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Quick Review of Remote Sensing Basic Theory Paolo Antonelli CIMSS University of Wisconsin-Madison South Africa, April

Quick Review of Remote Sensing Basic Theory Paolo Antonelli CIMSS University of Wisconsin-Madison South Africa, April 2006. Outline. Visible and Near Infrared: Vegetation Planck Function Infrared: Thermal Sensitivity. Visible (Reflective Bands). Infrared (Emissive Bands).

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Quick Review of Remote Sensing Basic Theory Paolo Antonelli CIMSS University of Wisconsin-Madison South Africa, April

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  1. Quick Review of Remote SensingBasic TheoryPaolo AntonelliCIMSSUniversity of Wisconsin-MadisonSouth Africa, April 2006

  2. Outline • Visible and Near Infrared: Vegetation • Planck Function • Infrared: Thermal Sensitivity

  3. Visible (Reflective Bands) Infrared (Emissive Bands)

  4. MODIS BAND 1 (RED) Low reflectance in Vegetated areas Higher reflectance in Non-vegetated land areas

  5. MODIS BAND 2 (NIR) Higher reflectance in Vegetated areas Lower reflectance in Non-vegetated land areas

  6. RED NIR Dense Vegetation Barren Soil

  7. NIR and VIS over Vegetation and Ocean Vegetation Ocean NIR (.86 micron) Green (.55 micron) Red (0.67 micron) RGB NIR

  8. Visible (Reflective Bands) Infrared (Emissive Bands)

  9. Spectral Characteristics of Energy Sources and Sensing Systems NIR IR

  10. Spectral Distribution of Energy Radiated from Blackbodies at Various Temperatures

  11. Radiation is governed by Planck’s Law In wavelenght: B(,T) = c1/{ 5 [e c2/T -1] }(mW/m2/ster/cm) where  = wavelength (cm) T = temperature of emitting surface (deg K) c1 = 1.191044 x 10-8 (W/m2/ster/cm-4) c2 = 1.438769 (cm deg K) In wavenumber: B(,T) = c13 / [e c2/T -1] (mW/m2/ster/cm-1) where  = # wavelengths in one centimeter (cm-1) T = temperature of emitting surface (deg K) c1 = 1.191044 x 10-5 (mW/m2/ster/cm-4) c2 = 1.438769 (cm deg K)

  12. B(max,T)~T5 B(max,T)~T3 max ≠(1/max) B(,T) versus B(,T) B(,T) B(,T) 100 20 10 6.6 5 4 3.3 wavelength [µm]

  13. wavelength  : distance between peaks (µm) Slide 4 wavenumber  : number of waves per unit distance (cm) =1/  d=-1/ 2 d 

  14. Using wavenumbers Wien's Law dB(max,T) / dT = 0 where (max) = 1.95T indicates peak of Planck function curve shifts to shorter wavelengths (greater wavenumbers) with temperature increase. Note B(max,T) ~ T**3.  Stefan-Boltzmann Law E =  B(,T) d = T4, where  = 5.67 x 10-8 W/m2/deg4. o states that irradiance of a black body (area under Planck curve) is proportional to T4 . Brightness Temperature c13 T = c2/[ln(______ + 1)] is determined by inverting Planck function B Brightness temperature is uniquely related to radiance for a given wavelength by the Planck function.

  15. Using wavenumbersUsing wavelengths c2/T c2/T B(,T) = c13 / [e -1] B(,T) = c1/{ 5 [e -1] } (mW/m2/ster/cm-1) (mW/m2/ster/cm) (max in cm-1) = 1.95T (max in cm)T = 0.2897 B(max,T) ~ T**3. B( max,T) ~ T**5.   E =  B(,T) d = T4, E =  B(,T) d  = T4, o o c13 c1 T = c2/[ln(______ + 1)] T = c2/[ ln(______ + 1)] B 5 B

  16. MODIS Planck Function and MODIS Bands

  17. MODIS BAND 20 • Window Channel: • little atmospheric absorption • surface features clearly visible Clouds are cold

  18. MODIS BAND 31 • Window Channel: • little atmospheric absorption • surface features clearly visible Clouds are cold

  19. Clouds at 11 µm look bigger than at 4 µm

  20. Temperature sensitivity dB/B =  dT/T The Temperature Sensitivity  is the percentage change in radiance corresponding to a percentage change in temperature Substituting the Planck Expression, the equation can be solved in : =c2/T

  21. ∆B11> ∆B4 ∆B11 T=300 K Tref=220 K ∆B4

  22. ∆B4/B4= 4∆T/T ∆B11/B11 = 11∆T/T ∆B4/B4>∆B11/B11  4 > 11 (values in plot are referred to wavelength)

  23. (Approximation of) B as function of  and T ∆B/B= ∆T/T Integrating the Temperature Sensitivity Equation Between Tref and T (Bref and B): B=Bref(T/Tref) Where =c2/T (in wavenumber space)

  24. B=Bref(T/Tref)B=(Bref/ Tref) T B T  The temperature sensitivity indicates the power to which the Planck radiance depends on temperature, since B proportional to T satisfies the equation. For infrared wavelengths,  = c2/T = c2/T. __________________________________________________________________ Wavenumber Typical Scene Temperature Temperature Sensitivity 900 300 4.32 2500 300 11.99

  25. N Tcold=220 K 1-N Thot=300 K Non-Homogeneous FOV B=NB(Thot)+(1-N)B(Tcold) BT=NBThot+(1-N)BTcold

  26. N 1-N Tcold Thot For NON-UNIFORM FOVs: Bobs=NBcold+(1-N)Bhot Bobs=N Bref(Tcold/Tref)+ (1-N) Bref(Thot/Tref) Bobs= Bref(1/Tref) (N Tcold + (1-N)Thot) For N=.5 Bobs= .5Bref(1/Tref) ( Tcold + Thot) Bobs= .5Bref(1/TrefTcold) (1+ (Thot/ Tcold)) The greater  the more predominant the hot term At 4 µm (=12) the hot term more dominating than at 11 µm (=4)

  27. Consequences • At 4 µm (=12) clouds look smaller than at 11 µm (=4) • In presence of fires the difference BT4-BT11 is larger than the solar contribution • The different response in these 2 windows allow for cloud detection and for fire detection

  28. Conclusions • Vegetation: highly reflective in the Near Infrared and highly absorptive in the visible red. The contrast between these channels is a useful indicator of the status of the vegetation; • Planck Function: at any wavenumber/wavelength relates the temperature of the observed target to its radiance (for Blackbodies) • Thermal Sensitivity: different emissive channels respond differently to target temperature variations. Thermal Sensitivity helps in explaining why, and allows for cloud and fire detection.

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