PRINCIPLES OF REMOTE SENSING. Electromagnetic Energy and Spectral Signatures

Size: px

Start display at page:

Download "PRINCIPLES OF REMOTE SENSING. Electromagnetic Energy and Spectral Signatures"

Cleopatra Lawson
6 years ago
Views:

1 PRINCIPLES OF REMOTE SENSING Electromagnetic Energy and Spectral Signatures

2 Remote sensing is the science and art of acquiring and analyzing information about objects or phenomena from a distance. As humans, we are intimately familiar with remote sensing in that we rely on visual perception to provide us with much of the information about our surroundings. As sensors, however, our eyes are greatly limited by 1) sensitivity to only the visible range of electromagnetic energy; 2) viewing perspectives dictated by the location of our bodies; and 3) the inability to form a lasting record of what we view. Because of these limitations, humans have continuously sought to develop technology that would enable us to increase our ability to see and record the physical properties of our environment. WHY REMOTE SENSING?

3 The Society of American Foresters, the national scientific and educational organization of the forestry profession, compiled a "top ten" list of forestry-related advances in the United States over the past century. One of those advances was: Remote sensing and other technologies. Through technology such as remote sensing, foresters can monitor the health of the forest, target management activities, map fire outbreak, and identify wildlife and fish habitat for protection. WHY REMOTE SENSING?

4 Satellite remote sensing, with its synoptic view of the earth s features, regular repetitive coverage over large areas, and digital mode of data capture, offers an effective means of inventorying and updating natural resources information, monitoring land use changes and environmental impacts near real time, and providing a historical profile for the purpose of policy formulation.. WHY REMOTE SENSING?

5 Together with Geographic Information Systems (GIS) and Global Positioning Systems (GPS), remotely sensed data can be analysed spatially, rapidly and accurately for timely decision making in order to address current issues relating to natural resources security, natural disaster mitigation and environmental protection. (Malaysian Centre for Remote Sensing (MACRES)) WHY REMOTE SENSING?

6 Different rock types? Vegetation? Snow depth? Topography? HOW TO REMOTELY SENSE?

7 Passive sensors Object = Target Eye = Sensor FOLLOWING OUR DESIGN

8 Passive sensors Beyond vision TO REMOTELY SENSE

9 Active sensors FOLLOWING OUR DESIGN

10 Active sensors RADAR TO REMOTELY SENSE LIDAR

11 A: Source of EMR B: Electromagnetic radiation (EMR) C: Object of interest D: Sensor E: Transmission to receiver(s) F: Data products G: Results of analyses B A A FORMALLY, A REMOTE SENSING SYSTEM

12 λ f or v Note that different groups reverse the order (placing Gamma Rays at the far left). The glue that holds it all together ELECTROMAGNETIC RADIATION

Wavelengths (λ) are the predominant means by which we (Geographic Remote Sensors)

Wavelengths are inversely related to frequency (f) by this equation: c = λ f (where

13 Wavelengths (λ) are the predominant means by which we (Geographic Remote Sensors) refer to EMR. Wavelengths are inversely related to frequency (f) by this equation: c = λ f (where c = speed of light, a constant) Thus, as the λ increases, the f decreases (because c is a constant). Frequency is directly related to our ability to detect the wavelength, since the lower the f, the less the energy (i.e., photons). WAVES / PARTICLES f = v (Also, think about the relation between temperature and wavelength.)

14 As a result, the longer the wavelength, the harder it will be to detect. This means that the detector needs to be more sensitive in order to detect it, and / or the source area needs to be larger, in order for the sensor to capture enough energy from the target area. This is why, in most remotely sensed data, less spatial detail is available for passive infrared images. Near Infrared Far Infrared Green Red Near Infrared Blue Sensor Sensor Sensor WAVES AND PHOTONS

15 m 1 m = 10 9 nm Wavelength THE VISIBLE SPECTRUM

16 Why we see the colours we do. THE VISIBLE SPECTRUM

Images taken in very narrow bands have the wavelengths of the associated waves noted (in nanometers).

