For high-density fiber optic distribution in communications central offices and high-capacity datacenters, Telect's Advanced Distribution Frame (ADF) provides the ultimate in circuit density, management, protection and access. This video details the components that comprise the ADF, providing a basic outline of how a system goes together, the key features that make the ADF an industry-leading platform for optical distribution, and the advantages that the ADF provides in a multitude of applications. The scalable ADF helps users effectively manage fiber optic traffic, as well as maintain a close handle on capital expenditures. A full-frame solution can handle up to 2,304 individual fiber optic circuits, with cable routing, protection and access features that make each individual circuit highly manageable. Learn more at www.telect.com.

Author: Telect1
Keywords: Telect ADF ODF Fiberoptic Optical Patching Central Office Datacenter Splicing Distribution Fiber
Added: December 11, 2008

First glance says it all: The PowerShot E1 and you are going to get along just great. After all, you love color that dares to surprise. And nothing delights you more than style that makes you smile. The PowerShot E1 goes everyplace you go...to parties, to the beach, far away and to fabulous times right around the corner. Every moment matters when you've got a camera that couldn't be more clever. Or cooler.

Author: TigerDirectBlog
Keywords: Canon PowerShot E1 Digital Camera bauer computertv tigertv compusa
Added: November 20, 2008

A quick tutorial on the basics of three common types of optical filters. Made to support the course "Engineering Optics" at Oklahoma State University.

Author: kridnix
Keywords: optical filters engineering physical science interference neutal density color glass
Added: October 27, 2008

FEATURES TOP General Premium 80 mm refractor Celestron's Starbright® XLT high transmission coatings Celestron combines a Fluorite based, low dispersion glass with high density crown glass for virtually color-free images across the visible spectrum 2" Crayford style focuser minimizes image shift Rotatable focuser for easy framing of objects for photography Extendable lens shade reduces glare and protects lens from moisture Built-in sighting scope to help accurately locate objects Integrated dovetail compatible with Celestron Computerized "GoTo" Aluminum case for convenient storage and protection

Author: skyspy2008
Keywords: FEATURES TOP General Premium 80 mm refractor Celestron's Starbright® XLT high transmission coatings Celestron
Added: September 14, 2008

The Cosmic Origins Spectrograph (COS) is designed to study the large-scale structure of the universe and how galaxies, stars and planets formed and evolved. It will help determine how elements needed for life such as carbon and iron first formed and how their abundances have increased over the lifetime of the universe. As a spectrograph, COS wont capture the majestic visual images that Hubble is known for, but rather it will perform spectroscopy, the science of breaking up light into its individual components. Any object that absorbs or emits light can be studied with a spectrograph to determine its temperature, density, chemical composition and velocity. A primary science objective for COS is to measure the structure and composition of the ordinary matter that is concentrated in what scientists call the cosmic web—long, narrow filaments of galaxies and intergalactic gas separated by huge voids. The cosmic web is shaped by the gravity of the mysterious, underlying cold dark matter, while ordinary matter serves as a luminous tracery of the filaments. COS will use scores of faint distant quasars as cosmic flashlights, whose beams of light have passed through the cosmic web. Absorption of this light by material in the web will reveal the characteristic spectral fingerprints of that material. This will allow Hubble observers to deduce its composition and its specific location in space. COS has two channels, the Far Ultraviolet (FUV) channel covering wavelengths from 115 to 177 nm, and the Near Ultraviolet (NUV) channel, covering 175-300 nm. Ultraviolet light, the type of radiation that causes sunburn, is more energetic than visible, optical light; and near UV refers to the part of the UV spectrum closer to the visible, just beyond the color violet. The light-sensing detectors of both channels are designed around thin micro-channel plates comprising thousands of tiny curved glass tubes, all aligned in the same direction. Simply described, incoming photons of light ultimately induce showers of electrons to be emitted from the walls of these tubes. The electron showers are accelerated, captured, and counted in electronic circuitry immediately behind the micro-channel plates. A key feature of COS—the one which makes it unique among Hubble spectrographs—is its maximized efficiency, or throughput. Each bounce of a light beam off an optical surface within an instrument takes some of the light away from the beam, reducing the throughput. This is a problem that is especially acute in the UV, and the COS FUV channel was designed specifically to minimize the number of light bounces. The incoming FUV beam makes one bounce off a selectable light-dispersing grating, and goes directly to the detector. An additional advantage within COS is the very low level of scattered light produced by its light-dispersing gratings. If astronauts are able to complete the on-orbit repair of the Space Telescope Imaging Spectrograph (STIS) aboard Hubble, it will highly complement the COS. The all purpose STIS, installed in 1997 during Servicing Mission 2, suffered an electronics failure in 2004 and is currently in safe hold. By design, the COS does not duplicate all of STISs capabilities. Possessing more than 30 times the sensitivity of STIS for FUV observations of faint objects such as distant quasars, COS will enable key scientific programs which would not be possible using STIS. On the other hand, COS is best suited to observing point sources of light such as stars and quasars, while STIS has the unique ability to observe the spectrum of light across spatially extended objects such as galaxies and nebulae. Should STIS be repaired, the two spectrographs working in tandem will provide astronomers with a full set of spectroscopic tools for astrophysical research. COS will be installed in the instrument bay currently occupied by COSTAR, the set of corrector mirrors on deployable arms that provided corrected light beams to the first generation of Hubble instruments after SM1 in 1993. Astronauts will store the no longer needed COSTAR instrument aboard the shuttle for its return to Earth.

Author: BrunoTheQuestionable
Keywords: Hubble COS Instrument
Added: September 11, 2008