1. Remote sensing: the collection of information about an object without being in direct physical contact with the object. the collection of information about an object without being in direct physical contact with the object. Jensen, 2000

2. Solar and Heliospheric Observatory (SOHO) Image of the Sun Obtained on September 14, 1999 Solar and Heliospheric Observatory (SOHO) Image of the Sun Obtained on September 14, 1999

3. Sources of Electromagnetic Energy Thermonuclear fusion on the surface of the Sun yields a continuous spectrum of electromagnetic energy. The 6,000 ˚K temperature of this process produces a large amount of short wavelength energy (from 0.4 - 0.7  m; blue, green, and red light) that travels through the vacuum of space at the speed of light. Some energy is intercepted by the Earth where it interacts with the atmosphere and surface materials. The Earth may reflect some of the energy directly back out to space or it may absorb the short wavelength energy and then re-emit it at a longer wavelength.

4. Wave Model of Electromagnetic Energy An electromagnetic wave is composed of electric and magnetic vectors that are orthogonal to one another and travel from the source at the speed of light (3 x 10 8 m s -1 ).

5. Wave Model of Electromagnetic Energy This illustration of an electromagnetic wave shows the inverse relationship between wavelength ( ) and frequency ( ). The longer the wavelength the lower the frequency; and vice versa. The amplitude of an electromagnetic wave is the height of the wave crest above the undisturbed position. Successive wave crests are numbered 1, 2, 3, and 4. An observer at the position of the clock records the number of crests that pass by in a second. This frequency is measured in cycles per second, or Hertz This illustration of an electromagnetic wave shows the inverse relationship between wavelength ( ) and frequency ( ). The longer the wavelength the lower the frequency; and vice versa. The amplitude of an electromagnetic wave is the height of the wave crest above the undisturbed position. Successive wave crests are numbered 1, 2, 3, and 4. An observer at the position of the clock records the number of crests that pass by in a second. This frequency is measured in cycles per second, or Hertz

6. The relationship between the wavelength,, and frequency,, of electromagnetic radiation is based on the following formula, where c is the speed of light: c =   c  Note that frequency, is inversely proportional to wavelength, The longer the wavelength, the lower the frequency; the shorter the wavelength, the higher the frequency. The relationship between the wavelength,, and frequency,, of electromagnetic radiation is based on the following formula, where c is the speed of light: c =   c  Note that frequency, is inversely proportional to wavelength, The longer the wavelength, the lower the frequency; the shorter the wavelength, the higher the frequency. Wave Model of Electromagnetic Energy

7. Using the wave model, it is possible to characterize the energy of the Sun which represents the ultimate source of most of the electromagnetic energy recorded by remote sensing systems (except radar). We may think of the Sun as a 6,000 ˚K blackbody (a theoretical construct which radiates energy at the maximum possible rate per unit area at each wavelength for any given temperature). The total emitted radiation (M ) from a blackbody is proportional to the fourth power of its absolute temperature. This is known as the Stefan-Boltzmann law and is expressed as: M =  T 4 where  is the Stefan-Boltzmann constant, 5.6697 x 10 -8 W m -2 K -4. Thus, the amount of energy emitted by an object such as the Sun or the Earth is a function of its temperature. Using the wave model, it is possible to characterize the energy of the Sun which represents the ultimate source of most of the electromagnetic energy recorded by remote sensing systems (except radar). We may think of the Sun as a 6,000 ˚K blackbody (a theoretical construct which radiates energy at the maximum possible rate per unit area at each wavelength for any given temperature). The total emitted radiation (M ) from a blackbody is proportional to the fourth power of its absolute temperature. This is known as the Stefan-Boltzmann law and is expressed as: M =  T 4 where  is the Stefan-Boltzmann constant, 5.6697 x 10 -8 W m -2 K -4. Thus, the amount of energy emitted by an object such as the Sun or the Earth is a function of its temperature. Stefan-Boltzmann Law

8. Radiant Intensity of the Sun Radiant Intensity of the Sun The Sun approximates a 6,000 K blackbody with a dominant wavelength of 0.5  m (green light). Earth approximates a 300 K blackbody with a dominant wavelength of 9.7  m. The 6,000 K Sun produces 41% of its energy in the visible region from 0.4 - 0.7  m (blue, green, and red light). The other 59% of the energy is in wavelengths shorter than blue light ( 0.7  m). Eyes are only sensitive to light from the 0.4 to 0.7  m. Remote sensor detectors can be made sensitive to energy in the non- visible regions of the spectrum. Jensen, 2000

9. In addition to computing the total amount of energy exiting a theoretical blackbody such as the Sun, we can also compute its dominant wavelength ( max ) as: max = k / T where k is a constant equaling 2898  m ˚K, and T is temperature in degrees Kelvin. The Sun approximates a 6,000 ˚K blackbody, therefore its dominant wavelength is:  m = 2898  m ˚K / 6000 ˚ K In addition to computing the total amount of energy exiting a theoretical blackbody such as the Sun, we can also compute its dominant wavelength ( max ) as: max = k / T where k is a constant equaling 2898  m ˚K, and T is temperature in degrees Kelvin. The Sun approximates a 6,000 ˚K blackbody, therefore its dominant wavelength is:  m = 2898  m ˚K / 6000 ˚ K Wien’s Displacement Law

