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. - PowerPoint PPT Presentation

Transcript of 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 NOISEJoe TenerelliSMOS L2OS Progress MeetingArles, France, September 26, 2011

SMOS PASSES USED IN THIS ANALYSISDRIFT IN 2010 ONLY

NO LOSS MODEL

ONE-SLOPE LOSS MODEL

TWO-SLOPE LOSS MODELEXTENSION THROUGH JUNE 2011

NO LOSS MODEL

ONE-SLOPE LOSS MODELNotice the significant desc-asc bias now appearing with both one and two slope loss models between Nov 2010 and April 2011. It is of opposite sign to that between Sep and Dec 2010 observed with no loss model. It appears that the loss correction is too strong in this period.

TWO-SLOPE LOSS MODELThe two-slope model seems to degrade desc-asc bias relative to the one-slope model.

ONE-SLOPE LOSS MODEL: IMPACT OF GALACTIC REFLECTION MODELIt turns out that, for the metrics used here, the impact of the formulation of galactic noise scattering at the surface on desc-asc bias is quite small even for descending passes in September.Kirchhoff scattering model for galactic noise

ONE-SLOPE LOSS MODEL: IMPACT OF GALACTIC REFLECTION MODELIt turns out that, for the metrics used here, the impact of the formulation of galactic noise scattering at the surface on desc-asc bias is quite small even for descending passes in September.Flat surface reflection model for galactic noiseDRIFT METRICSLONG 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, there is very little net drift in the AF and EAF FoVsIn the ascending passes. SHORT TERM DRIFT IN 2010 AND 2011

The two-slope model seems to degrade desc-asc bias relative to the one-slope model.Two-slope degrades desc-asc consistencyLATEST OPERATIONAL BIAS CURVES

The following are bias curves for operational DPGS Level 1B data:

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

Comparing Original DPGS with L1PP

NO LOSS MODELLATEST OPERATIONAL BIAS CURVESUPDATE 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 MAPSHOVMOLLER 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 RESIDUALSFITTING 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 MAPSNEW SEMI-EMPIRICAL MODEL

CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPSORIGINAL KIRCHHOFF MODEL

CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPSNEW SEMI-EMPIRICAL MODEL: Ascending Passes

CROSS SECTIONS THROUGH THE CELESTIAL SKY MAPSNEW SEMI-EMPIRICAL MODEL: Descending passesIMPACT 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 RESULTSIMPACT 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 VIEWIMPACT OF GALACTIC MODEL ON BIAS TREND ANALYSIS

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSISThe curves show the contribution of scattered celestial sky noise to FoV biases, based upon the Kirchhoff model evaluated at a 3 m/s wind speed.

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSISSimilar to previous slide but for the flat surface reflected celestial sky noise.

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSISThe bias curves below were computed using the original Kirchhoff model evaluated at a 3 m/s wind speed.

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSISWith the new empirical geometric optics model the curves change very little.

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSISEven switching to flat surface reflected galactic noise makes little difference:

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSISFor these curves we have used the original theoretical roughness emission model. This also makes little difference.IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS

IMPACT OF GALACTIC NOISE MODEL ON BIAS TREND ANALYSIS