17 The Sun emits electromagnetic radiation at many wavelengths across the EM spectrum. These images show the Sun in the infrared, visible light, four different ultraviolet wavelengths, and in X-rays. Images taken in very narrow bands have the wavelengths of the associated waves noted (in nanometers). The photosphere is most prominent in the visible light images, while UV and X-ray views show details of the solar atmosphere. Note that almost all of these images are "false color" representations, since your eyes cannot see X-rays or ultraviolet or infrared "light". THE SOURCE FOR MOST SYSTEMS

18 The wavelength of maximum emission ( ) of any body is inversely proportional to its absolute (K) temperature. Thus, the higher the temperature, the shorter the wavelength that is emitted the most. This phenomenon is often called Wien's Law. The following equation describes this law: Where b is a constant ~ 2900 μm K, T is the temperature (Kelvin) WHERE?

19 The amount of electromagnetic radiation emitted by a body is directly related to its temperature. If the body is a perfect emitter (i.e., a black body), the amount of radiation given off is proportional to the 4th power of its temperature as measured in Kelvin. This natural phenomenon is described by the Stefan-Boltzmann Law. The following simple equation describes this law: HOW MUCH?

20 The area under the curve. STEFAN-BOLTZMANN LAW

21 1 m = 10 6 micrometres. STEFAN-BOLTZMANN AND WIEN S LAWS

22 Note how the Infrared wavelengths are divided into Near IR and Far IR. The sun s temperature is around 6000 K The earth s temperature is around 300 K Note that the graph axes are logarithmic. WIEN S AND STEFAN-BOLTZMANN LAWS demo

23 What happens to EMR in the atmosphere? Passive systems Beyond vision TO REMOTELY SENSE

24 In remote sensing of the earth, the sensor is looking through a layer of atmosphere separating the sensor from the Earth's surface being observed. Hence, it is essential to understand the effects of atmosphere on the electromagnetic radiation travelling from the Earth to the sensor through the atmosphere. The atmospheric constituents cause wavelength-dependent absorption and scattering of radiation. These effects degrade the quality of images, although some of the atmospheric effects can be corrected for. THE ATMOSPHERE

Rayleigh scattering occurs when particles are very small compared to the wavelength of the radiation. These could be particles such as small specks of dust or nitrogen and oxygen molecules.

25 Rayleigh scattering occurs when particles are very small compared to the wavelength of the radiation. These could be particles such as small specks of dust or nitrogen and oxygen molecules. Rayleigh scattering causes shorter wavelengths of energy to be scattered much more than longer wavelengths. Rayleigh scattering is the dominant scattering mechanism in the upper atmosphere. WHY THE SKY IS BLUE

26 WHY SUNSETS ARE RED 1/sin(sun s angle)

27 Mie scattering occurs when the particles are just about the same size as the wavelength of the radiation. Dust, pollen, smoke and water vapour are common causes of Mie scattering, which tends to affect wavelengths longer than those affected by Rayleigh scattering. Mie scattering occurs mostly in the lower portions of the atmosphere where larger particles are more abundant, and dominates when cloud conditions are overcast. WHY CLOUDS ARE WHITE

28 NOT ALL GETS THROUGH Absorption is the other main mechanism at work when electromagnetic radiation interacts with the atmosphere. In contrast to scattering, this phenomenon causes molecules in the atmosphere to absorb energy at various wavelengths. Ozone, carbon dioxide, and water vapour are the three main atmospheric constituents which absorb radiation.

29 The Sun, if a perfect Black body Black body radiation Mie scattering, Rayleigh scattering, Absorption, etc. THE END OF (BLACK BODY) PERFECTION 1 micron = 1000 nanometres

30 ATMOSPHERIC WINDOWS The windows are conceptual, not physical.

31 ATMOSPHERIC WINDOWS

32 What happens when EMR strikes an object (or is emitted by an object)? Passive systems Beyond vision TO REMOTELY SENSE

33 THE DIFFERENCES THAT MAKE A DIFFERENCE

34 In remote sensing of the earth, the sensor is recording the EMR reflected by the Earth's surface and by the atmosphere. Generally we are primarily interested in the surface effects, and therefore understanding how EMR interacts with surface features is important. There will be object-specific wavelength-dependent absorption, scattering and emission of radiation. These effects provide the basis for identifying features in remotely sensed images. NOT THE ATMOSPHERE

35 A surface s flatness is relative to the wavelength striking it The differences that make a difference

36 D EMR can be: Reflected like a mirror (Specular reflection), reflected uniformly in all directions (Diffuse reflection), or, as in most cases, the reflection properties will lie somewhere in between. S BIDIRECTIONAL REFLECTANCE

