PDS_VERSION_ID               = PDS3
RECORD_TYPE                  = STREAM
DATA_SET_ID                  =  "MEX-M-MRS-1/2/3-EXT1-0770-V1.0"
STANDARD_DATA_PRODUCT_ID     = ENB
PRODUCER_ID                  = "SUE"
PRODUCT_ID                   = "M00SUE0L1A_ENB_060220407_00.TXT"
PRODUCT_CREATION_TIME        =  2009-05-07T14:18:43.000
INSTRUMENT_HOST_ID           = "MEX"
OBJECT                       = TEXT
  PUBLICATION_DATE             = 2007-11-29
  NOTE                         = "MEX SUE Experimenter Notes"
END_OBJECT                   = TEXT
END

From tzegers@rssd.esa.int Fri Dec 23 02:16:28 2005
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Date: Fri, 23 Dec 2005 11:18:07 +0100
From: Tanja Zegers <tzegers@rssd.esa.int>
Subject: specular pointing test 2606
To: Dick Simpson <rsimpson@magellan.stanford.edu>,
        Martin Patzold <paetzold@geo.uni-koeln.de>,
        "Joerg.Selle@Unibw-Muenchen.De" <joerg.selle@unibw-muenchen.de>,
        Hannes Griebel <Hannes.Griebel@unibw-muenchen.de>,
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Dear Dick and Martin,
The BSR in orbit 2606 on January 22nd will be done as a specular
pointing test. The same time window as the inertial pointing that is
currently in the ptr will be used. I will get back to you in January
with the details of the algorithm that flight dynamics will use for this
test.
I wish you all happy hollidays and new year !
Best regards,
Tanja

--
Dr. T.E. Zegers
Research and Scientific Support Department, European Space Agency, ESTEC
tel: +31-71-5656585 mobile: +31-6-30395627


From rsimpson Sun Jan 22 16:48:13 2006
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Date: Sun, 22 Jan 2006 16:47:50 -0800 (PST)
From: Dick Simpson 650-723-3525 <rsimpson>
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To: Daniel.S.Kahan@jpl.nasa.gov, H.J.Walker@rl.ac.uk,
        JValencia@jftl.jpl.nasa.gov, JVelasco@jftl.jpl.nasa.gov,
        John.Reynolds@esa.int, Michel.Denis@esa.int, Olivier.Reboud@esa.int,
        Ricardo.G.Torres@jpl.nasa.gov, Sophia.M.No@jpl.nasa.gov,
        art.freiley@jpl.nasa.gov, audenrie@geo.uni-koeln.de,
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        dhinson@stanford.edu, dwight.holmes@jpl.nasa.gov, fred.jansen@esa.int,
        gene.goltz@jpl.nasa.gov, joerg.selle@unibw-muenchen.de,
        john.c.klose@jpl.nasa.gov, jtwicken@stanford.edu,
        len.tyler@stanford.edu, mexmps@esa.int, mueller@geo.uni-koeln.de,
        paetzold@geo.uni-koeln.de, rene.pischel@rssd.esa.int, rsimpson,
        sami.asmar@jpl.nasa.gov, stanzel@geo.uni-koeln.de,
        stupar@geo.uni-koeln.de, thomas.w.thompson@jpl.nasa.gov,
        tzegers@rssd.esa.int, walter@geo.uni-koeln.de
Subject: MEX BSR DOY 021 and 022
Content-Length: 2473
Status: RO

MEX BSR planning and support colleagues:

Two experiments have been conducted successfully within the
past 48 hours, including the first with specular point
tracking.

The target on 2006/021 was Hellas Planitia, and the
observations were conducted very soon after pericenter
meaning that Doppler shifts and Doppler spreading were very
large.  In fact, we monitored the carrier using the 250
ksps option on the receiving system, the first time we have
gone above 100 ksps.  Echoes were only visible on S- and X-
Band LCP in real time; the RCP signals were expected to be
weak because the incidence angle at the specular point was
only 32 deg.  It is likely that we will need the 100 ksps
data for science analysis because of the extreme Dopplers;
we collected about 30 minutes of noise data during the
ground pre-cal to facilitate this work.

