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Joe Tenerelli SMOS L2OS Progress Meeting Arles, France, September 26, 2011 PowerPoint PPT Presentation


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UPDATE ON SMOS LONG-TERM BIASES OVER THE OCEAN AND ROUGH SURFACE SCATTERING OF CELESTIAL SKY NOISE. Joe Tenerelli SMOS L2OS Progress Meeting Arles, France, September 26, 2011. SMOS PASSES USED IN THIS ANALYSIS. DRIFT IN 2010 ONLY. NO LOSS MODEL. ONE-SLOPE LOSS MODEL.

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Joe Tenerelli SMOS L2OS Progress Meeting Arles, France, September 26, 2011

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UPDATE ON SMOS LONG-TERM BIASES OVER THE OCEAN AND ROUGH SURFACE SCATTERING OF CELESTIAL SKY NOISE

Joe Tenerelli

SMOS L2OS Progress Meeting

Arles, France, September 26, 2011


SMOS PASSES USED IN THIS ANALYSIS


DRIFT IN 2010 ONLY


NO LOSS MODEL


ONE-SLOPE LOSS MODEL


TWO-SLOPE LOSS MODEL


EXTENSION THROUGH JUNE 2011


NO LOSS MODEL


ONE-SLOPE LOSS MODEL

Notice the significantdesc-ascbiasnowappearingwithboth one and twoslopelossmodelsbetweenNov 2010 and April 2011. It is of opposite sign to thatbetween Sep and Dec 2010 observedwith no loss model. It appearsthat the loss correction istoostrong in thisperiod.


TWO-SLOPE LOSS MODEL

The two-slope model seems to degradedesc-ascbias relative to the one-slope model.


ONE-SLOPE LOSS MODEL: IMPACT OF GALACTIC REFLECTION MODEL

It turns out that, for the metricsusedhere, the impact of the formulation of galactic noise scatteringat the surface on desc-ascbiasisquitesmalleven for descending passes in September.

Kirchhoff scatteringmodel for galactic noise


ONE-SLOPE LOSS MODEL: IMPACT OF GALACTIC REFLECTION MODEL

It turns out that, for the metricsusedhere, the impact of the formulation of galactic noise scatteringat the surface on desc-ascbiasisquitesmalleven for descending passes in September.

Flat surface reflection model for galactic noise


DRIFT METRICS


LONG TERM DRIFT JAN-DEC 2010


LONG TERM DRIFT JUN-DEC 2010


LONG TERM DRIFT JUNE 2010 – JUNE 2011

Considering the June 2010 to June 2011 period, thereisverylittle net drift in the AF and EAF FoVs

In the ascending passes.


SHORT TERM DRIFT IN 2010 AND 2011

The two-slope model seems to degradedesc-ascbias relative to the one-slope model.

Two-slopedegradesdesc-ascconsistency


LATEST OPERATIONAL BIAS CURVES


The following are biascurves for operational DPGS Level 1B data:


The following are biascurves for operational DPGS Level 1A data and using JRECON with no direct sun correction:


Comparing Original DPGS with L1PP


NO LOSS MODEL


LATEST OPERATIONAL BIAS CURVES


UPDATE ON GALACTIC NOISE MODEL


UPDATE ON GALACTIC NOISE MODEL


UPDATE ON GALACTIC NOISE MODEL


UPDATE ON GALACTIC NOISE MODEL


UPDATE ON GALACTIC NOISE MODEL


CELESTIAL SKY NOISE MAPS


HOVMOLLER PLOTS OF REFLECTED SKY NOISE


SMOS RESIDUALS BASED ON COMMISSIONING REPROCESSING DATA


SMOS RESIDUALS BASED ON COMMISSIONING REPROCESSING DATA


FITTING A GEOMETRIC OPTICS MODEL TO THE RESIDUALS


FITTING A GEOMETRIC OPTICS MODEL TO THE RESIDUALS


FITTING A GEOMETRIC OPTICS MODEL TO THE RESIDUALS


FITTING A GEOMETRIC OPTICS MODEL TO THE RESIDUALS


FITTING A GEOMETRIC OPTICS MODEL TO THE RESIDUALS


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS

NEW SEMI-EMPIRICAL MODEL


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS

ORIGINAL KIRCHHOFF MODEL


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS

NEW SEMI-EMPIRICAL MODEL: Ascending Passes


CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPS

NEW SEMI-EMPIRICAL MODEL: Descending passes


IMPACT ON CELESTIAL SKY BIASES


BIAS: ORIGINAL KIRCHHOFF MODEL


BIAS: KIRCHHOFF MODEL EVALUATED AT 3 M/S WIND SPEED


BIAS: EMPIRICAL GEOMETRIC OPTIC


NEW SEMI-EMPIRICAL GO MODEL SWATH RESULTS


IMPACT ON SWATH BIASES: ALIAS-FREE FIELD OF VIEW


IMPACT ON SWATH BIASES: ALIAS-FREE FIELD OF VIEW


IMPACT ON SWATH BIASES: ALIAS-FREE FIELD OF VIEW


IMPACT OF GALACTIC MODEL ON BIAS TREND ANALYSIS


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

The curves show the contribution of scatteredcelestialsky noise to FoVbiases, basedupon the Kirchhoff model evaluatedat a 3 m/s wind speed.


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

Similar to previousslide but for the flat surface reflectedcelestialsky noise.


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

The biascurvesbelowwerecomputedusing the original Kirchhoff model evaluatedat a 3 m/s wind speed.


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

With the new empiricalgeometricoptics model the curves change verylittle.


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

Evenswitching to flat surface reflectedgalactic noise makeslittledifference:


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

For thesecurveswe have used the original theoreticalroughnessemission model. This alsomakeslittledifference.


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS


IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS


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