured temperature of the reference
surface, and Rs is the integrated radiance of space (~0 W cm-2 str-1). These
equations can be solved for the two unknown values, Ri and IRF, giving:
Ri = ( Vs*Rr - Vr*Rs ) / ( Vs - Vr )
IRF = Vr / ( Rr - Ri )
Or:
IRF = Vs / ( Rs - Ri )
These computed values then are used to compute the radiance of the planet:
Rp = ( Vp / IRF ) + Ri
4.2 THERMAL BOLOMETER ALGORITHM VERSION V001.A
The simultaneous determination of IRF and Ri requires space (S) and reference
surface (R) observations spaced closely in time. Typically these are acquired
as consecutive or interleaved observations that are termed "SR-pairs". The
IRF is assumed to vary slowly, whereas Ri can vary throughout the orbit.
Thus, the SR-pairs are only acquired several times per orbit to determine
IRF, whereas Space observations are acquired approximately every 3-5 minutes
to determine Ri.
Prior to calibration, the weighted integrated radiance as a function of scene
temperature is computed by convolving the instrument relative spectral
response with the blackbody radiance at each wavenumber from 0 through 2500
with a step of 2 wavenumbers. The relative spectral response of the TES
thermal bolometer was determined pre-launch and is given in the TES
Calibration Report. The integrated radiance is computed for temperature
values from 60K through 400K with a step of 0.01 degrees. A look-up table
consisting of two columns: temperature and weighted integrated radiance, is
stored in a separate file, and is used to convert brightness temperature (TB)
to radiance and radiance to TB.
The following sequence of operations is carried out for spectral calibration:
1) Read the data associated with all the observations under consideration.
2) Find all of the single and double scan SR-pairs and Space observations (S)
in the given set of observations.
3) At each SR-pair, compute the temperature of the instrument (Ti) and IRF.
For each detector:
a) Average the voltage of all the Space observations having the same
scan length. This is Vs.
b) Average the voltage of all the reference observations having the
same scan length. This is Vr. Average the reference surface
thermistor temperatures (aux_temp[1-3]) to find the average
temperature of the reference surface for this SR-pair. This is Tr.
c) Compute the radiance of the reference surface (Rr) at temperature
Tr using the TB-to-radiance look-up table.
d) Assume the radiance of space (Rs) to be equal to zero.
e) Compute IRF using the equation:
IRF = Vs / ( Rs - Ri)
f) Compute the integrated radiance of the instrument by substituting
the calculated values in the equation:
Ri = ( Vs*Rr - Vr*Rs ) / ( Vs - Vr )
g) Compute the instrument brightness temperature of the instrument
(Ti) from the radiance Ri using the radiance-to-brightness
temperature look-up table.
4)Store the computed values of IRF and Ti into one packet, tag it as an SR-
pair with its starting sclk_time and pool it among other similar packets for
SR-pairs and Space observations in ascending order of their sclk_time. This
pool is called the IRF-pool.
5) Replicate the first SR-pair as an additional SR-pair in the beginning of
the given set of observations.
6) Replicate the last SR-pair as an additional SR-pair at the end of the
given set of observations.
7) At each set of Space observations, compute Vs. Vs is used to compute the
radiance of the instrument (Ri) in the planet calibration using the equation:
Ri = Rs - ( Vs / IRF )
For each detector:
a) Average the voltage of all the Space observations in a given set
of consecutive observations having the same scan length. This is Vs.
b) Store the value of Vs for this Space observation into one packet,
tag this packet as an S with its starting sclk_time, and pool it in
ascending order of its sclk_time.
8) At each planet observation compute Rp. For each detector:
a) Interpolate linearly over sclk_time between the IRF values at the
two bounding SR or S observations to determine the IRF at this planet
observation.
b) Interpolate linearly over sclk_time between the Vs values at the
two bounding SR or S observations to compute Vs at this planet
observation.
c) Compute Rp from IRF and Vs using:
Rp = ( Vp / IRF ) + Ri.
Replacing Ri in this equation with Ri = Rs - ( Vs / IRF )
gives:
Rp = Rs + ( Vp - Vs ) / IRF
d) Convert Rp to the brightness temperature of the planet (Tp) using
the radiance-to-brightness temperature look-up table.
9) Write the brightness temperature to the database.
5.0 SURFACE TEMPERATURE DETERMINATION
A simple algorithm was performed on each TES spectrum in order to estimate
the effective surface kinetic temperature using the TES spectrometer data.
The primary use of this temperature is for emissivity determination where
only a first-order estimate of the surface temperature is required. No
attempt is made to model mixtures of surface materials at different kinetic
temperatures, nor to remove atmospheric effects.
This algorithm is based on the desire to use the entire spectrum to locate
the region with the highest emissivity, where the brightness temperature will
provide the closest approximation to the surface kinetic temperature. In
practice, both in laboratory measurements and in TES data, the short-
wavelength region (<8 microns) often has the highest emissivity.
Unfortunately, at low temperatures (<~225 K), the short-wavelength region of
the spectrum has significant noise and measurements in this spectral region
are unreliable. Thus, it is necessary to have a flexible algorithm that uses
the best available data to estimate surface temperature.
1) Convert the calibrated radiance to brightness temperature at each
wavenumber assuming that: a) the emissivity is unity (temp. = TB); and b) the
emissivity is 0.97 and dividing the calibrated radiance by this value before
determining the brightness temperature (temp. = TB'). Filter the brightness
temperatures using a unity-weight filter 7 samples wide to reduce noise
effects.
2) Find the maximum brightness temperature over the sample ranges from:
a) 300 to 1350 cm-1, excluding the region from 500 cm-1 to 800 cm-1
where atmospheric CO2 has strong absorptions. This range was
selected to include both the long and short wavelength portions of
the spectrum, and to include the wavenumber typically with the
highest brightness temperature (~1300 cm-1) as determined by both the
Mariner 9 IRIS and the preliminary TES data.
b) 300 to 500 cm-1 only. This range covers only the long wavelength
portion of the spectrum.
3) If TB is greater than or equal to T2 (225 K), set Tsurface to TB; If TB'
is less than or equal to T1 (215 K) set Tsurface to TB'. Otherwise, provide a
smooth transition between these to cases by setting Tsurface to weighted
average of TB and TB'. Weighting is determined by:
Weight1 = 1 - ( (T2-TB) / (T2-T1) )
Weight2 = 1 - ( (TB'-T1) / (T2-T1) )
If Weight1 or Weight2 < 0, then they are set to 0.
