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GEOGG141/ GEOG3051 Principles & Practice of Remote Sensing EM Radiation ( ii). Dr. Mathias (Mat) Disney UCL Geography Office: 113, Pearson Building Tel: 7679 0592 Email: mdisney@ucl.geog.ac.uk http://www2.geog.ucl.ac.uk/~mdisney/teaching/GEOGG141/GEOGG141.html - PowerPoint PPT Presentation
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UCL DEPARTMENT OF GEOGRAPHYUCL DEPARTMENT OF GEOGRAPHY
GEOGG141/ GEOG3051Principles & Practice of Remote SensingEM Radiation (ii)
Dr. Mathias (Mat) DisneyUCL GeographyOffice: 113, Pearson BuildingTel: 7679 0592Email: mdisney@ucl.geog.ac.ukhttp://www2.geog.ucl.ac.uk/~mdisney/teaching/GEOGG141/GEOGG141.htmlhttp://www2.geog.ucl.ac.uk/~mdisney/teaching/3051/GEOG3051.html
UCL DEPARTMENT OF GEOGRAPHY
EMR arriving at Earth
2
• We now know how EMR spectrum is distributed• Radiant energy arriving at Earth’s surface• NOT blackbody, but close
• “Solar constant”• solar energy irradiating surface perpendicular to solar beam• ~1373Wm-2 at top of atmosphere (TOA)• Mean distance of sun ~1.5x108km so total solar energy emitted = 4r2x1373
= 3.88x1026W
• Incidentally we can now calculate Tsun (radius=6.69x108m) from SB Law
• T4sun = 3.88x1026/4 r2 so T = ~5800K
UCL DEPARTMENT OF GEOGRAPHY
Departure from blackbody assumption
• Interaction with gases in the atmosphere– attenuation of solar radiation
3
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: spatial relations
4
• Now cover what happens when radiation interacts with Earth System• Atmosphere
• On the way down AND way up• Surface• Multiple interactions between surface and atmosphere• Absorption/scattering of radiation in the atmosphere
UCL DEPARTMENT OF GEOGRAPHY
Radiation passing through media
5
• Various interactions, with different results
From http://rst.gsfc.nasa.gov/Intro/Part2_3html.html
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: spatial relations
6
• Definitions of radiometric quantities• Radiant energy emitted, transmitted of received per unit time is
radiant flux (usually Watts, or Js-1)• Radiant flux density is flux per unit area (Wm-2)
• Irradiance is radiant flux density incident on a surface (Wm-2) e.g. Solar radiation arriving at surface
• Emittance (radiance or radiant exitance) (Wm-2) is radiant flux density emitted by a surface
• For parallel beam, flux density defined in terms of plane perpendicular to beam. What about from a point?
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: point source
7
d dF dAPoint source
r
• Consider flux dF emitted from point source into solid angle d, where dF and d very small• Intensity I defined as flux per unit solid angle i.e. I = dF/d (Wsr-1) • Solid angle d = dA/r2 (steradians, sr)
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: plane source
8
dS cos
dF
Plane source dS
• What about when we have a plane source rather than a point?• Element of surface with area dS emits flux dF in direction at angle to normal• Radiant emittance, M = dF / dS (Wm-2)• Radiance L is intensity in a particular direction (dI = dF/) divided by the apparent area of
source in that direction i.e. flux per unit area per solid angle (Wm-2sr-1)• Projected area of dS is direction is dS cos , so…..• Radiance L = (dF/) / dS cos = dI/dS cos (Wm-2sr-1)
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: radiance
9
• So, radiance equivalent to:• intensity of radiant flux observed in a particular direction
divided by apparent area of source in same direction• Note on solid angle (steradians):
• 3D analog of ordinary angle (radians)• 1 steradian = angle subtended at the centre of a sphere by an
area of surface equal to the square of the radius. The surface of a sphere subtends an angle of 4 steradians at its centre.
