Syllabus & Introduction

Faculty of Applied Engineering and Urban Planning

Civil Engineering Department

Lecture - Week 1

2nd Semester 2008/2009

Photo

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Lecturer Information

Eng. Maha A. Muhaisen

MSc. Infrastructure Engineering

Office: BK210

Tel.: Ext. 1127

O. Hours: Will be provided later

Course Outline

•Introduction

•Concepts and Foundations of Remote Sensing

•Elements of Photographic Systems

•Basic Photographic Measurements and Mapping

•Introduction to Airphoto Interpretation

Lillesand, TM, Kiefer, RW & Chipman, JW

Remote sensing and image interpretation,

5th Edition

2004

Text Book

Activities

Lectures

• Theory and Principles

• Examples

• Group Work and Discussion

• Quizzes

Grade Policy

Mid-term Exam 30%

Final Exam 40%

Assignments, Quizzes 30%

100%

IntroductionIntroduction

Definitions:

Remote sensing: the identification and study of objects from a remote distance using reflected or emitted electromagnetic energy over different portions of the electromagnetic spectrum.

Photogrammetry: the art or science of obtaining reliable quantitative information from aerial photographs.

What is Remote Sensing (RS)?

Formal and comprehensive definitionFormal and comprehensive definition “The acquisition and measurement of data/information

on some property(ies) of a phenomenon, object, or material by a recording device not in physical, intimate contact with the feature(s) under surveillance; techniques involve amassing knowledge pertinent to environments by measuring force fields, electromagnetic radiation, or acoustic energy employing cameras, radiometers and scanners, lasers, radio frequency receivers, radar systems, sonar, thermal devices, seismographs, magnetometers, gravimeters, and other instruments. ”

What is Remote Sensing (RS)?

Remote Sensing involves gathering data and information about the physical "world" by detecting and measuring radiation, particles, and fields associated with objects located beyond the immediate vicinity of the sensor device(s).

What is Remote Sensing (RS)?

Remote Sensing is a technology for sampling electromagnetic radiation to acquire and interpret non-immediate geospatial data from which to extract information about features, objects, and classes on the Earth's land surface, oceans, and atmosphere (and, where applicable, on the exteriors of other bodies in the solar system, or, in the broadest framework, celestial bodies such as stars and galaxies).

What is Remote Photogrammetry

Photogrammetry

”The science or art of obtaining reliable measurements by means of photographs.”

”Photogrammetry is the art, science, and technology of obtaining reliable information about physical objects and the environment through the processes of recording, measuring, and interpreting photographic images and patterns of electromagnetic radiant energy and other

phenomena.” (ASPRS, 1980)

Definitions (2)Analog PhotogrammetryAnalog PhotogrammetryUsing optical, mechanical and electronical components,

and where the images are hardcopies. Re-creates a 3D model for measurements in 3D space.

Analytical PhotogrammetryAnalytical PhotogrammetryThe 3D modelling is mathematical (not re-created) and

measurements are made in the 2D images.Digital PhotogrammetryDigital PhotogrammetryAnalytical solutions applied in digital images. Can also

incorporate computer vision and digital image processing techniques.

or Softcopy Photogrammetry”Softcopy” refers to the display of a digital image, as

opposed to a ”hardcopy” (a physical, tangible photo).

What is Photogrammetry

Photograph ImageA scene which was detected as well as recorded on film.

A scene which was detected

electronically.

Chemical reactions on a light sensitive film detects the intensity of the incoming energy.

Generate an electrical signal

proportional to the incoming

energy.

Simple, cheap, well known,

high degree of spatial detail.

Can sense in many wavelengths,

data can be easily converted

into digital form for automated

processing.

Only sense in the wavelength of

0.3 – 0.9 μm, manual interpretation.

Complex,

expensive sensors

Relationships of the Mapping Sciences as they relate to Mathematics and Logic, and the Physical, Biological, and Social Sciences

Photogrammetry

A Brief History of Photogrammetry & RS

1851: Only a decade after the invention of the Daguerrotypie by Daguerre and Niepce, the french officer Aime Laussedat develops the first photogrammetrical devices and methods. He is seen as the initiator of photogrammetry.

1858: The German architect A. Meydenbauer develops photogrammetrical techniques for the documentation of buildings and installs the first photogrammetric institute in 1885 (Royal Prussian Photogrammetric Institute).

1866: The Viennese physicist Ernst Mach publishes the idea to use the stereoscope to estimate volumetric measures.

1885: The ancient ruins of Persepolis were the first archaeological object recorded photogrammetrically.

1889: The first German manual of photogrammetry was published by C. Koppe. 1896: Eduard Gaston and Daniel Deville present the first stereoscopical

instrument for vectorized mapping. 1897/98: Theodor Scheimpflug invents the double projection. 1901: Pulfrich creates the first Stereokomparator and revolutionates the

mapping from stereopairs. 1903: Theodor Scheimpflug invents the Perspektograph, an instrument for

optical rectification.

1910: The ISP (International Society for Photogrammetry), now ISPRS, was founded by E. Dolezal in Austria.

1911: The Austrian Th. Scheimpflug finds a way to create rectified photographs. He is considered as the initiator of aerial photogrammetry, since he was the first succeeding to apply the photogrammetrical principles to aerial photographs.