37 The angle at which the EMR strikes the object can have a significant effect, depending on the surface characteristics. Topography is, therefore, a significant factor. THE DIFFERENCES THAT MAKE A DIFFERENCE

38 WHY VEGETATION IS GREEN The differences that make a difference

39 SPECTRAL REFLECTANCE CURVES

40 Vegetation under stress reflects that stress. (Actually, it reflects less when under stress, and we can detect that.) SPECTRAL REFLECTANCE CURVES

41 The glue that holds it all together NAMED SPECTRAL REGIONS

It is useful to consider the different spectral regions (gamma rays,

) and how important they might be to a remote sensor.

42 It is useful to consider the different spectral regions (gamma rays, visible light, infrared, etc.) and how important they might be to a remote sensor. Gamma and X-rays: Almost fully blocked by the atmosphere, therefore of no use in satellite remote sensing. Ultraviolet: nm; mostly blocked by the Earth s atmosphere (O 3 absorption), but a window exists at nm. Useful in detecting oil slicks. NAMED SPECTRAL REGIONS

Visible: 400-700 nm; peak solar wavelengths, atmospheric window fairly transparent.

495-0.570 um) Red (0.620-0.750 um) Panchromatic? Read the CBC s handout.

43 Visible: nm; peak solar wavelengths, atmospheric window fairly transparent. The visible spectrum is typically divided into three regions: Blue ( um) Green ( um) Red ( um) Panchromatic? Read the CBC s handout. How constant are these terms? Yellow and orange lie between green and red, but typically aren t named ( um) NAMED SPECTRAL REGIONS

Reflective (near) infrared: 700-3000 nm (0.7-3.

0 10,000 ųm; emitted by the earth and other warm

44 Reflective (near) infrared: nm ( ųm); a number of atmospheric windows exist; photographic IR is limited to ųm Thermal (far) infrared: ,000 ųm; emitted by the earth and other warm objects, majority absorbed by water vapour and CO 2 in atmosphere NAMED SPECTRAL REGIONS

45 THERMAL IMAGING SENSORS

46 Microwave: cm; wavelengths used in RADAR, atmosphere window fairly transparent, a large number of named microwave regions SPECTRAL REGIONS

47 At any given time our ability to detect EMR is limited by the current technology. Therefore, every sensor reflects a compromise a decision has to be made as to which regions to detect (that is, we can t detect ALL the useful EMR regions, so we detect those that we feel would provide the greatest amount of information). Every sensor is designed to detect selected bands within the various EMR regions. Thus, although spectral reflectance is a continuous curve, the use of bands discretizes that curve. Analog versus digital SENSING A COMPROMISE

For example: ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer) is an imaging instrument flying on Terra, a satellite launched in December 1999 as part of NASA's Earth Observing

48 For example: ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer) is an imaging instrument flying on Terra, a satellite launched in December 1999 as part of NASA's Earth Observing System (EOS). ASTER is being used to obtain detailed maps of land surface temperature, reflectance and elevation. Red Green Blue Sensor Near Infrared Near Infrared Sensor Note the increasing funnel sizes (aka decreasing spatial resolution) as the wavelengths increase (15 m visible and VNIR, 30 m SWIR, 90 m TIR) for ASTER images. SENSING A COMPROMISE

49 TO EACH THEIR OWN

50 EMR is the thing being sensed by remote sensing devices. EMR is affected by the atmosphere (absorption, scattering, transmission) Atmospheric windows EMR is affected by the target (absorption, reflectance, transmission, emission); this effect is dependent on the angle of incidence. All of these effects are wavelength-dependent. A SUMMARY

51 Regions with the EM spectrum are dissected into bands by different sensors. The shorter the wavelength the easier it is to detect it (because it has greater energy associated with it). Sensors can be either active (RADAR, LiDAR) or passive (e.g., MSS, SPOT, ASTER, MODIS). SUMMARY

52 GOTLAND ISLAND AND PHYTOPLANKTON SWIRLS

Electromagnetic Waves

ELECTROMAGNETIC RADIATION AND THE ELECTROMAGNETIC SPECTRUM Electromagnetic Radiation (EMR) THE ELECTROMAGNETIC SPECTRUM Electromagnetic Waves A wave is characterized by: Wavelength (λ - lambda) is the