Between the pre-cal and the beginning of tracking, we lost
the S-RCP signal for about 15 minutes.  We lost it again
twice later, for about 10 minutes each time.  Fortunately,
the outages were during (mostly) periods of little
activity; but we did lose about 10 minutes from the post-
cal.  Personnel from the station and from JPL investigated,
but were unable to diagnose the problem except to localize
it to the S-RCP maser.  By the time we were ready to begin
the experiment on 2006/022, the maser had been declared
"red," limiting us to three downlink channels.  I think the
data from  2006/021, despite the interruptions, are
probably OK.  For what it's worth, S-RCP was expected to
have the weakest echoes of the four channels; if we were
going to lose one, that was probably a good choice.

On 2006/022 the target was Mars northern plains (Utopia
Planitia).  Echoes were visible in all three channels, with
the two X-band echoes being roughly equal in strength.
Since the HGA tracked the specular point, we were able to
observe the reflections for a full hour.  There was a minor
problem with the X-LCP mini-calibration, which means we
will have to compensate for the fact that noise diode
energy is superimposed on the X-LCP echo for a few minutes
at the beginning.

With the exception of the maser problem on S-RCP, I
consider these two experiments to be very successful and
look forward to having the opportunity to collect more
specular track data in the future.  When we have something
to look at, I'll plan to share a figure showing an hour's
worth of Mars echoes.

Regards,
Dick


From gene.goltz@jpl.nasa.gov Mon Jan 23 06:55:31 2006
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To: Dick Simpson 650-723-3525 <rsimpson@magellan.stanford.edu>
From: Gene Goltz <gene.goltz@jpl.nasa.gov>
Subject: 2006-022 MEX Occultation Data
Cc: sami Asmar <sami.asmar@jpl.nasa.gov>,
        Martin =?iso-8859-1?Q?P=E4tzold?=
  <paetzold@geo.Uni-Koeln.DE>,
        mueller@geo.Uni-Koeln.DE, walter@geo.Uni-Koeln.DE,
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Status: RO


Dick,

The MEX Occultation on DOY 022 (pass 0967) was conducted at DSS-63.  RSR
open-loop data were recorded and played back as follows:

     -  X-band, 2-way
     -  RSR2B1
     -  2 kHz, 16 bits
     -  start = 21:53:04
     -  LOS = 22:07:23 (predicted)
     -  stop = 22:13:00
     -  SFDUs = 1,197

   and:

     -  S-band, 2-way
     -  RSR2A1
     -  2 kHz, 16 bits
     -  start = 21:53:04
     -  LOS = 22:07:23 (predicted)
     -  stop = 22:13:00
     -  SFDUs = 1,197


These data should now be available on the RS TDS for you to query.

NOTES:  1) these recordings were done "in the blind" using scripts



From rmdc@zeus.jpl.nasa.gov Mon Jan 23 14:22:07 2006
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Subject: 41 RMDC Delivery
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Tracking data for spacecraft 41 (MEX)

Comments:
RMDCT delivery to MEX-RS
1-sec Doppler compression time

F2 : good
SQR : good

Created by ljc at Mon Jan 23 22:21:54 GMT 2006

OSCARX:/ftp/ras/sc41/odfs/06022O022_63X_1S.SC041

*******************************************************************************

                                               DATA CMPT CH   DATA
 SCN  UL   DL       FROM             TO        TYPE FCOM LC  POINTS COMMENTS
 === ==== ==== =============== =============== ==== ==== == ======= ===========
  41 63X  63X  06-022T19:17:04 06-022T22:07:20 F2      1  5   10217
  41 63X  63X  06-022T19:19:57 06-022T22:02:06 SQR     4 20      48