4) Finally:
Tsurface = ( (TB*Weight1) + (TB'*Weight2) ) / (Weight1 + Weight2)
6.0 DATA QUALITY/ANOMALIES
6.1 SPECTRAL RINGING
The TES spectra occasionally exhibit a high frequency "ringing" in which the
amplitude of the spectrum oscillates from one spectral point to the next.
This ringing has been found to occur when there is a large change in scene
temperature from one observation to the next. These large temperature
variations frequently occur during observations of Mars acquired at large
distances where there is a significant change in position on the planet
between successive observations. The TES analog electronics are designed to
keep the DC (base) level of interferogram centered at zero volts. However,
when the radiance of the scene changes, the base level of the interferogram
changes and there is a finite time required for the electronics to
compensate. The frequency of the TES interferogram information band is
10-100 Hz, so the electronics are designed to pass all information within
this band to avoid filtering out signal information. Therefore, the base
correction electronics are designed to have a time constant >0.1 seconds to
avoid altering the true interferogram spectral information. There are only
0.2 seconds between the end of one interferogram and the start of the next,
so if the scene changes temperature rapidly between observations, then the
electronics will not have sufficient time to fully recenter the base level of
the interferogram before the start of the next scan. In this case the
interferogram will still be settling (or rising) toward the base level during
the first ~0.1-0.2 seconds of the interferogram scan. This settling results
in a discontinuity at the beginning of the scan due to the fact that the
first point is significantly greater (or less) than zero. Because this spike
occurs at the beginning of the scan, it always produces a sine wave at the
highest possible frequency in the transformed spectrum. As a result, a sine
wave with a point-to-point variation is superimposed on the data. The
interferogram base level can be increasing or decreasing if the temperature
of the current scan is higher or lower respectively than the previous scan.
Therefore, the phase of the superimposed sine wave can vary by 180 degrees.
An algorithm has been developed to artificially remove the spectral ringing
by transforming the spectral data back to frequency and removing the end
points of the interferogram. However, this approximation lowers the spectral
resolution of the data, and has not been applied to the calibrated spectra
on the TES CD-ROMS in this release. A more sophisticated approach is being
developed using the measured time constant of the TES electronics to model
the settling of the interferogram toward the base level. This correction will
be applied in later releases of the TES data.
Up to 80% of the low resolution data acquired away from periapsis can show
significant ringing. Even data that do not exhibit a visible ringing can
have higher than expected power in the highest frequency, suggesting that
some "ringing" is present. The ringing effect should be significantly
reduced when the TES is operated in the planned mode during mapping.
6.2 SPECTROMETER NON-ZERO BACKGROUND CALIBRATED RADIANCE
In-flight observations indicate that a small, systematic calibration offset
with a magnitude of ~1x10-7 W cm-2 str-1 cm-1 is present in the TES data
presented on this CD-ROM. This error is primarily due to slight variations
in the instrument background energy between observations taken of space at an
angle of -90 aft (0 degrees = nadir) for calibration and those viewing
the planet at angle other than -90 degrees. This error is not significant
for surface observations at temperatures above ~240 K. However, for
observations of the polar caps and the atmosphere above the limbs, where the
radiance is low, this error can be significant.
Observations have been collected to characterize the variation in the
calibration offset with pointing mirror angle and instrument temperatures.
Models are being developed to account for this effect. This correction will
be applied in later releases of the TES data.
7.0 REFERENCES
Christensen, P.R., D.L. Anderson, J. S.C. Chase, R.N. Clark, H.H. Kieffer,
M.C. Malin, J.C. Pearl, J. Carpenter, N. Bandiera, F.G. Brown, and S.
Silverman, Thermal emission spectrometer experiment: Mars Observer mission,
J. Geophys. Res., 97, 7719-7734, 1992.
APPENDIX
Table A1. Spectrometer Wavenumber Position - Double Scan
Sample Number Det. 1 Det. 2 Det. 3 Det. 4 Det. 5 Det. 6
Single Double
scan scan
1 1 148.66 148.57 148.66 148.36 148.45 148.36
2 153.99 153.89 153.99 153.66 153.74 153.66
2 3 159.31 159.21 159.31 158.95 159.06 158.95
4 164.61 164.50 164.61 164.25 164.35 164.25
3 5 169.94 169.82 169.94 169.58 169.64 169.58
6 175.23 175.11 175.23 174.87 174.96 174.87