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: solid angle
10
• Cone of solid angle = 1sr from sphere
• = area of surface A / radius2
From http://www.intl-light.com/handbook/ch07.html
• Radiant intensity
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: terms and units
11
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: cosine law
12
• Emission and absorption• Radiance linked to law describing spatial distn of radiation emitted by
Bbody with uniform surface temp. T (total emitted flux = T4)• Surface of Bbody then has same T from whatever angle viewed• So intensity of radiation from point on surface, and areal element of
surface MUST be independent of , angle to surface normal• OTOH flux per unit solid angle divided by true area of surface must be
proportional to cos
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: cosine law
13
• Case 1: radiometer ‘sees’ dA, flux proportional to dA• Case 2: radiometer ‘sees’ dA/cos (larger) BUT T same, so emittance of
surface same and hence radiometer measures same• So flux emitted per unit area at angle to cos so that product of
emittance ( cos ) and area emitting ( 1/ cos ) is same for all • This is basis of Lambert’s Cosine Law
Radiometer
X
Y X
Y
Radiometer
dA
dA/cos
Adapted from Monteith and Unsworth, Principles of Environmental Physics
UCL DEPARTMENT OF GEOGRAPHY
Radiation Geometry: Lambert’s Cosine Law
14
• When radiation emitted from Bbody at angle to normal, then flux per unit solid angle emitted by surface is cos
• Corollary of this:• if Bbody exposed to beam of radiant energy at an angle to normal, the
flux density of absorbed radiation is cos • In remote sensing we generally need to consider directions of
both incident AND reflected radiation, then reflectivity is described as bi-directional
Adapted from Monteith and Unsworth, Principles of Environmental Physics
UCL DEPARTMENT OF GEOGRAPHY
Recap: radiance
15
• Radiance, L• power emitted (dF) per unit of solid
angle (d) and per unit of the projected surface (dS cos) of an extended widespread source in a given direction, ( = zenith angle, = azimuth angle)
• L = d2F / (d dS cos ) (in Wm-2sr-1)• If radiance is not dependent on i.e. if
same in all directions, the source is said to be Lambertian. Ordinary surfaces rarely found to be Lambertian.
Ad. From http://ceos.cnes.fr:8100/cdrom-97/ceos1/science/baphygb/chap2/chap2.htm
d
Projected surface dS cos
UCL DEPARTMENT OF GEOGRAPHY
Recap: emittance
16
• Emittance, M (exitance)• emittance (M) is the power emitted
(dW) per surface unit of an extended widespread source, throughout an hemisphere. Radiance is therefore integrated over an hemisphere. If radiance independent of i.e. if same in all directions, the source is said to be Lambertian.
• For Lambertian surface • Remember L = d2F / (d dS cos ) =
constant, so M = dF/dS = • M = L
Ad. From http://ceos.cnes.fr:8100/cdrom-97/ceos1/science/baphygb/chap2/chap2.htm
UCL DEPARTMENT OF GEOGRAPHY
Recap: irradiance
17
• Radiance, L, defined as directional (function of angle)• from source dS along viewing
angle of sensor ( in this 2D case, but more generally (, ) in 3D case)
• Emittance, M, hemispheric • Why??• Solar radiation scattered by
atmosphere• So we have direct AND diffuse
components
Ad. From http://ceos.cnes.fr:8100/cdrom-97/ceos1/science/baphygb/chap2/chap2.htm
Direct
Diffuse
UCL DEPARTMENT OF GEOGRAPHY
Reflectance
18
• Spectral reflectance, (), defined as ratio of incident flux to reflected flux at same wavelength • () = L()/I()
• Extreme cases:• Perfectly specular: radiation incident at angle reflected away from surface
at angle -• Perfectly diffuse (Lambertian): radiation incident at angle reflected
equally in all angles
UCL DEPARTMENT OF GEOGRAPHY
Interactions with the atmosphere
19From http://rst.gsfc.nasa.gov/Intro/Part2_4.html
UCL DEPARTMENT OF GEOGRAPHY
Interactions with the atmosphere
20
• Notice that target reflectance is a function of• Atmospheric irradiance• reflectance outside target scattered into path• diffuse atmospheric irradiance• multiple-scattered surface-atmosphere interactions
From: http://www.geog.ucl.ac.uk/~mdisney/phd.bak/final_version/final_pdf/chapter2a.pdf
R1
target
R2
target
R3
target
R4
target
UCL DEPARTMENT OF GEOGRAPHY
Interactions with the atmosphere: refraction
21
• Caused by atmosphere at different T having different density, hence refraction• path of radiation alters moving from medium of one density to
another (different velocity)• index of refraction (n) is ratio of speed of light in a vacuum (c)
to speed cn in another medium (e.g. Air) i.e. n = c/cn
• note that n always >= 1 i.e. cn <= c• Examples
• nair = 1.0002926• nwater = 1.33
UCL DEPARTMENT OF GEOGRAPHY
Refraction: Snell’s Law
22
• Refraction described by Snell’s Law• For given freq. f, n1 sin 1 = n2 sin 2 • where 1 and 2 are the angles from the
normal of the incident and refracted waves respectively
• (non-turbulent) atmosphere can be considered as layers of gases, each with a different density (hence n)
• Displacement of path - BUT knowing Snell’s Law can be removed
After: Jensen, J. (2000) Remote sensing of the environment: an Earth Resources Perspective.