From rmdc@zeus.jpl.nasa.gov Mon Jan 23 14:24:10 2006
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Subject: 41 RMDC Delivery
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Tracking data for spacecraft 41 (MEX)

Comments:
RMDCT delivery to MEX-RS
1-sec Doppler compression time

F2 : good

Created by ljc at Mon Jan 23 22:23:47 GMT 2006

OSCARX:/ftp/ras/sc41/odfs/06022O022_63S_1S.SC041

*******************************************************************************

                                               DATA CMPT CH   DATA
 SCN  UL   DL       FROM             TO        TYPE FCOM LC  POINTS COMMENTS
 === ==== ==== =============== =============== ==== ==== == ======= ===========
  41 63X  63S  06-022T21:32:37 06-022T22:07:19 F2      1  7    2083


From sami.asmar@jpl.nasa.gov Mon Jan 23 14:19:26 2006
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Date: Mon, 23 Jan 2006 14:15:44 -0800
To: rsimpson@magellan.stanford.edu
From: Sami Asmar <sami.asmar@jpl.nasa.gov>
Subject: Fwd: dss14 s-band maser
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--=====================_92796354==.ALT
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>Date: Mon, 23 Jan 2006 14:05:50 -0800
>From: "Klose, John" <JKlose@jftl.jpl.nasa.gov>
>Subject: dss14 s-band maser
>To: Cassini Radio Science Ops <rsops@rodan.jpl.nasa.gov>
>Cc: "Hampton, Sherill" <SHampton@jftl.jpl.nasa.gov>,
>  "Klose, John" <JKlose@jftl.jpl.nasa.gov>
>X-Mailer: Internet Mail Service (5.5.2657.72)
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>Original-recipient: rfc822;asmar@mail.jpl.nasa.gov
>
>Howdy All;
>I received a call from Gene Goltz over the weekend
>About some problems with the MEX Bi-Static Experiment
>On DOY 021. The root cause of the problem was the S-Band
>MASER at DSS-14. The MASER has been calibrated,
>And the latest status from GDSCC is "Green".
>
>
>
>  Regards,
>
>-John C. Klose V
>
>DSN O&M Program, Network Engineering
>Software Operations Engineer:
>Radio Science, SPT, BVE, and 34M/70M UPL
>Tel: (626) 305-6127
>Pgr: (626) 491-0044
><mailto:jklose@jftl.jpl.nasa.gov>jklose@jftl.jpl.nasa.gov
><mailto:john.c.klose@jpl.nasa.gov>john.c.klose@jpl.nasa.gov
>




From sami.asmar@jpl.nasa.gov Tue Jan 24 20:35:04 2006
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To: Dick Simpson 650-723-3525 <rsimpson@magellan.stanford.edu>
From: Sami Asmar <sami.asmar@jpl.nasa.gov>
Subject: Re: S-RCP Maser
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Sorry Dick... let me understand, SCLP was the one the went off
line and they went to a HEMPT (right?)... so you're saying the
SRCP maser was also bad but the station did not have an indication?



At 03:44 PM 1/24/2006, you wrote:

>After sniping at a maser that could turn itself on and off, depending
>on how it felt it was doing, I've now actually had a chance to look
>at some of the data.  And it wasn't doing very well. Compared to the
>other channels where 1 sec averages of noise had an rms on the order
>of 0.02 dB, SRCP was wandering over a range approaching +/-0.5 dB.
>So maybe smart masers do exist and this one did the right thing in
>spite of my doubts.  Whether "calibration" is the right cure, is
>another question.



From rsimpson Wed Jan 25 10:23:47 2006
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Date: Wed, 25 Jan 2006 10:23:47 -0800 (PST)
From: Dick Simpson 650-723-3525 <rsimpson>
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>Sorry Dick... let me understand, SCLP was the one the went off
>line and they went to a HEMPT (right?)... so you're saying the
>SRCP maser was also bad but the station did not have an indication?