4 7 180.56 180.43 180.56 180.17 180.25 180.17
8 185.86 185.75 185.86 185.47 185.57 185.47
5 9 191.19 191.04 191.19 190.77 190.86 190.77
10 196.51 196.36 196.51 196.06 196.15 196.06
6 11 201.81 201.65 201.81 201.36 201.47 201.36
12 207.14 206.97 207.14 206.69 206.76 206.69
7 13 212.43 212.29 212.43 211.98 212.08 211.98
14 217.76 217.58 217.76 217.28 217.37 217.28
8 15 223.06 222.90 223.06 222.58 222.66 222.58
16 228.38 228.19 228.38 227.87 227.98 227.87
9 17 233.68 233.52 233.68 233.17 233.28 233.17
18 239.01 238.81 239.01 238.50 238.60 238.50
10 19 244.31 244.13 244.31 243.79 243.89 243.79
20 249.60 249.45 249.60 249.09 249.18 249.09
11 21 254.93 254.74 254.93 254.39 254.50 254.39
22 260.23 260.06 260.23 259.69 259.79 259.69
12 23 265.55 265.35 265.55 264.98 265.11 264.98
24 270.85 270.67 270.85 270.28 270.40 270.28
13 25 276.18 275.99 276.18 275.58 275.69 275.58
26 281.47 281.28 281.47 280.90 281.01 280.90
14 27 286.80 286.60 286.80 286.20 286.30 286.20
28 292.10 291.89 292.10 291.50 291.62 291.50
15 29 297.42 297.21 297.42 296.79 296.91 296.79
30 302.72 302.50 302.72 302.09 302.20 302.09
16 31 308.02 307.82 308.02 307.39 307.52 307.39
32 313.35 313.14 313.35 312.69 312.81 312.69
17 33 318.64 318.43 318.64 317.98 318.13 317.98
34 323.97 323.75 323.97 323.28 323.42 323.28
18 35 329.27 329.04 329.27 328.58 328.71 328.58
36 334.59 334.36 334.59 333.87 334.03 333.87
19 37 339.89 339.65 339.89 339.20 339.32 339.20
38 345.19 344.97 345.19 344.50 344.64 344.50
20 39 350.51 350.30 350.51 349.79 349.93 349.79
40 355.81 355.59 355.81 355.09 355.23 355.09
21 41 361.14 360.91 361.14 360.39 360.55 360.39
42 366.44 366.20 366.44 365.68 365.84 365.68
22 43 371.73 371.52 371.73 370.98 371.16 370.98
44 377.06 376.81 377.06 376.28 376.45 376.28
23 45 382.36 382.13 382.36 381.58 381.74 381.58
46 387.68 387.45 387.68 386.87 387.06 386.87
24 47 392.98 392.74 392.98 392.17 392.35 392.17
48 398.28 398.06 398.28 397.47 397.67 397.47
25 49 403.60 403.35 403.60 402.76 402.96 402.76
50 408.90 408.67 408.90 408.09 408.25 408.09
26 51 414.23 413.96 414.23 413.39 413.57 413.39
52 419.52 419.28 419.52 418.68 418.86 418.68
27 53 424.85 424.60 424.85 423.98 424.18 423.98
54 430.15 429.89 430.15 429.28 429.47 429.28
28 55 435.45 435.21 435.45 434.57 434.76 434.57
56 440.77 440.50 440.77 439.87 440.08 439.87
29 57 446.07 445.82 446.07 445.17 445.37 445.17
58 451.40 451.14 451.40 450.47 450.69 450.47
30 59 456.69 456.43 456.69 455.76 455.98 455.76
60 462.02 461.75 462.02 461.06 461.27 461.06
31 61 467.32 467.05 467.32 466.36 466.59 466.36
62 472.64 472.37 472.64 471.65 471.89 471.65
32 63 477.94 477.66 477.94 476.95 477.21 476.95
64 483.24 482.98 483.24 482.25 482.50 482.25
33 65 488.56 488.30 488.56 487.54 487.79 487.54
66 493.86 493.59 493.86 492.84 493.11 492.84
34 67 499.19 498.91 499.19 498.17 498.40 498.17
68 504.49 504.20 504.49 503.47 503.69 503.47
35 69 509.81 509.52 509.81 508.76 509.01 508.76
70 515.11 514.84 515.11 514.06 514.30 514.06
36 71 520.41 520.13 520.41 519.36 519.62 519.36
72 525.73 525.45 525.73 524.65 524.91 524.65
37 73 531.03 530.74 531.03 529.95 530.20 529.95
74 536.36 536.06 536.36 535.25 535.52 535.25
38 75 541.65 541.35 541.65 540.54 540.81 540.54
76 546.98 546.67 546.98 545.84 546.13 545.84
39 77 552.28 551.99 552.28 551.14 551.42 551.14
78 557.61 557.28 557.61 556.43 556.71 556.43
40 79 562.90 562.60 562.90 561.73 562.03 561.73
80 568.23 567.89 568.23 567.03 567.32 567.03
41 81 573.53 573.21 573.53 572.36 572.64 572.36
82 578.85 578.50 578.85 577.65 577.93 577.65
42 83 584.15 583.82 584.15 582.95 583.22 582.95
84 589.48 589.15 589.48 588.25 588.55 588.25
43 85 594.77 594.44 594.77 593.54 593.84 593.54
86 600.07 599.76 600.07 598.84 599.16 598.84
44 87 605.40 605.05 605.40 604.14 604.45 604.14
88 610.69 610.37 610.69 609.43 609.74 609.43
45 89 616.02 615.66 616.02 614.73 615.06 614.73
90 621.32 620.98 621.32 620.03 620.35 620.03
46 91 626.65 626.30 626.65 625.32 625.67 625.32
92 631.94 631.59 631.94 630.65 630.96 630.65
47 93 637.27 636.91 637.27 635.95 636.25 635.95
94 642.57 642.20 642.57 641.25 641.57 641.25
48 95 647.86 647.52 647.86 646.54 646.86 646.54
96 653.19 652.81 653.19 651.84 652.18 651.84
49 97 658.49 658.13 658.49 657.14 657.47 657.14
98 663.81 663.42 663.81 662.43 662.76 662.43
50 99 669.11 668.74 669.11 667.73 668.08 667.73
100 674.44 674.06 674.44 673.03 673.37 673.03
51 101 679.74 679.35 679.74 678.32 678.69 678.32
102 685.06 684.67 685.06 683.62 683.98 683.62
52 103 690.36 689.96 690.36 688.95 689.27 688.95
104 695.66 695.28 695.66 694.25 694.59 694.25
53 105 700.98 700.57 700.98 699.54 699.88 699.54
106 706.28 705.90 706.28 704.84 705.20 704.84
54 107 711.61 711.22 711.61 710.14 710.50 710.14
108 716.90 716.51 716.90 715.43 715.79 715.43
55 109 722.23 721.83 722.23 720.73 721.11 720.73
110 727.53 727.12 727.53 726.03 726.40 726.03
56 111 732.82 732.44 732.82 731.32 731.72 731.32
