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Satellite remote sensing presents an amazing opportunity to inform biodiversity conservation by inexpensively gathering repeated monitoring information for vast areas of the Earth. However, these observations first need processing and interpretation if they are to inform conservation action. Through a series of case studies, this book presents detailed examples of the application of satellite remote sensing, covering both aquatic and terrestrial ecosystems, to conservation. The authors describe how collaboration between the remote sensing and conservation communities makes satellite data functional for operational conservation, and provide concrete examples of the lessons learned in addition to the scientific details. The editors, one at NASA and the other at a conservation NGO, have brought together leading researchers in conservation remote sensing to share their experiences from project development through to application, and emphasise the human side of these projects.
At the convergence of the land and sea, coastal environments are some of the most dynamic and populated places on Earth. This book explains how the many varied forms of spatial analysis, including mapping, monitoring and modelling, can be applied to a range of coastal environments such as estuaries, mangroves, seagrass beds and coral reefs. Presenting empirical geographical approaches to modelling, which draw on recent developments in remote sensing technology, geographical information science and spatial statistics, it provides the analytical tools to map, monitor and explain or predict coastal features. With detailed case studies and accompanying online practical exercises, it is an ideal resource for undergraduate courses in spatial science. Taking a broad view of spatial analysis and covering basic and advanced analytical areas such as spatial data and geostatistics, it is also a useful reference for ecologists, geomorphologists, geographers and modellers interested in understanding coastal environments.
Introducing planetary photometry as a quantitative remote sensing tool, this handbook demonstrates how reflected light can be measured and used to investigate the physical properties of bodies in our Solar System. The author explains how data gathered from telescopes and spacecraft are processed and used to infer properties such as the size, shape, albedo, and composition of celestial objects including planets, moons, asteroids, and comets. Beginning with an overview of the history and background theory of photometry, later chapters delve into the physical principles behind commonly used photometric models and the mechanics of observation, data reduction, and analysis. Real-world examples, problems, and case studies are included, all at an introductory level suitable for new graduate students, planetary scientists, amateur astronomers and researchers looking for an overview of this field.
Begins with an elementary overview of our physical understanding of light, including polarization, followed by its interaction with matter - scattering, reflection, and refraction. The interaction of light with individual particles is of fundamental importance in photometric models, and a brief description of this interaction is included. Modern photometric models also incorporate the behavior of ensembles of scatterers using the principles of radiative transfer. These are described and used to show how the simplest scattering models can be derived from its first principles. Finally, the opposition surge and the effects of surface roughness on scattered light are described along with the methods used to account for these in modern photometric models.
An overview of the methods used to extract information about planetary objects from disk-integration (telescopic) observations. The primary relationship between planetary size, albedo, and absolute magnitude is derived. Complications in this relationship for comets and irregular asteroids are discussed, including the characterization of lightcurves. The planetary phase curve is of fundamental importance in disk-integrated work and its construction and use is described. Again, comets and asteroids have more complicated phase curves and these complications are described, along with the modern HG magnitude system for asteroids and its origin. The polarization properties of small bodies provide additional physical information, especially when cast into the form of a polarization phase curve, and the empirical relations that have been gleaned from extensive laboratory work are introduced, along with their application to asteroid and comet studies. Finally, a recent published application of these principles to the study of Mercury is examined.
Introduces the mechanical devices and methods necessary for modern photometry. Telescopes of different types and their optical properties are described, followed by an extensive discussion of the modern CCD camera. After describing how telescopes and CCDs are matched for optimal work, there is an overview of the reduction and calibration process, primarily for ground-based work. Spacecraft processing is covered in Chapter 7.
Introduces the major conventions and terms needed to understand planetary photometry. Included are the definitions and uses of the major coordinate systems, definitions of time scales and their use in planetary work, major terms used in planetary photometry - such as irradiance and radiance - and their interrelationships, the different types of magnitudes used by planentary sciences, the origin and overview of photometric systems such as the UBVRI system, and the standard stars and scales that tie these systems together.
An overview of the methods used to extract information about planetary objects from disk-resolved observations, dominately from the laboratory and spacecraft. Laboratoratory methods of photometric goniometers are described with examples. Next, the differences in observation and calibration between spacecraft and telescopic sensors are discussed. Spacecraft observations require enormously more ancillary information than ground-based which are often managed by the SPICE system - a database and analysis system developed by NASA and used by most modern missions. Finally, a variety of case studies are examined, including a laboratory test of the Hapke model, the reduction and analysis of MESSENGER MDIS data to construct global mosaics of Mercury, and the use of Clementine UVVis images to calibrate the reflectance of the Moon and study the lunar opposition surge and phase reddening.
An overview of the most common methods of describing the reflectance of planetary surfaces, including radiance factor, bidirectional reflectance function, albedo, etc., and the assorted variations on these themes. Each of these is described for disk-integrated and disk-resolved conditions. The scattering behavior of the most commonly used photometric models is derived or described, including Lambertian, Lommel-Seeliger, Minnaert, Hapke, and Lumme-Bowell models.
Defines the concept of planetary photometry and provides a broad overview of its history, including early theories of vision and light, the origin of the stellar magnitude scale, and the seminal work of Bouguer and Lambert in the development of the field. It concludes with early photometric work to define the brightness of objects in the solar system and its recent success in elucidating the state of the lunar regolith prior to landing there.