  No, there was never any problem with S-LCP, which has always
  been on the HEMT (I think).  The S-RCP maser had problems
  and eventually died; but, since the HEMT is being used for
  LCP, there is no backup and we ran with only three channels.

  John Klose (and the station) both suggested swapping in the
  HEMT; but I don't think they realized we couldn't give up
  LCP in order to receive RCP.  Eventually we got it straight
  with the station.

  If you think there is a third LNA for S-band, then we should look
  into that.  The chart I got from Art Freiley last year shows only
  a BLK-4 and the HEMT available for S.  We need two channels, so
  there's no backup when one of the two known LNA's is red.



From Daniel.S.Kahan-121461@jpl.nasa.gov Wed Jan 25 10:28:23 2006
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Dick,

MEX Bi-Static Radar RSR open-loop data from DOY 022 at DSS-14 (pass 0966)
have been played back to the TDS as follows:

 -  X-band, RCP, 1-way
 -  RSR2B3
 -  25 kHz, 16 bits
 -  start = 04:07:01
 -  stop = 05:05:00
 -  start = 05:35:00
 -  stop = 08:45:00
 -  SFDUs = 59,524

and:

 -  S-band, RCP, 1-way
 -  RSR2A3
 -  25 kHz, 16 bits
 -  NOT Recorded

and:

 -  X-band, LCP, 1-way
 -  RSR3B3
 -  25 kHz, 16 bits
 -  start = 04:07:01
 -  stop = 05:05:00
 -  start = 05:35:00
 -  stop = 08:45:00
 -  SFDUs = 59,524

and:

 -  S-band, LCP, 1-way
 -  RSR3A3
 -  25 kHz, 16 bits
 -  start = 04:07:01
 -  stop = 05:05:00
 -  start = 05:35:00
 -  stop = 08:45:00
 -  SFDUs = 59,524

These data should now be available for you to query.

Regards,
Danny


From Daniel.S.Kahan-121461@jpl.nasa.gov Wed Jan 25 13:21:02 2006
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From: Daniel S Kahan <Daniel.S.Kahan-121461@jpl.nasa.gov>
To: Dick Simpson 650-723-3525 <rsimpson@magellan.stanford.edu>
Cc: Gene Goltz <gene.goltz@jpl.nasa.gov>
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Subject: MEX 2006/022 Bi-Static Radar Data (100 KHz)
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Dick,

MEX Bi-Static Radar RSR open-loop data from DOY 022 at DSS-14 (pass 0966) have been played back to the TDS as follows:

-  X-band, RCP, 1-way
-  RSR2B3
-  100 kHz, 16 bits
-  start = 06:20:59
-  stop = 07:17:00
-  SFDUs = 67,240

and:

-  S-band, RCP, 1-way
-  RSR2A3
-  100 kHz, 16 bits
-  NOT Recorded

and:

-  X-band, LCP, 1-way
-  RSR3B3
-  100 kHz, 16 bits
-  start = 06:21:00
-  stop = 07:17:00
-  SFDUs = 67,220

and:

-  S-band, LCP, 1-way
-  RSR3A3
-  100 kHz, 16 bits
-  start = 06:21:00
-  stop = 07:17:00
-  SFDUs = 67,220

These data should now be available for you to query.

Regards,
Danny

From rsimpson Thu Feb  9 22:02:38 2006
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Date: Thu, 9 Feb 2006 22:02:36 -0800 (PST)
From: Dick Simpson 650-723-3525 <rsimpson>
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To: paetzold@geo.Uni-Koeln.DE, bernd.haeusler@unibw-muenchen.de,
        len.tyler@stanford.edu, rsimpson
Subject: Specular Point Results
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Martin and others:

  Here are some results from the specular point track experiment that we
did about three weeks ago.

  The waterfall plot shows the X-RCP and X-LCP power spectra.  Each spectrum
is an average of 30 seconds of data; time increases from front to back
(bottom to top).  These are calibrated data; what you see are the number of
zeptowatts in each bin (24.414 Hz each).  The noise pedestal is included in
each plot; it is about 7.5 zw.  The curves are offset by 1 zw to create
the waterfall effect.