112 738.15 737.76 738.15 736.62 737.01 736.62
57 113 743.45 743.05 743.45 741.95 742.30 741.95
114 748.78 748.37 748.78 747.24 747.62 747.24
58 115 754.07 753.66 754.07 752.54 752.91 752.54
116 759.37 758.98 759.37 757.84 758.23 757.84
59 117 764.70 764.27 764.70 763.14 763.52 763.14
118 769.99 769.59 769.99 768.43 768.81 768.43
60 119 775.32 774.91 775.32 773.73 774.13 773.73
120 780.62 780.20 780.62 779.03 779.42 779.03
61 121 785.94 785.52 785.94 784.32 784.74 784.32
122 791.24 790.81 791.24 789.62 790.03 789.62
62 123 796.54 796.13 796.54 794.92 795.32 794.92
124 801.86 801.42 801.86 800.24 800.64 800.24
63 125 807.16 806.74 807.16 805.54 805.93 805.54
126 812.49 812.06 812.49 810.84 811.25 810.84
64 127 817.79 817.35 817.79 816.13 816.54 816.13
128 823.11 822.68 823.11 821.43 821.83 821.43
65 129 828.41 827.97 828.41 826.73 827.16 826.73
130 833.71 833.29 833.71 832.03 832.45 832.03
66 131 839.03 838.58 839.03 837.32 837.77 837.32
132 844.33 843.90 844.33 842.62 843.06 842.62
67 133 849.66 849.22 849.66 847.92 848.35 847.92
134 854.95 854.51 854.95 853.21 853.67 853.21
68 135 860.25 859.83 860.25 858.51 858.96 858.51
136 865.58 865.12 865.58 863.81 864.28 863.81
69 137 870.88 870.44 870.88 869.10 869.57 869.10
138 876.20 875.73 876.20 874.43 874.86 874.43
70 139 881.50 881.05 881.50 879.73 880.18 879.73
140 886.80 886.37 886.80 885.03 885.47 885.03
71 141 892.12 891.66 892.12 890.32 890.79 890.32
142 897.42 896.98 897.42 895.62 896.08 895.62
72 143 902.75 902.27 902.75 900.92 901.37 900.92
144 908.04 907.59 908.04 906.21 906.69 906.21
73 145 913.37 912.88 913.37 911.51 911.98 911.51
146 918.67 918.20 918.67 916.81 917.27 916.81
74 147 923.96 923.49 923.96 922.10 922.59 922.10
148 929.29 928.81 929.29 927.40 927.88 927.40
75 149 934.59 934.13 934.59 932.70 933.20 932.70
150 939.92 939.43 939.92 937.99 938.49 937.99
76 151 945.21 944.75 945.21 943.32 943.79 943.32
152 950.51 950.04 950.51 948.62 949.11 948.62
77 153 955.84 955.36 955.84 953.92 954.40 953.92
154 961.13 960.65 961.13 959.21 959.72 959.21
78 155 966.46 965.97 966.46 964.51 965.01 964.51
156 971.76 971.26 971.76 969.81 970.30 969.81
79 157 977.08 976.58 977.08 975.10 975.62 975.10
158 982.38 981.90 982.38 980.40 980.91 980.40
80 159 987.68 987.19 987.68 985.70 986.23 985.70
160 993.01 992.51 993.01 990.99 991.52 990.99
81 161 998.30 997.80 998.30 996.29 996.81 996.29
162 1003.63 1003.12 1003.63 1001.59 1002.13 1001.59
82 163 1008.93 1008.41 1008.93 1006.88 1007.42 1006.88
164 1014.22 1013.73 1014.22 1012.18 1012.74 1012.18
83 165 1019.55 1019.05 1019.55 1017.48 1018.03 1017.48
166 1024.85 1024.34 1024.85 1022.78 1023.32 1022.78
84 167 1030.17 1029.66 1030.17 1028.10 1028.64 1028.10
168 1035.47 1034.95 1035.47 1033.40 1033.93 1033.40
85 169 1040.77 1040.27 1040.77 1038.70 1039.25 1038.70
170 1046.09 1045.56 1046.09 1043.99 1044.54 1043.99
86 171 1051.39 1050.88 1051.39 1049.29 1049.83 1049.29
172 1056.72 1056.17 1056.72 1054.59 1055.15 1054.59
87 173 1062.01 1061.49 1062.01 1059.88 1060.44 1059.88
174 1067.34 1066.82 1067.34 1065.18 1065.76 1065.18
88 175 1072.64 1072.11 1072.64 1070.48 1071.06 1070.48
176 1077.94 1077.43 1077.94 1075.77 1076.35 1075.77
89 177 1083.26 1082.72 1083.26 1081.07 1081.67 1081.07
178 1088.56 1088.04 1088.56 1086.37 1086.96 1086.37
90 179 1093.89 1093.33 1093.89 1091.67 1092.25 1091.67
180 1099.18 1098.65 1099.18 1096.99 1097.57 1096.99
91 181 1104.48 1103.97 1104.48 1102.29 1102.86 1102.29
182 1109.81 1109.26 1109.81 1107.59 1108.18 1107.59
92 183 1115.10 1114.58 1115.10 1112.88 1113.47 1112.88
184 1120.40 1119.87 1120.40 1118.18 1118.76 1118.18
93 185 1125.73 1125.19 1125.73 1123.48 1124.08 1123.48
186 1131.03 1130.48 1131.03 1128.77 1129.37 1128.77
94 187 1136.35 1135.80 1136.35 1134.07 1134.69 1134.07
188 1141.65 1141.12 1141.65 1139.37 1139.98 1139.37
95 189 1146.95 1146.41 1146.95 1144.66 1145.27 1144.66
190 1152.27 1151.73 1152.27 1149.96 1150.59 1149.96
96 191 1157.57 1157.02 1157.57 1155.26 1155.88 1155.26
192 1162.90 1162.34 1162.90 1160.56 1161.20 1160.56
97 193 1168.19 1167.63 1168.19 1165.85 1166.49 1165.85
194 1173.49 1172.95 1173.49 1171.15 1171.78 1171.15
98 195 1178.82 1178.24 1178.82 1176.48 1177.10 1176.48
196 1184.11 1183.57 1184.11 1181.77 1182.39 1181.77
99 197 1189.44 1188.89 1189.44 1187.07 1187.72 1187.07
198 1194.74 1194.18 1194.74 1192.37 1193.01 1192.37
100 199 1200.04 1199.50 1200.04 1197.66 1198.30 1197.66
200 1205.36 1204.79 1205.36 1202.96 1203.62 1202.96
101 201 1210.66 1210.11 1210.66 1208.26 1208.91 1208.26
202 1215.99 1215.40 1215.99 1213.56 1214.23 1213.56
102 203 1221.28 1220.72 1221.28 1218.85 1219.52 1218.85
204 1226.58 1226.01 1226.58 1224.15 1224.81 1224.15
103 205 1231.91 1231.33 1231.91 1229.45 1230.13 1229.45
206 1237.20 1236.65 1237.20 1234.74 1235.42 1234.74
104 207 1242.53 1241.94 1242.53 1240.04 1240.74 1240.04