10. Blackbody Radiation Curves Blackbody Radiation Curves Blackbody radiation curves for several objects including the Sun and the Earth which approximate 6,000 ˚K and 300 ˚K blackbodies, respectively. Notice that as the temperature of the object increases, its dominant wavelength shifts toward the short wavelength portion of the spectrum. Jensen, 2000

11. Remote Sensing Flow Chart

12. Energy-matter Interactions in the Atmosphere, at the Study Area, and at the Remote Sensor Detector

13. Scattering Scatter differs from reflection in that the direction associated with scattering is unpredictable, whereas the direction of reflection is predictable. There are essentially three types of scattering: Rayleigh, Mie, and non-selective scattering. Scatter differs from reflection in that the direction associated with scattering is unpredictable, whereas the direction of reflection is predictable. There are essentially three types of scattering: Rayleigh, Mie, and non-selective scattering.

14. Atmospheric Scattering Atmospheric Scattering The type of scattering is a function of: the wavelength of the incident radiant energy, and the size of the gas molecule, dust particle, or water vapor droplet encountered. The type of scattering is a function of: the wavelength of the incident radiant energy, and the size of the gas molecule, dust particle, or water vapor droplet encountered.

15. Rayleigh Scattering Rayleigh Scattering The intensity of Rayleigh scattering varies inversely with the fourth power of the wavelength ( -4 ). The intensity of Rayleigh scattering varies inversely with the fourth power of the wavelength ( -4 ).

16. Deforestation

17. Absorption of the Sun's Incident Electromagnetic Energy in the Region from 0.1 to 30  m by Various Atmospheric Gases Absorption of the Sun's Incident Electromagnetic Energy in the Region from 0.1 to 30  m by Various Atmospheric Gases

19. Remote Sensing Flow Chart

20. Radiometric Quantities Radiometric quantities have been developed that allow us to keep careful record of the incident and exiting radiant flux. The simple radiation budget equation states that the total amount of radiant flux incident to the terrain (I ) in specific wavelengths, must be accounted for by evaluating the amount of energy reflected from the surface (r ), the amount of energy absorbed by the surface (  ), and the amount of radiant energy transmitted through the surface (  ), where: I    r  +  +  The radiometric quantities are based on the amount of radiant incident to a surface from any angle in a hemisphere (i.e. a half of a sphere). Radiometric quantities have been developed that allow us to keep careful record of the incident and exiting radiant flux. The simple radiation budget equation states that the total amount of radiant flux incident to the terrain (I ) in specific wavelengths, must be accounted for by evaluating the amount of energy reflected from the surface (r ), the amount of energy absorbed by the surface (  ), and the amount of radiant energy transmitted through the surface (  ), where: I    r  +  +  The radiometric quantities are based on the amount of radiant incident to a surface from any angle in a hemisphere (i.e. a half of a sphere).

21. Reflectance Reflectance is the process whereby radiation “bounces off” an object like a cloud or the terrain. Actually, the process is more complicated, involving re-radiation of photons in unison by atoms or molecules in a layer one- half wavelength deep. Reflection exhibits fundamental characteristics that are important in remote sensing. First, the incident radiation, the reflected radiation, and a vertical to the surface from which the angles of incidence and reflection are measured all lie in the same plane. Second, the angle of incidence and the angle of reflection are equal. Reflectance is the process whereby radiation “bounces off” an object like a cloud or the terrain. Actually, the process is more complicated, involving re-radiation of photons in unison by atoms or molecules in a layer one- half wavelength deep. Reflection exhibits fundamental characteristics that are important in remote sensing. First, the incident radiation, the reflected radiation, and a vertical to the surface from which the angles of incidence and reflection are measured all lie in the same plane. Second, the angle of incidence and the angle of reflection are equal.

22. Reflectance

23. Radiometric Quantities We often take the hemispherical reflectance equation and multiply it by 100 to obtain an expression for percent spectral reflectance (p r ), r  p r   x 100  This quantity is used in remote sensing research to describe the general spectral reflectance characteristics of various materials. We often take the hemispherical reflectance equation and multiply it by 100 to obtain an expression for percent spectral reflectance (p r ), r  p r   x 100  This quantity is used in remote sensing research to describe the general spectral reflectance characteristics of various materials.

24. Spectral Reflectance Curves of Selected Materials

25. Spectral Bandwidths of Landsat and SPOT Sensor Systems

26. Spectral Reflectance Curves of Selected Materials Jensen, 2000

27. Landsat MSS Bandwidths

28. Spectral Resolution Jensen, 2000

29. Remote Sensing Flow Chart