n1
n3
n2
Optically less dense
Optically more dense
Optically less dense
Incident radiation
2
3
1
Path affected by atmosphere
Path unaffected by atmosphere
UCL DEPARTMENT OF GEOGRAPHY
Interactions with the atmosphere: scattering
23
• Caused by presence of particles (soot, salt, etc.) and/or large gas molecules present in the atmosphere
• Interact with EMR anc cause to be redirected from original path.
• Scattering amount depends on:• of radiation• abundance of particles or gases• distance the radiation travels through the
atmosphere (path length)
After: http://www.ccrs.nrcan.gc.ca/ccrs/learn/tutorials/fundam/chapter1/chapter1_4_e.html
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric scattering 1: Rayleigh
24
• Particle size << of radiation• e.g. very fine soot and dust or N2, O2
molecules• Rayleigh scattering dominates shorter
and in upper atmos.• i.e. Longer scattered less (visible red scattered
less than blue )• Hence during day, visible blue tend to dominate
(shorter path length)• Longer path length at sunrise/sunset so
proportionally more visible blue scattered out of path so sky tends to look more red
• Even more so if dust in upper atmosphere• http://www.spc.noaa.gov/publications/corfidi/sunset/• http://www.nws.noaa.gov/om/educ/activit/bluesky.htm
After: http://www.ccrs.nrcan.gc.ca/ccrs/learn/tutorials/fundam/chapter1/chapter1_4_e.html
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric scattering 1: Rayleigh
25From http://hyperphysics.phy-astr.gsu.edu/hbase/atmos/blusky.html
• So, scattering -4 so scattering of blue light (400nm) > scattering of red light (700nm) by (700/400)4 or ~ 9.4
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric scattering 2: Mie
26
• Particle size of radiation• e.g. dust, pollen, smoke and water vapour • Affects longer than Rayleigh, BUT weak dependence on • Mostly in the lower portions of the atmosphere
• larger particles are more abundant• dominates when cloud conditions are overcast
• i.e. large amount of water vapour (mist, cloud, fog) results in almost totally diffuse illumination
After: http://www.ccrs.nrcan.gc.ca/ccrs/learn/tutorials/fundam/chapter1/chapter1_4_e.html
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric scattering 3: Non-selective
27
• Particle size >> of radiation• e.g. Water droplets and larger dust
particles, • All affected about equally (hence
name!)• Hence results in fog, mist, clouds
etc. appearing white• white = equal scattering of red,
green and blue s
After: http://www.ccrs.nrcan.gc.ca/ccrs/learn/tutorials/fundam/chapter1/chapter1_4_e.html
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric absorption
28
• Other major interaction with signal• Gaseous molecules in atmosphere can
absorb photons at various • depends on vibrational modes of molecules• Very dependent on
• Main components are:• CO2, water vapour and ozone (O3)• Also CH4 ....• O3 absorbs shorter i.e. protects us from UV
radiation
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric absorption
29
• CO2 as a “greenhouse” gas• strong absorber in longer (thermal) part of EM
spectrum• i.e. 10-12m where Earth radiates• Remember peak of Planck function for T = 300K• So shortwave solar energy (UV, vis, SW and NIR)
is absorbed at surface and re-radiates in thermal• CO2 absorbs re-radiated energy and keeps warm• $64M question!
• Does increasing CO2 increasing T??• Anthropogenic global warming??• Aside....
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric CO2 trends
30
• Keeling et al.• Annual variation + trend• Smoking gun for anthropogenic
change, or natural variation??
• Antarctic ice core records
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric “windows”
31
• As a result of strong dependence of absorption• Some totally unsuitable for remote sensing as most
radiation absorbed
Atmospheric windows
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric “windows”
• If you want to look at surface– Look in atmospheric windows where transmissions high
• If you want to look at atmosphere however....pick gaps• Very important when selecting instrument channels
– Note atmosphere nearly transparent in wave i.e. can see through clouds!– V. Important consideration....