208 1247.83 1247.26 1247.83 1245.34 1246.03 1245.34
105 209 1253.13 1252.55 1253.13 1250.66 1251.32 1250.66
210 1258.45 1257.87 1258.45 1255.96 1256.64 1255.96
106 211 1263.75 1263.16 1263.75 1261.26 1261.93 1261.26
212 1269.08 1268.48 1269.08 1266.55 1267.25 1266.55
107 213 1274.37 1273.77 1274.37 1271.85 1272.54 1271.85
214 1279.67 1279.09 1279.67 1277.15 1277.83 1277.15
108 215 1285.00 1284.38 1285.00 1282.45 1283.15 1282.45
216 1290.29 1289.70 1290.29 1287.74 1288.44 1287.74
109 217 1295.62 1295.02 1295.62 1293.04 1293.76 1293.04
218 1300.92 1300.32 1300.92 1298.34 1299.05 1298.34
110 219 1306.21 1305.64 1306.21 1303.63 1304.34 1303.63
220 1311.54 1310.93 1311.54 1308.93 1309.67 1308.93
111 221 1316.84 1316.25 1316.84 1314.23 1314.96 1314.23
222 1322.17 1321.54 1322.17 1319.52 1320.25 1319.52
112 223 1327.46 1326.86 1327.46 1324.82 1325.57 1324.82
224 1332.76 1332.15 1332.76 1330.12 1330.86 1330.12
113 225 1338.09 1337.47 1338.09 1335.41 1336.18 1335.41
226 1343.38 1342.79 1343.38 1340.71 1341.47 1340.71
114 227 1348.71 1348.08 1348.71 1346.01 1346.76 1346.01
228 1354.01 1353.40 1354.01 1351.31 1352.08 1351.31
115 229 1359.30 1358.69 1359.30 1356.63 1357.37 1356.63
230 1364.63 1364.01 1364.63 1361.93 1362.69 1361.93
116 231 1369.93 1369.30 1369.93 1367.23 1367.98 1367.23
232 1375.25 1374.62 1375.25 1372.52 1373.27 1372.52
117 233 1380.55 1379.91 1380.55 1377.82 1378.59 1377.82
234 1385.88 1385.23 1385.88 1383.12 1383.88 1383.12
118 235 1391.18 1390.55 1391.18 1388.41 1389.17 1388.41
236 1396.47 1395.84 1396.47 1393.71 1394.49 1393.71
119 237 1401.80 1401.16 1401.80 1399.01 1399.78 1399.01
238 1407.10 1406.45 1407.10 1404.31 1405.10 1404.31
120 239 1412.42 1411.77 1412.42 1409.60 1410.39 1409.60
240 1417.72 1417.06 1417.72 1414.90 1415.68 1414.90
121 241 1423.05 1422.39 1423.05 1420.20 1421.00 1420.20
242 1428.34 1427.68 1428.34 1425.49 1426.30 1425.49
122 243 1433.64 1433.00 1433.64 1430.79 1431.62 1430.79
244 1438.97 1438.32 1438.97 1436.09 1436.91 1436.09
123 245 1444.27 1443.61 1444.27 1441.38 1442.20 1441.38
246 1449.59 1448.93 1449.59 1446.68 1447.52 1446.68
124 247 1454.89 1454.22 1454.89 1451.98 1452.81 1451.98
248 1460.22 1459.54 1460.22 1457.27 1458.13 1457.27
125 249 1465.51 1464.83 1465.51 1462.57 1463.42 1462.57
250 1470.81 1470.15 1470.81 1467.87 1468.71 1467.87
126 251 1476.14 1475.44 1476.14 1473.17 1474.03 1473.17
252 1481.43 1480.76 1481.43 1478.49 1479.32 1478.49
127 253 1486.76 1486.05 1486.76 1483.79 1484.61 1483.79
254 1492.06 1491.37 1492.06 1489.09 1489.93 1489.09
128 255 1497.38 1496.69 1497.38 1494.38 1495.22 1494.38
256 1502.68 1501.98 1502.68 1499.68 1500.54 1499.68
129 257 1508.01 1507.30 1508.01 1504.98 1505.83 1504.98
258 1513.31 1512.59 1513.31 1510.27 1511.12 1510.27
130 259 1518.63 1517.91 1518.63 1515.57 1516.44 1515.57
260 1523.93 1523.20 1523.93 1520.87 1521.73 1520.87
131 261 1529.26 1528.52 1529.26 1526.16 1527.05 1526.16
262 1534.55 1533.81 1534.55 1531.46 1532.34 1531.46
132 263 1539.88 1539.14 1539.88 1536.76 1537.63 1536.76
264 1545.18 1544.43 1545.18 1542.06 1542.96 1542.06
133 265 1550.50 1549.75 1550.50 1547.35 1548.25 1547.35
266 1555.80 1555.07 1555.80 1552.65 1553.57 1552.65
134 267 1561.13 1560.36 1561.13 1557.95 1558.86 1557.95
268 1566.43 1565.68 1566.43 1563.24 1564.15 1563.24
135 269 1571.75 1570.97 1571.75 1568.54 1569.47 1568.54
270 1577.05 1576.29 1577.05 1573.84 1574.76 1573.84
136 271 1582.38 1581.58 1582.38 1579.13 1580.08 1579.13
272 1587.67 1586.90 1587.67 1584.43 1585.37 1584.43
137 273 1593.00 1592.19 1593.00 1589.73 1590.66 1589.73
274 1598.30 1597.51 1598.30 1595.03 1595.98 1595.03
138 275 1603.62 1602.80 1603.62 1600.32 1601.27 1600.32
276 1608.92 1608.12 1608.92 1605.62 1606.59 1605.62
139 277 1614.25 1613.41 1614.25 1610.92 1611.88 1610.92
278 1619.54 1618.73 1619.54 1616.21 1617.17 1616.21
140 279 1624.87 1624.05 1624.87 1621.51 1622.49 1621.51
280 1630.17 1629.34 1630.17 1626.81 1627.78 1626.81
141 281 1635.50 1634.66 1635.50 1632.10 1633.07 1632.10
282 1640.82 1639.95 1640.82 1637.40 1638.39 1637.40
142 283 1646.12 1645.27 1646.12 1642.70 1643.68 1642.70
284 1651.45 1650.56 1651.45 1647.99 1649.00 1647.99
143 285 1656.74 1655.89 1656.74 1653.29 1654.29 1653.29
286 1662.07 1661.18 1662.07 1658.59 1659.58 1658.59
144 287 1667.40 1666.50 1667.40 1663.89 1664.91 1663.89
288 1672.69 1671.79 1672.69 1669.15 1670.20 1669.15
145 289 1678.02 1677.11 1678.02 1674.45 1675.52 1674.45
290 1683.32 1682.40 1683.32 1679.75 1680.81 1679.75
146 291 1688.64 1687.72 1688.64 1685.04 1686.10 1685.04
292 1693.97 1693.04 1693.97 1690.34 1691.42 1690.34
147 293 1699.27 1698.33 1699.27 1695.64 1696.71 1695.64
294 1704.60 1703.65 1704.60 1700.93 1702.03 1700.93
148 295 1709.92 1708.94 1709.92 1706.23 1707.32 1706.23
296 1715.22 1714.26 1715.22 1711.53 1712.61 1711.53
Table A2. Spectrometer Line Shape. Full-width Half-maximum. Double Scan.
