Cassegrain Telescopes
Cassegrain Telescopes - Related Videos
10:35
Bringing the Visible Universe into Focus with Robo-AO
0 Views •
Cited by 17 •
2013
Light from astronomical objects must travel through the earth's turbulent atmosphere before it can be imaged by ground-based telescopes. To enable direct imaging at maximum theoretical angular resolution, advanced techniques such as those employed by the Robo-AO adaptive-optics system must be used.
12:50
Continuous Instream Monitoring of Nutrients and Sediment in Agricultural Watersheds
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Cited by 3 •
2017
With the advancement of technology and the rise in end-user expectations, the need and use of higher temporal resolution data for pollutant load estimation has increased. This protocol describes a method for continuous in situ water quality monitoring to obtain higher temporal resolution data for informed water resource management decisions.
07:04
Physiological, Morphological and Neurochemical Characterization of Neurons Modulated by Movement
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2011
A technique is described to quantify the in vivo physiological response of mammalian neurons during movement and correlate the physiology of the neuron with neuronal morphology, neurochemical phenotype and synaptic microcircuitry.
10:41
Method to Measure Tone of Axial and Proximal Muscle
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Cited by 5 •
2011
We have developed a device (Twister) to study the regulation of tonic muscle activity during active postural maintenance. Twister measures torsional resistance and muscular responses in standing subjects during twisting of the body axis. The device can be flexibly configured to study various aspects of tonic control across the neck, trunk, and/or hips.
11:15
A Guide to Structured Illumination TIRF Microscopy at High Speed with Multiple Colors
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Cited by 114 •
2016
This article provides an in depth guide for the assembly and operation of a structured illumination microscope operating with total internal reflection fluorescence illumination (TIRF-SIM) to image dynamic biological processes with optical super-resolution in multiple colors.
FAQs
Mirror spacing controls how the reflected light travels between the primary and secondary mirrors before reaching the opening in the primary. A suitable arrangement produces a long effective focal length without requiring an equally long physical tube. In mathematical modeling, changing this spacing changes the ray path, focal-length relationship, and predicted image formation.
Conic sections provide mathematical descriptions of the mirror shapes used to control reflected light. Their geometry determines how incoming rays change direction and where those rays converge after reflection. Studying the relevant curves allows optical designers to relate mirror shape, focal length, and image position instead of treating the telescope as a purely empirical system.
Ray angles determine the direction of light after each reflection. Light first changes direction at the concave primary mirror and then again at the convex secondary, so the combined angles establish the final path toward the detector or eyepiece. Mathematical ray tracing uses these relationships to predict whether the optical arrangement forms the intended image.
A model can specify the geometry of both mirrors, the distance separating them, and the relevant focal lengths, then follow representative rays through successive reflections. Comparing the calculated ray paths with the intended image location reveals how the design forms an image. This approach supports analysis of optical layouts before constructing or adjusting an instrument.
Begin by describing the mirror geometries and assigning their focal-length parameters. Next, determine how representative rays reflect from the primary and secondary surfaces, while accounting for mirror spacing. Finally, evaluate where the redirected rays reach the opening and image-forming device. These steps connect geometric assumptions with a predicted optical outcome.
They are useful when an observer needs a long effective focal length in a compact optical instrument. The arrangement sends the converging light toward an eyepiece, camera, or detector through the primary mirror’s opening. This makes the design relevant to astronomical observation while also providing a concrete system for studying reflection and image formation.
Their operation provides a practical setting for applying conic sections, reflection geometry, ray angles, focal lengths, and mirror spacing. These mathematical quantities are not separate abstractions: together, they determine the light path and image location. Consequently, the telescope can support lessons, optical-design studies, and mathematical modeling of reflection systems.