Chile is home to many traditions, foods, experiences and mysteries. But one of Chile’s greatest attractions is its view of the stars, from La Silla Observatory’s Very Large Telescope (owned by
European Southern Observatory.)
GENERAL INFORMATION
The Very Large Telescope at La Silla Observatory is actually more than just one telescope. Four
“Unit Telescopes” work together to provide extremely high-resolution images of the cosmos.
The scopes have large lenses for gathering light, at 8.2 meters across. These scopes have been
“...named Antu, Kueyen, Melipal and Yepun for the Sun, the Moon, the Southern Cross, and
Venus in the language of the Mapuche people.” (Gregersen) Working with these scopes are four smaller “Auxiliary Scopes” with diameters of 1.8 meters. These eight
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(Gregersen)
TECHNICAL SPECIFICS
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The Very Large Telescope is more than just lenses and mirrors. In order for its four 8.2 meter lenses to gather enough light, the environment has to be perfect. The telescope is located at an altitude of 2635 meters, providing excellent views of space due to the lessened atmospheric interference. (VLT) To make sure that the telescope produces the most accurate images, the mirrors are thoroughly cleaned every 18 months. This cleaning involves removing the aluminum from the mirrors and recoating the mirrors. The amount of aluminum used is about 12 grams
(less than a soda can), and when spread over the mirrors produces a layer of the material 80 nanometers thick. (European Southern Observatory) The lenses of the scope have to be near- perfect in every way. Even the slightest bump in the glass can cause warped images to appear, which is why the lenses were constructed with such skill that if they were scaled to the size of the Earth, the largest imperfection would be no larger than a pebble. (
COST OF ASSEMBLY AND REGULAR
Example #1: This movie of C/1997 T1 (Utsunomiya) was obtained by Tim Puckett on 1997 October 7. It was obtained with a 60-cm reflector and shows the comet's motion over a period of about 75 minutes. The field of view is 9 x 9 arc minutes or about one-third the diameter of the full moon.
Ground-based observations also have played a major role in recent advances in scientific understanding of nebulae. The emission of gas in the radio and submillimetre wavelength ranges provides crucial information regarding physical conditions and molecular composition. Large radio telescope array's, in which several individual telescopes function collectively as a single enormous instrument, give spatial resolutions in the radio regime far superior to any yet achieved by optical means.
The first Fresnel Lens date back to 1822 when a French physicist by the name of Augustin Fresnel wanted to make our bodies of water safer for sailors throughout the world. The Fresnel Lens originally were a type of compact lens created by Fresnel for lighthouses. A Fresnel lens replaces the curved surface of a conventional lens with a series of concentric grooves, molded into the surface of a thin, lightweight plastic sheet (“Fresnel Lenses”). The Fresnel Lens were beneficial for lighthouses because they have the ability to capture more oblique light which allowed lighthouses that used them to be seen from greater distances. Fresnel’s lens resembles a giant beehive with a complex system of multi-faceted glass prisms mounted in a brass framework.
Though this was the original plan, the telescope ended up returning images that were drastically lower quality than expected. This
I will be talking about how images in a convex lens in a magnifying glass are affected by focal length. Concave lenses always produce virtual images because refracted rays do not intersecct. Images being reflected might change size depending on the material it is being reflected on. In some reflections it is common for an object to be reflected upside down because f the effect the material gives.
Before you can observe with a Newtonian reflector telescope, you need to align or collimate its optical parts. The goal of collimation is to insure that both the primary and secondary mirrors as well as the eyepiece are correctly lined up to give clear, sharp views.
Farsighted people need a lens system that will converge the rays so that as it enters the cornea, it will refract light rays onto the fovea.
Damrosch, David, and David Pike. The Longman Anthology of World Literature. The Ancient World. Volume A. Second Edition. New York: Pearson/Longman, 2009. Pgs. .656-691. Print.
* A telescope typically requires the collecting area to be aligned within 1/10 of the wavelength it is designed for. Because it is almost impossible to get all the parts of a sufficiently large telescope aligned to within 80 nm, radio telescopes *can* be built much larger.
And they can perhaps to help us to reflect what we really see when we interpret aerophotos and lidar imagery.
First, I am going to talk about how the lens works to allow us to see objects at different distances clearly. If you refer to figure 3, you will see the ciliary zonules attached to the lens via
Most microscopes consist of twelve parts; the eyepiece lens, the tube, the arm, the base, the illuminator, the mirror, the stage, the turret, the objective lenses, the rack stop, the condenser lens and the iris. Every part of a microscope has a very important responsibility in order for people to see smaller things clearly. For example the eyepiece lens is what you look through to observe. An illuminator is a one hundred and ten volt light source that i...
Refracting telescopes are designed with lense at the front of the telescope the biggest so when the light rays enter, the real image is formed closer to the eyepiece, magnifying the image more. The equation to calculate the magnification of a telescope it M = Fo/Fe (Magnification = Focal length of object/Focal length of eyepiece).
Bisecting the fixed mirror and the movable mirror is a beamsplitter, where a collimated beam of radiation which could be infrared light emitted by an external source (Globar, metal wire, Nernst bar ), can be partially reflected to the fixed mirror (at point F for the median ray) and partially transmitted to the movable mirror (at point M). When the beams return to the
At the heart of the Atacama desert , here you are in the charming village of San Pedro. Here, the beauty of the skies will put your eyes full: the Milky Way and a myriad of stars are offered to you in the vastness of the natural spaces of Chile. Guided by an experienced astronomer, you will become unbeatable on the Great Bear, the Orion Belt and