Det. 1 Det. 2 Det. 3 Det. 4 Det. 5 Det. 6
1 6.33 6.24 6.33 6.30 6.24 6.30
2 6.33 6.24 6.33 6.30 6.21 6.30
3 6.33 6.24 6.33 6.33 6.24 6.33
4 6.33 6.27 6.33 6.33 6.24 6.33
5 6.36 6.24 6.36 6.33 6.21 6.33
6 6.33 6.27 6.33 6.33 6.24 6.33
7 6.36 6.27 6.36 6.33 6.24 6.33
8 6.36 6.27 6.36 6.33 6.24 6.33
9 6.36 6.27 6.36 6.33 6.24 6.33
10 6.39 6.27 6.39 6.33 6.27 6.33
11 6.36 6.27 6.36 6.33 6.24 6.33
12 6.39 6.27 6.39 6.36 6.27 6.36
13 6.36 6.27 6.36 6.36 6.27 6.36
14 6.39 6.27 6.39 6.36 6.27 6.36
15 6.36 6.30 6.36 6.36 6.27 6.36
16 6.39 6.27 6.39 6.36 6.27 6.36
17 6.39 6.30 6.39 6.39 6.27 6.39
18 6.39 6.30 6.39 6.39 6.27 6.39
19 6.39 6.30 6.39 6.39 6.27 6.39
20 6.39 6.30 6.39 6.39 6.27 6.39
21 6.39 6.30 6.39 6.36 6.30 6.36
22 6.39 6.30 6.39 6.36 6.27 6.36
23 6.39 6.33 6.39 6.39 6.30 6.39
24 6.42 6.30 6.42 6.39 6.30 6.39
25 6.42 6.33 6.42 6.39 6.27 6.39
26 6.42 6.33 6.42 6.39 6.30 6.39
27 6.42 6.33 6.42 6.39 6.30 6.39
28 6.42 6.33 6.42 6.39 6.30 6.39
29 6.45 6.33 6.45 6.39 6.30 6.39
30 6.42 6.33 6.42 6.42 6.30 6.42
31 6.45 6.33 6.45 6.42 6.30 6.42
32 6.45 6.33 6.45 6.42 6.30 6.42
33 6.45 6.33 6.45 6.42 6.30 6.42
34 6.45 6.36 6.45 6.42 6.30 6.42
35 6.48 6.33 6.48 6.42 6.33 6.42
36 6.45 6.36 6.45 6.42 6.30 6.42
37 6.48 6.33 6.48 6.45 6.33 6.45
38 6.48 6.36 6.48 6.45 6.33 6.45
39 6.48 6.36 6.48 6.45 6.30 6.45
40 6.48 6.36 6.48 6.45 6.33 6.45
41 6.51 6.36 6.51 6.42 6.30 6.42
42 6.48 6.36 6.48 6.42 6.33 6.42
43 6.51 6.36 6.51 6.42 6.33 6.42
44 6.51 6.36 6.51 6.42 6.33 6.42
45 6.51 6.36 6.51 6.45 6.33 6.45
46 6.51 6.36 6.51 6.45 6.33 6.45
47 6.54 6.39 6.54 6.45 6.33 6.45
48 6.51 6.36 6.51 6.45 6.33 6.45
49 6.54 6.39 6.54 6.45 6.33 6.45
50 6.57 6.36 6.57 6.45 6.33 6.45
51 6.54 6.39 6.54 6.45 6.33 6.45
52 6.57 6.39 6.57 6.48 6.33 6.48
53 6.57 6.39 6.57 6.48 6.33 6.48
54 6.60 6.39 6.60 6.48 6.36 6.48
55 6.57 6.39 6.57 6.48 6.33 6.48
56 6.60 6.39 6.60 6.51 6.36 6.51
57 6.63 6.42 6.63 6.51 6.33 6.51
58 6.60 6.39 6.60 6.51 6.33 6.51
59 6.63 6.39 6.63 6.54 6.36 6.54
60 6.63 6.42 6.63 6.54 6.33 6.54
61 6.66 6.39 6.66 6.54 6.36 6.54
62 6.66 6.42 6.66 6.54 6.36 6.54
63 6.66 6.39 6.66 6.54 6.33 6.54
64 6.69 6.42 6.69 6.54 6.36 6.54
65 6.66 6.42 6.66 6.57 6.33 6.57
66 6.69 6.42 6.69 6.57 6.36 6.57
67 6.72 6.42 6.72 6.57 6.36 6.57
68 6.72 6.42 6.72 6.57 6.36 6.57
69 6.72 6.42 6.72 6.57 6.36 6.57
70 6.72 6.45 6.72 6.60 6.33 6.60
71 6.75 6.42 6.75 6.60 6.36 6.60
72 6.75 6.45 6.75 6.60 6.36 6.60
73 6.75 6.42 6.75 6.60 6.36 6.60
74 6.78 6.42 6.78 6.60 6.36 6.60
75 6.81 6.45 6.81 6.63 6.36 6.63
76 6.78 6.42 6.78 6.63 6.36 6.63
77 6.81 6.45 6.81 6.63 6.36 6.63
78 6.84 6.45 6.84 6.63 6.36 6.63
79 6.84 6.45 6.84 6.63 6.36 6.63
80 6.84 6.45 6.84 6.66 6.39 6.66
81 6.84 6.45 6.84 6.66 6.36 6.66
82 6.87 6.45 6.87 6.69 6.36 6.69
83 6.90 6.48 6.90 6.69 6.39 6.69
84 6.87 6.45 6.87 6.69 6.36 6.69
85 6.90 6.48 6.90 6.72 6.39 6.72
86 6.93 6.48 6.93 6.72 6.36 6.72
87 6.90 6.48 6.90 6.72 6.36 6.72
88 6.93 6.48 6.93 6.72 6.39 6.72
89 6.96 6.45 6.96 6.75 6.36 6.75
90 6.96 6.48 6.96 6.75 6.39 6.75
91 6.96 6.48 6.96 6.75 6.39 6.75
92 6.99 6.48 6.99 6.75 6.39 6.75
93 6.99 6.48 6.99 6.78 6.39 6.78
94 7.02 6.48 7.02 6.78 6.36 6.78
95 6.99 6.48 6.99 6.78 6.39 6.78
96 7.02 6.51 7.02 6.78 6.39 6.78
97 7.05 6.48 7.05 6.78 6.39 6.78
98 7.05 6.51 7.05 6.81 6.39 6.81
99 7.08 6.51 7.08 6.81 6.39 6.81
100 7.08 6.51 7.08 6.84 6.39 6.84
101 7.08 6.51 7.08 6.84 6.39 6.84
102 7.11 6.51 7.11 6.87 6.39 6.87
103 7.14 6.51 7.14 6.87 6.39 6.87