  If you look closely, you will see that the XL echo is about twice as large
as the XR echo at the beginning (front).  Both echoes get stronger during the
experiment, but the XR is about 30 percent larger than XL at the end; so we
have passed through the Brewster angle.

  Angle of incidence at the beginning is about 56.5 deg; at the end it is
about 64.8 deg.  The Brewster angle occurs at about 62.3 deg, making the
dielectric constant about 3.6.  This is on the high end of what we have
been seeing in previous experiments.

  The Word document is a tabulation of the results - one line for each pair
of spectra.  Incidence angle is in the third column (PHI), dielectric
constant is on the far right.  You will see that there is a slow drift toward
lower values of dielectric constant during the experiment; 3.6 is lower
than most.

  During the experiment the specular point latitude moved from 40N to 48N
and from 93E to 88E.  The HGA illuminated a spot 300 km across (or about
5 degrees of latitude).  So there aren't a lot of independent measurements
here.  My software doesn't estimate the width of the echo; but I have done
a few calculations by hand.  It appears the rms surface roughness is about
2.7 degrees at the beginning and about 3.3 degrees at the end; so the
surface itself helps to improve the spatial resolution slightly (down from
the 5 deg of the HGA spot).

  The numbers look pretty firm here.  The calibrations are almost identical
to what they were the day before, when we had an inertial pointing experiment
near pericenter over Hellas.  The two white stripes in the X-RCP plot are
from interfering MGS signals; I removed the contamination from the power
estimates for the later one (less than 5 percent change), but the first was
too weak and I decided not to try - even though it's clearly visible in
these plots.

  These are really nice data and a pleasure to work with after struggling
with the inertial pointing experiments.  They will probably be the center
of my LPSC poster, which needs to be done in a month.

  Because of the S-RCP maser failure, we don't have anything comparable at
S-Band.  But the S-LCP echo is clearly visible and (if I had the time to
attempt an absolute calibration of that channel), it might be possible to
get an estimate of the dielectric constant at S-Band.

  The LPSC abstract summarizes results from 12 Dec, when we got X-band
rms surface roughness 4.0 deg and dieletric constant 3.6, which I thought
was a bit high at the time.  The new experiment supports higher values.
The puzzling part about 12 Dec was that the S-Band dielectric constant was
2.4, when we would normally expect it to be larger than 3.6.

  We also have some very nice cross-spectra from the latest experiment,
giving me renewed confidence that we will be successful when VEX probes
Maxwell Montes in June.

Regards,
Dick

---
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7ENVeAQAHAQpAL39W9MkyXEkiD6f/BW5DxABRSbZYR53vJEgKKQcYIAFZoUzsrMyUqguNnrY
                               ...


From rsimpson Sat Feb 11 16:21:54 2006
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Date: Sat, 11 Feb 2006 16:21:49 -0800 (PST)
From: Dick Simpson 650-723-3525 <rsimpson>
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To: paetzold@geo.Uni-Koeln.DE, mueller@geo.Uni-Koeln.DE,
        walter@geo.Uni-Koeln.DE, audenrie@geo.Uni-Koeln.DE,
        kuerten@geo.Uni-Koeln.DE, hahn@geo.Uni-Koeln.DE,
        stanzel@geo.Uni-Koeln.DE, carone@geo.Uni-Koeln.DE,
        walter@geo.Uni-Koeln.DE, bernd.haeusler@unibw-muenchen.de,
        joerg.selle@unibw-muenchen.de, sami.asmar@jpl.nasa.gov,
        gene.goltz@jpl.nasa.gov, Daniel.S.Kahan@jpl.nasa.gov,
        dwight.holmes@jpl.nasa.gov, len.tyler@stanford.edu,
        dhinson@stanford.edu, jtwicken@stanford.edu, tzegers@rssd.esa.int,
        fred.jansen@esa.int, rene.pischel@rssd.esa.int, John.Reynolds@esa.int,
        Michel.Denis@esa.int, Olivier.Reboud@esa.int, H.J.Walker@rl.ac.uk,
        mexmps@esa.int, JValencia@jftl.jpl.nasa.gov,
        JVelasco@jftl.jpl.nasa.gov, Ricardo.G.Torres@jpl.nasa.gov,
        Sophia.M.No@jpl.nasa.gov, thomas.w.thompson@jpl.nasa.gov,
        art.freiley@jpl.nasa.gov, john.c.klose@jpl.nasa.gov, rsimpson
Subject: MEX BSR Preliminary Results
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MEX BSR Support People:

  After our first specular point experiment on 22 January, I promised you
a plot showing what we collected.  The plot is attached.

  The left panel shows average spectra from X-Band right circular
polarization (X-RCP); each curve is the average of 210 seconds of data.
The right panel shows the corresponding X-Band left circular (X-LCP)
echoes.  Time increases from front (bottom) to back (top).

  The baseline is the background microwave radiothermal noise; from the
earliest spectra you can see that it is about 7.5 zW (10^-21 watts) on
each channel.  The gaussian-shaped signal is the surface echo; its width
is proportional to the rms surface roughness Z and its strength is
proportional to the Fresnel reflectivity of the surface material.  By
taking the ratio of the echo power in the two channels and accounting for
the angle of incidence on the surface, we can obtain the material
dielectric constant E.

  You can see from the plots that X-LCP is stronger by a factor of about 2
at the beginning but that X-RCP is stronger by about 30 percent at the end.
At the Brewster angle (B), the two signals are equal; the dielectric
constant in that case is very simply   E = [tan(B)]^2

  The specular point moved from about (40N,93E) to about (48N,88E) during
the observations and the MEX HGA illuminated an area about 300 km across;
so our coverage is not extensive and our resolution (before Doppler
sorting) is not very good.  But we do see a change during the experiment
from (Z=2.7 deg, E=3.9) to (Z=3.3 deg, E = 3.5).  The values for E are
higher than expected, but consistent with results obtained from the HGA
inertial experiment conducted on 2005/346, also in northern plains.

  In the last 4-5 pairs, you can see features drifting through the spectra;
these result from inhomogeneities in the scattering surface illuminated by
the HGA.  They can often be attributed to craters.  The specular point
moves from featureless northern plains into an area with a few craters at
the end, but I was not able to associate these features with anything
specific in a quick check with photomosaics or geologic maps.  That may
come later and is not entirely surprising; the X-band signal is most
sensitive to surface structure having dimensions of a few centimeters to
a few meters, which is below the resolution of most imaging instruments.

  For comparison, each 2-3 pairs of spectra (< 10 min) from this specular
point experiment is roughly equivalent in science value to an entire
experiment conducted with HGA inertial pointing.

  One negative note: because the S-RCP maser failed the previous day and
could not be repaired in time for the observations on 2006/022, we have
only the LCP channel from S-Band.  LCP appears to be well-calibrated; but
the S-Band signals are always much weaker and the fact that we cannot find
the RCP/LCP ratio means that the S-Band analysis will be more difficult.

  With the exception of a couple errors in the calibration procedure, an
MGS interference problem (which has been mostly corrected), and the maser
problem on S-RCP, these data are among the best we have collected
in terms of system stability and calibration accuracy; I have a very high
confidence in the numbers which will result.

  Please note that what I have said above is preliminary and intended to
provide you with feedback on the experiment execution.  You should not
forward the plot or these comments beyond the current distribution list
without permission of the MaRS Team Leader, Martin Paetzold.

  Many thanks for your assistance in making this experiment possible.  I
look forward to many future opportunities to explore Mars with specular
point tracking in MEX BSR.

Dick Simpson

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                               ...