1913: The first congress of the ISP was held in Vienna. until 1945: development and improvment of measuring (metric) cameras

and analogue plotters. 1964: First architectural tests with the new stereometric camera-system,

which had been invented by Carl Zeiss, Oberkochen and Hans Foramitti, Vienna.

1964: Charte de Venise. 1968: First international Symposium for photogrammetrical applications

to historical monuments was held in Paris - Saint Mand.

A Brief History of Photogrammetry & RS

1970: Constitution of CIPA (Comit International de la Photogrammetrie Architecturale) as one of the international specialized committees of ICOMOS (International Council on Monuments and Sites) in cooperation with ISPRS. The two main activists were Maurice Carbonnell, France, and Hans Foramitti, Austria.

1970ies: The analytical plotters, which were first used by U. Helava in 1957, revolutionate photogrammetry. They allow to apply more complex methods: aerotriangulation, bundle-adjustment, the use of amateur cameras etc.

1980ies: Due to improvements in computer hardware and software, digital photogrammetry is gaining more and more importance.

1996: 83 years after its first conference, the ISPRS comes back to Vienna, the town, where it was founded.

1996: The film starring Brad Pitt, Fight Club is an excellent example of the use of photogrammetry in film where it is used to combine live action with computer generated imagery in movie post-production.

2005: Topcon PI-3000 Image Station is launched.

A Brief History of Photogrammetry & RS

Short History (1)

Analogue Photogrammetry

(Pure optical-mechanical way, 1911-1945): the large, complicated and expensive instruments could only be handled with a lot of experience photogrammetric operators.

Steroscopic Transfer Instruments-- Stereoplotters that Use Diapositives

Short History (2)

Analytical Photogrammetry (1957-1980): reconstruct the orientation no more analogue but algorithmic. The equipment became significantly smaller, cheaper and easier to handle,… with servo motors to provide the ability to position the photos directly by the computer.

Automated (Analytical) Stereoplotter

Short History (3)

Digital Photogrammetry (1980-now): use digital

photos and do the work directly with the computer.

Photogrammetry

Aerial Photmgrammetry Terrestial Photogrammetry

Chapter (1)Concept and Fundamentals of Remote

Sensing

Fundamental Principles ofElectromagnetic Radiation

Wave Theoryc = ν λ where: c = speed of light = 3 x 108 m s-1ν = frequency (s-1, cycles/s, or Hz)λ = wavelength (m)

Finding Frequency from Wavelength

Given: λ = 0.55 μm [green light]Find: νSolution: c = νλν = c / λν = (3 x 108 m s-1) / (0.55 x 10-6 m)ν = 5.45 x 1014 s-1

Finding Wavelength from requency

Given: ν = 6000 MHz = 6000 x 106 s-1Find: λSolution: c = νλλ = c / νλ = (3 x 108 m s-1) / (6 x 109 s-1)λ = 0.05 m = 5 cm[microwave, or radar wavelength]

Particle Theory

Q = hνwhere Q = energy of a quantum, Joules (J)h = Planck’s constant, 6.626 x 10-34 J sν = frequency (s-1)

Relating Wave and Particle Theory

Q = hν and c = νλ ;ν = c / λ

therefore, Q = hc / λ The longer the wavelength, the lower the

energy content.

The Electromagnetic Spectrum

near-IR = 0.7 – 1.3 μm earth during daytime:mid-IR = 1.3 – 3.0 μm more reflected sunlight

thermal IR = 3.0 – 14 μm more emitted energy

Figure 1.3 The electromagnetic spectrum.

Visible Light

Nominal Regions of the Spectrum

Ultraviolet: 0.3 - 0.4 μm Visible: 0.4 - 0.7 μm

Blue: 0.4 - 0.5 μm Green: 0.5 - 0.6 μm Red: 0.6 - 0.7 μm

Near Infrared: 0.7 - 1.3 μm Photographic Infrared: 0.7 - 0.9 μm

Mid Infrared: 1.3 - 3 μm Thermal Infrared: 3 - 14 μm Microwave (Radar): 1 mm - 1 m

Unit Prefix Notation

Multiplier Prefix Example103 kilo (k) kilometer10-3 milli (m) millimeter10-6 micro (μ) micrometer10-9 nano (n) nanometerSee also inside back cover of textbookNote: one “micron” = one “micrometer”

Sources ofElectromagnetic Radiation

Figure 1.4 Spectral distribution of energy radiated from blackbodies of various temperatures.

The Stefan-Boltzmann Law

M = σT4Where: M = total radiant exitance, or emitted

energy (W m-2)

σ = Stefan-Boltzmann constant (5.6697 x 10-8 W m-2 K-4)

T = temperature (K)

Note: All temperatures must be expressed in degrees Kelvin (“kelvins”) K = °C + 273.15

Wien’s Displacement Law

λM = A / T

Where: λM = wavelength of maximum radiant exitance (μm)

A = constant (2898 μm K)T= temperature (K)Note: All temperatures must be

expressed in degrees Kelvin (“kelvins”)K = °C + 273.15

Figure 1.4 Spectral distribution of energy radiated from blackbodies of various temperatures.

Atmospheric Effects onElectromagnetic Radiation

Figure 1.1 Electromagnetic remote sensing of earth resources.