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Listed here are software packages useful for conducting scientific research in astronomy, and for seeing, exploring, and learning about the data used in astronomy. Package Name Pro
A star tracker is an optical device that measures the positions of stars using photocells or a camera. [1] As the positions of many stars have been measured by astronomers to a high degree of accuracy, a star tracker on a satellite or spacecraft may be used to determine the orientation (or attitude) of the spacecraft with respect to the stars ...
The equipment used varies from webcams and basic security cameras to specialized video astronomy cameras. Recent growing interest in the video 'near-live' aspect of astronomy has brought about websites devoted purely to the practice [6] and forums for users of the equipment [7] [8] [9]
The Astronomical Image Processing System (AIPS) is a software package to support the reduction and analysis of data taken with radio telescopes. Developed predominantly for use with the then under-construction VLA, the generality inherent in its design allowed it to become the standard data-reduction package for most radio interferometers, including VLBI.
In the past, plate solving was done manually by accurately measuring photographic glass plates taken with an astrograph (astrographic camera) [2] [3] Currently, astrometric solving is exclusively done by software programs. The program extracts the star x,y positions from the celestial image, groups them in three-star triangles or four-star quads.
The Virtual Operation System (VOS) provides a portable interface for the application tasks. It is modeled after the Unix system functions, but with an API for the IRAF specific Subset Preprocessor language (SPP). The Host System Interface (HSI) is the kernel providing an interface between the host system and the functions of the VOS. It also ...
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In a camera or imaging system an object far away gets imaged onto the film or detector plane by the objective lens, and the far field diffraction pattern is observed at the detector. The resulting image is a convolution of the ideal image with the Airy diffraction pattern due to diffraction from the iris aperture or due to the finite size of ...