32
UCL DEPARTMENT OF GEOGRAPHY
Atmospheric “windows”
• Vivisble + NIR part of the spectrum– windows, roughly: 400-750, 800-1000, 1150-1300, 1500-1600, 2100-2250nm
33
UCL DEPARTMENT OF GEOGRAPHY
Summary• Measured signal is a function of target reflectance
– plus atmospheric component (scattering, absorption)– Need to choose appropriate regions (atmospheric windows)
• μ-wave region largely transparent i.e. can see through clouds in this region• one of THE major advantages of μ-wave remote sensing
• Top-of-atmosphere (TOA) signal is NOT target signal • To isolate target signal need to...
– Remove/correct for effects of atmosphere– A major part component of RS pre-processing chain
• Atmospheric models, ground observations, multiple views of surface through different path lengths and/or combinations of above
34
UCL DEPARTMENT OF GEOGRAPHY
Summary• Generally, solar radiation reaching the surface composed of
– <= 75% direct and >=25 % diffuse• attentuation even in clearest possible conditions
– minimum loss of 25% due to molecular scattering and absorption about equally
– Normally, aerosols responsible for significant increase in attenuation over 25%
– HENCE ratio of diffuse to total also changes– AND spectral composition changes
35
UCL DEPARTMENT OF GEOGRAPHY
Reflectance
36
• When EMR hits target (surface)• Range of surface reflectance behaviour
• perfect specular (mirror-like) - incidence angle = exitance angle• perfectly diffuse (Lambertian) - same reflectance in all directions
independent of illumination angle)
From http://www.ccrs.nrcan.gc.ca/ccrs/learn/tutorials/fundam/chapter1/chapter1_5_e.html
Natural surfaces somewhere in
between
UCL DEPARTMENT OF GEOGRAPHY
Surface energy budget
37
• Total amount of radiant flux per wavelength incident on surface, () Wm-1 is summation of:• reflected r, transmitted t, and absorbed, a
• i.e. () = r + t + a
• So need to know about surface reflectance, transmittance and absorptance
• Measured RS signal is combination of all 3 components
After: Jensen, J. (2000) Remote sensing of the environment: an Earth Resources Perspective.
UCL DEPARTMENT OF GEOGRAPHY
Reflectance: angular distribution
38
• Real surfaces usually display some degree of reflectance ANISOTROPY• Lambertian surface is
isotropic by definition• Most surfaces have some
level of anisotropy
From: http://www.geog.ucl.ac.uk/~mdisney/phd.bak/final_version/final_pdf/chapter2a.pdf
Figure 2.1 Four examples of surface reflectance: (a) Lambertian reflectance (b) non-Lambertian (directional) reflectance (c) specular (mirror-like) reflectance (d)
retro-reflection peak (hotspot).
(a) (b)
(c) (d)
UCL DEPARTMENT OF GEOGRAPHY
Directional reflectance: BRDF
39
• Reflectance of most real surfaces is a function of not only λ, but viewing and illumination angles
• Described by the Bi-Directional Reflectance Distribution Function (BRDF)
• BRDF of area A defined as: ratio of incremental radiance, dLe, leaving surface through an infinitesimal solid angle in direction (v, v), to incremental irradiance, dEi, from illumination direction ’(i, i) i.e.
After: Jensen, J. (2000) Remote sensing of the environment: an Earth Resources Perspective.
1
)(),()',( sr
dEdLBRDF
i
e
Ω'Ω'ΩΩΩ
• is viewing vector (v, v) are view zenith and azimuth angles; ’ is illum. vector (i, i) are illum. zenith and azimuth angles
• So in sun-sensor example, is position of sensor and ’ is position of sun
UCL DEPARTMENT OF GEOGRAPHY
Directional reflectance: BRDF
40
• Note that BRDF defined over infinitesimally small solid angles , ’ and interval, so cannot measure directly• In practice measure over some finite angle and and assume valid
From: http://www.geog.ucl.ac.uk/~mdisney/phd.bak/final_version/final_pdf/chapter2a.pdf
surface area Asurface tangent vector
i2-v
vi
incident solid angle
incident diffuse
radiation
direct irradiance (Ei) vector
exitant solid angle
viewer
Configuration of viewing and illumination vectors in the viewing hemisphere, with respect to an element of surface area, A.
UCL DEPARTMENT OF GEOGRAPHY
Directional reflectance: BRDF
41
• Spectral behaviour depends on illuminated/viewed amounts of material• Change view/illum. angles, change these proportions so change reflectance
• Information contained in angular signal related to size, shape and distribution of objects on surface (structure of surface)
• Typically CANNOT assume surfaces are Lambertian (isotropic)
From: http://www.geog.ucl.ac.uk/~mdisney/phd.bak/final_version/final_pdf/chapter2a.pdf
Modelled barley reflectance, v from –50o to 0o (left to right, top to bottom).