104 7.11 6.54 7.11 6.87 6.39 6.87
105 7.14 6.51 7.14 6.87 6.39 6.87
106 7.17 6.54 7.17 6.90 6.39 6.90
107 7.17 6.54 7.17 6.90 6.42 6.90
108 7.20 6.54 7.20 6.90 6.39 6.90
109 7.20 6.54 7.20 6.93 6.42 6.93
110 7.20 6.54 7.20 6.93 6.39 6.93
111 7.23 6.54 7.23 6.93 6.39 6.93
112 7.26 6.54 7.26 6.93 6.42 6.93
113 7.26 6.54 7.26 6.96 6.39 6.96
114 7.29 6.54 7.29 6.99 6.42 6.99
115 7.29 6.54 7.29 6.99 6.42 6.99
116 7.32 6.54 7.32 6.99 6.39 6.99
117 7.32 6.57 7.32 7.02 6.42 7.02
118 7.35 6.54 7.35 7.02 6.39 7.02
119 7.38 6.57 7.38 7.02 6.42 7.02
120 7.38 6.57 7.38 7.02 6.42 7.02
121 7.38 6.57 7.38 7.05 6.42 7.05
122 7.41 6.57 7.41 7.05 6.42 7.05
123 7.41 6.57 7.41 7.05 6.42 7.05
124 7.44 6.57 7.44 7.08 6.42 7.08
125 7.47 6.60 7.47 7.11 6.42 7.11
126 7.50 6.57 7.50 7.11 6.42 7.11
127 7.50 6.60 7.50 7.11 6.42 7.11
128 7.53 6.60 7.53 7.14 6.42 7.14
129 7.53 6.60 7.53 7.14 6.42 7.14
130 7.56 6.60 7.56 7.14 6.42 7.14
131 7.56 6.63 7.56 7.14 6.45 7.14
132 7.59 6.60 7.59 7.17 6.42 7.17
133 7.62 6.63 7.62 7.20 6.45 7.20
134 7.65 6.60 7.65 7.20 6.42 7.20
135 7.65 6.63 7.65 7.23 6.42 7.23
136 7.68 6.63 7.68 7.23 6.45 7.23
137 7.71 6.63 7.71 7.23 6.42 7.23
138 7.74 6.63 7.74 7.23 6.45 7.23
139 7.74 6.66 7.74 7.26 6.45 7.26
140 7.77 6.63 7.77 7.29 6.42 7.29
141 7.77 6.66 7.77 7.29 6.45 7.29
142 7.80 6.63 7.80 7.32 6.42 7.32
143 7.83 6.66 7.83 7.32 6.45 7.32
144 7.83 6.66 7.83 7.32 6.45 7.32
145 7.86 6.66 7.86 7.35 6.45 7.35
146 7.89 6.66 7.89 7.38 6.45 7.38
147 7.92 6.69 7.92 7.38 6.45 7.38
148 7.95 6.66 7.95 7.41 6.45 7.41
149 7.98 6.69 7.98 7.41 6.45 7.41
150 7.98 6.69 7.98 7.41 6.45 7.41
151 8.01 6.69 8.01 7.44 6.45 7.44
152 8.04 6.69 8.04 7.47 6.45 7.47
153 8.07 6.69 8.07 7.47 6.45 7.47
154 8.10 6.69 8.10 7.50 6.45 7.50
155 8.13 6.72 8.13 7.50 6.48 7.50
156 8.13 6.69 8.13 7.50 6.45 7.50
157 8.16 6.72 8.16 7.56 6.48 7.56
158 8.19 6.72 8.19 7.56 6.45 7.56
159 8.22 6.72 8.22 7.56 6.45 7.56
160 8.25 6.72 8.25 7.59 6.48 7.59
161 8.28 6.75 8.28 7.62 6.45 7.62
162 8.31 6.72 8.31 7.65 6.48 7.65
163 8.31 6.75 8.31 7.65 6.48 7.65
164 8.34 6.72 8.34 7.65 6.48 7.65
165 8.37 6.75 8.37 7.68 6.48 7.68
166 8.40 6.75 8.40 7.71 6.48 7.71
167 8.43 6.75 8.43 7.74 6.48 7.74
168 8.46 6.75 8.46 7.74 6.48 7.74
169 8.49 6.78 8.49 7.74 6.48 7.74
170 8.52 6.78 8.52 7.80 6.48 7.80
171 8.55 6.78 8.55 7.80 6.48 7.80
172 8.55 6.81 8.55 7.83 6.48 7.83
173 8.58 6.78 8.58 7.86 6.48 7.86
174 8.61 6.81 8.61 7.86 6.51 7.86
175 8.67 6.81 8.67 7.89 6.48 7.89
176 8.70 6.81 8.70 7.89 6.51 7.89
177 8.73 6.81 8.73 7.95 6.48 7.95
178 8.76 6.81 8.76 7.95 6.48 7.95
179 8.79 6.81 8.79 7.98 6.51 7.98
180 8.82 6.84 8.82 8.01 6.48 8.01
181 8.85 6.81 8.85 8.01 6.51 8.01
182 8.88 6.84 8.88 8.04 6.51 8.04
183 8.91 6.84 8.91 8.04 6.48 8.04
184 8.94 6.84 8.94 8.10 6.51 8.10
185 9.00 6.84 9.00 8.10 6.51 8.10
186 9.03 6.87 9.03 8.13 6.51 8.13
187 9.06 6.84 9.06 8.16 6.51 8.16
188 9.09 6.87 9.09 8.19 6.51 8.19
189 9.12 6.90 9.12 8.19 6.51 8.19
190 9.15 6.87 9.15 8.25 6.51 8.25
191 9.18 6.90 9.18 8.25 6.51 8.25
192 9.21 6.90 9.21 8.28 6.51 8.28
193 9.27 6.90 9.27 8.31 6.54 8.31
194 9.30 6.90 9.30 8.34 6.51 8.34
195 9.33 6.93 9.33 8.34 6.54 8.34
196 9.36 6.90 9.36 8.40 6.54 8.40
197 9.39 6.93 9.39 8.40 6.51 8.40
198 9.42 6.93 9.42 8.46 6.54 8.46
199 9.48 6.93 9.48 8.46 6.51 8.46
200 9.51 6.93 9.51 8.49 6.54 8.49
201 9.54 6.96 9.54 8.52 6.54 8.52
202 9.57 6.96 9.57 8.55 6.51 8.55
203 9.60 6.96 9.60 8.61 6.54 8.61
