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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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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









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





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



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
























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 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.




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