UCL DEPARTMENT OF GEOGRAPHY
Directional Information
42
UCL DEPARTMENT OF GEOGRAPHY
Directional Information
43
UCL DEPARTMENT OF GEOGRAPHY
Features of BRDF• Bowl shape
– increased scattering due to increased path length through canopy
44
UCL DEPARTMENT OF GEOGRAPHY
Features of BRDF• Bowl shape
– increased scattering due to increased path length through canopy
45
UCL DEPARTMENT OF GEOGRAPHY
46
UCL DEPARTMENT OF GEOGRAPHY
Features of BRDF• Hot Spot
– mainly shadowing minimum
– so reflectance higher
47
UCL DEPARTMENT OF GEOGRAPHY
The “hotspot”
48See http://www.ncaveo.ac.uk/test_sites/harwood_forest/
UCL DEPARTMENT OF GEOGRAPHY
49
UCL DEPARTMENT OF GEOGRAPHY
Directional reflectance: BRDF
50
• Good explanation of BRDF:• http://geography.bu.edu/brdf/brdfexpl.html
UCL DEPARTMENT OF GEOGRAPHY
51
• Hotspot effect from MODIS image over Brazil
UCL DEPARTMENT OF GEOGRAPHY
Measuring BRDF via RS
52
• Need multi-angle observations. Can do three ways:• multiple cameras on same platform (e.g. MISR, POLDER,
POLDER 2). BUT quite complex technically.• Broad swath with large overlap so multiple orbits build up
multiple view angles e.g. MODIS, SPOT-VGT, AVHRR. BUT surface can change from day to day.
• Pointing capability e.g. CHRIS-PROBA, SPOT-HRV. BUT again technically difficult
UCL DEPARTMENT OF GEOGRAPHY
Albedo
53
• Total irradiant energy (both direct and diffuse) reflected in all directions from the surface i.e. ratio of total outgoing to total incoming• Defines lower boundary condition of surface energy budget hence v. imp. for
climate studies - determines how much incident solar radiation is absorbed
• Albedo is BRDF integrated over whole viewing/illumination hemisphere• Define directional hemispherical refl (DHR) - reflectance integrated over whole
viewing hemisphere resulting from directional illumination• and bi-hemispherical reflectance (BHR) - integral of DHR with respect to
hemispherical (diffuse) illumination
2,1 ΩΩΩ ;Ω dBRDF2DHR =
222
,12;2 ΩΩΩΩΩΩ ddBRDFdBHR =
UCL DEPARTMENT OF GEOGRAPHY
Albedo
54
SW
dp
• Actual albedo lies somewhere between DHR and BHR• Broadband albedo, , can be approximated as
• where p() is proportion of solar irradiance at ; and () is spectral albedo• so p() is function of direct and diffuse components of solar radiation and so is
dependent on atmospheric state• Hence albedo NOT intrinsic surface property (although BRDF is)
UCL DEPARTMENT OF GEOGRAPHY
55
Typical albedo values
UCL DEPARTMENT OF GEOGRAPHY
Surface spectral information
56
• Causes of spectral variation in reflectance?• (bio)chemical & structural properties • e.g. In vegetation, phytoplankton: chlorophyll concentration • soil - minerals/ water/ organic matter
• Can consider spectral properties as continuous • e.g. mapping leaf area index or canopy cover
• or discrete variable • e.g. spectrum representative of cover type (classification)
UCL DEPARTMENT OF GEOGRAPHY
Surface spectral information: vegetation
57vegetation
UCL DEPARTMENT OF GEOGRAPHY
Surface spectral information: vegetation
58vegetation
UCL DEPARTMENT OF GEOGRAPHY
Surface spectral information: soil
59soil
UCL DEPARTMENT OF GEOGRAPHY
60
Surface spectral information: canopy
UCL DEPARTMENT OF GEOGRAPHY
Summary
61
• Last week• Introduction to EM radiation, the EM spectrum, properties of wave /
particle model of EMR• Blackbody radiation, Stefan-Boltmann Law, Wien’s Law and Planck
function• This week
• radiation geometry • interaction of EMR with atmosphere
• atmospheric windows
• interaction of EMR with surface (BRDF, albedo)• angular and spectral reflectance properties
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