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This article discusses research which detailed the algorithm used to build a three-dimensional (3-D) model of the above-water portion of icebergs using surface imaging. Topics discussed include the methodology involving algorithm for extrusion and intersection, algorithm for extrusion and intersection and data processing to produce 3-D models of icebergs.

Emission patterns from molecules at interfaces encode many details about their local environment and their axial position, along the microscope's optical axis. We introduce an advanced approach that synergizes back focal plane (BFP) imaging with innovative 'smart' surfaces make surface imaging more qualitative, more reliable, and more robust. Our method is particularly focused on accurately measuring the refractive index (RI) of transparent thin films and their imperfections close to the interfaces. Our technique utilizes a 'smart' surface, which features a uniform fluorescent thin film of about 4 nm thickness together with back-focal plane (BFP) imaging. We manage to detect bubbles or other imperfection in 100 nm thin film of polymer with RI of 1.34. [ABSTRACT FROM AUTHOR]

Current planet hunting methods using the radial velocity method are limited to observing middleaged main-sequence stars where the signatures of stellar activity are much less than on young stars that have just arrived on the main-sequence. In this work we apply our knowledge from the surface imaging of these young stars to place realistic limitations on the possibility of detecting orbiting planets. In general we find that the magnitude of the stellar jitter is directly proportional to the stellar vsini. For G and K dwarfs, we find that it is possible, for models with high stellar activity and low stellar vsini, to be able to detect a 1 MJupiter mass planet within 50 epochs of observations and for the M dwarfs it is possible to detect a habitable zone Earth-like planet in 10s of observational epochs. [ABSTRACT FROM AUTHOR]