204 9.66 6.99 9.66 8.61 6.54 8.61
205 9.69 6.96 9.69 8.64 6.54 8.64
206 9.72 6.99 9.72 8.67 6.54 8.67
207 9.75 6.99 9.75 8.70 6.57 8.70
208 9.78 6.99 9.78 8.73 6.54 8.73
209 9.84 6.99 9.84 8.76 6.54 8.76
210 9.87 7.02 9.87 8.82 6.54 8.82
211 9.93 6.99 9.93 8.82 6.54 8.82
212 9.96 7.02 9.96 8.85 6.57 8.85
213 10.00 7.05 10.00 8.88 6.54 8.88
214 10.06 7.02 10.06 8.91 6.57 8.91
215 10.09 7.05 10.09 8.97 6.57 8.97
216 10.12 7.05 10.12 8.97 6.54 8.97
217 10.15 7.05 10.15 9.03 6.57 9.03
218 10.21 7.05 10.21 9.06 6.57 9.06
219 10.24 7.08 10.24 9.09 6.57 9.09
220 10.30 7.08 10.30 9.12 6.57 9.12
221 10.33 7.08 10.33 9.18 6.57 9.18
222 10.39 7.11 10.39 9.18 6.57 9.18
223 10.42 7.08 10.42 9.24 6.57 9.24
224 10.45 7.11 10.45 9.27 6.57 9.27
225 10.48 7.11 10.48 9.30 6.57 9.30
226 10.54 7.11 10.54 9.33 6.60 9.33
227 10.60 7.11 10.60 9.39 6.57 9.39
228 10.63 7.14 10.63 9.42 6.60 9.42
229 10.69 7.14 10.69 9.45 6.60 9.45
230 10.72 7.14 10.72 9.51 6.57 9.51
231 10.75 7.17 10.75 9.54 6.60 9.54
232 10.78 7.14 10.78 9.57 6.60 9.57
233 10.84 7.17 10.84 9.60 6.60 9.60
234 10.90 7.20 10.90 9.66 6.60 9.66
235 10.93 7.20 10.93 9.72 6.57 9.72
236 10.96 7.20 10.96 9.72 6.60 9.72
237 11.02 7.20 11.02 9.78 6.60 9.78
238 11.05 7.23 11.05 9.84 6.60 9.84
239 11.11 7.20 11.11 9.87 6.60 9.87
240 11.17 7.23 11.17 9.93 6.63 9.93
241 11.20 7.26 11.20 9.93 6.60 9.93
242 11.23 7.23 11.23 10.00 6.60 10.00
243 11.29 7.26 11.29 10.06 6.63 10.06
244 11.32 7.26 11.32 10.09 6.60 10.09
245 11.38 7.26 11.38 10.15 6.63 10.15
246 11.41 7.29 11.41 10.18 6.63 10.18
247 11.47 7.29 11.47 10.21 6.63 10.21
248 11.50 7.32 11.50 10.27 6.63 10.27
249 11.53 7.29 11.53 10.33 6.60 10.33
250 11.62 7.32 11.62 10.39 6.63 10.39
251 11.65 7.35 11.65 10.42 6.63 10.42
252 11.68 7.32 11.68 10.48 6.63 10.48
253 11.74 7.35 11.74 10.54 6.63 10.54
254 11.77 7.35 11.77 10.54 6.66 10.54
255 11.80 7.38 11.80 10.60 6.63 10.60
256 11.89 7.38 11.89 10.66 6.63 10.66
257 11.92 7.38 11.92 10.72 6.66 10.72
258 11.95 7.41 11.95 10.75 6.63 10.75
259 12.01 7.38 12.01 10.81 6.66 10.81
260 12.04 7.41 12.04 10.87 6.66 10.87
261 12.10 7.44 12.10 10.93 6.66 10.93
262 12.13 7.41 12.13 10.99 6.66 10.99
263 12.19 7.44 12.19 11.02 6.66 11.02
264 12.22 7.44 12.22 11.08 6.66 11.08
265 12.25 7.47 12.25 11.14 6.66 11.14
266 12.31 7.47 12.31 11.20 6.69 11.20
267 12.37 7.47 12.37 11.23 6.66 11.23
268 12.40 7.50 12.40 11.29 6.69 11.29
269 12.46 7.53 12.46 11.35 6.66 11.35
270 12.49 7.50 12.49 11.41 6.66 11.41
271 12.52 7.53 12.52 11.47 6.69 11.47
272 12.58 7.53 12.58 11.53 6.66 11.53
273 12.64 7.53 12.64 11.56 6.69 11.56
274 12.67 7.56 12.67 11.62 6.69 11.62
275 12.73 7.56 12.73 11.68 6.69 11.68
276 12.76 7.59 12.76 11.74 6.69 11.74
277 12.79 7.59 12.79 11.80 6.69 11.80
278 12.85 7.59 12.85 11.86 6.69 11.86
279 12.88 7.62 12.88 11.89 6.69 11.89
280 12.94 7.62 12.94 11.95 6.72 11.95
281 13.00 7.62 13.00 12.01 6.69 12.01
282 13.03 7.65 13.03 12.07 6.72 12.07
283 13.06 7.65 13.06 12.13 6.72 12.13
284 13.12 7.68 13.12 12.19 6.72 12.19
285 13.15 7.68 13.15 12.25 6.72 12.25
286 13.18 7.68 13.18 12.28 6.72 12.28
287 13.27 7.71 13.27 12.37 6.72 12.37
288 13.30 7.74 13.30 12.43 6.72 12.43
289 13.33 7.71 13.33 12.49 6.75 12.49
290 13.39 7.74 13.39 12.55 6.72 12.55
291 13.42 7.77 13.42 12.61 6.75 12.61
292 13.45 7.77 13.45 12.67 6.72 12.67
293 13.51 7.77 13.51 12.70 6.72 12.70
294 13.54 7.80 13.54 12.76 6.75 12.76
295 13.57 7.80 13.57 12.82 6.72 12.82
296 13.63 7.83 13.63 12.88 6.75 12.88