Objective Lens Lab Report

The telescope is an optical instrument designed to make distant objects appear nearer. It contains an arrangement of lenses or mirrors or both that gathers visible light, permitting direct observation or photographic recording of distant objects. (Lacki, B. C. 2011). With the use of telescopes we have been able to learn a lot more about the planets in our universe. It has helped us understand about some of the history of everything around us. Also it has been able to track asteroids and comets or any randomly flying objet in outer space that might become threatening to our planet.

Figures 1.6 and 1.7 illustrate how the position of the dots can be used to compute the eye's wavefront aberration. Figure 6 is a magnified view of a single lenslet shown in Fig. 3, with a portion

Meridian has been manufacturing fine telescopes for 80 years and has developed a well-earned reputation for quality craftsmanship. The company itself produces and sells two distinct lines of telescopes, which are produced in its 200,000 square feet facility. Furthermore, both lines have been developed to appeal to distinct target audiences who have an interest in the company’s products. The older line, for which there has been steady demand, consists of small professional telescopes that ultimately have laid the foundation for Meridian’s strong reputation. Following the success of

Measuring both telescopes to Galileo’s telescope and the Hubble Space Telescope, they are all remarkable with their individual functions and purposes. The Hubble Space Telescope is more high-technology than the other three and has made tons of findings from the outer aspect of the Earth. Though Galileo’s telescope was not as impressive compare to the modern ones, knowing the early times was limited but Galileo still has the idea and ability to make it was impressive and worth the

The telescope was not an invention made just to look up into the stars and see what you can find it actually helped make discoveries like Dark energy, how old the universe is and how the universe were different long ago. First, the

Scientists came up with a solution to correct the defect in which they came up with a replacement "contact" lens called COSTAR. The Corrective Optics Space Telescope Axial Replacement consisted of several minute mirrors that would intercept the beam of the flawed mirror and relay the corrected beam to the scientific instruments at the focus of the mirror.

As proposed in an article posted on amazing space.org, “The telescope, a basic reflector with a 94.5 in (2.4 meters) mirror.” While also having being a second mirror that the light bounces to to. Within that mirror, many instruments were compacted together that allowed for clear and visible views in infrared and ultraviolet light. It was different compared to any other ground based telescope whereas it allowed astronomers to observe and witness details that had never been seen before due to Earth being in the way for those other telescopes. The telescope revolves around the earth completely every ninety-seven minutes at the speed of five miles per second, allowing for many observations in space. The observations occur when light hits the main mirror and then bounces towards the second mirror in which the second one focuses the light. The telescope began to be created in 1977 and was originally supposed to launch during the year of 1985. Unfortunately an accident had occurred when a space shuttle challenger exploded and flights into space took a halt. It was finally launched on April 4th of 1990 once the halt had stopped. The improved observations had begun and the history of astronomy had changed. Unfortunately there were some minor setbacks that had to be dealt with. One setback was that the primary mirror was ground incorrectly in which the curve of it was too flat. It was off just

Focal Length is the calculation of an optical distance from where rays of light meet to form a sharp image of an object. The focal length of a lens is calculated when the lens is focused at infinity. The longer

The Subaru Telescope is located in Mauna Kea, Hawaii, and is an 8.2 metre optical-infrared telescope, operated by the National Astronomical Observatory of Japan (‘Subaru telescope’, n.d.). Situated in the summit of Mauna Kea, the telescope collects light using a mirror, and focuses the photons to create high resolution image. The mirrors in the telescope have a small error margin of 0.012 μm, which allows for the telescope to provide crisp images.

These telescopes are essentially titanic versions of the telescopes used in everyday stargazing. The most recognisable telescope is the Hubble Space Telescope. The Hubble Space Telescope has a number of features. One of them is its ability to see “...three different kinds of light: near-ultraviolet, visible and near-infrared.” (HubbleSite) It uses this ability to “study dark energy and dark matter, the formation of individual stars and the discovery of extremely remote galaxies previously beyond Hubble's vision.” (HubbleSite). Hubble has allowed us to “[Discover]...the age of the universe” just by taking photos with its many cameras. “An interesting fact: When hubble takes a picture of deep space, the naked eye perceives it as darkness. However, over a very long exposure, pictures are brought forth that show thousands upon thousands of galaxies and illustrate the enormity of the universe.” (My dad((no

Today’s lab we will be covering thin lenses both converging and diverging. With great regard to understand when forming an image there is always an object that the lens is using to create. Using both size and orientation of the image to find out the ray of light as it flows through and object. Furthermore, we will be using the thin lens equation to calculate the image distance and variables related to the lens in addition to the light diagram. Where f is the focal length of the lens, do is the object distance, and di is the image distance. With the focal length equation, we can calculate the image distance. Finally, we will be using our magnification equations to calculate the focal lengths for converging and diverging

The Thirty Meter Telescope (TMT) is being worked on to become the most advance and powerful optical telescope on Earth by a team of scientists, engineers and specialists. After long controversy, its planned location will be in Mauna Kea, Hawaii. The TMT is a reflecting telescope because it uses a mirrors over lenses. “TMT, with its 30-meter (nearly 100 foot) diameter mirror, will have nine times the light gathering power of today’s best telescopes (Gateway, 2010). TMT’s smaller parts, which are less than two meters across, can be created, handled and replaced a whole lot easier. The telescope will be designed to observe from near-ultraviolet to mid-infrared, in addition to having an adaptive optics system. That system will help fix any image blur

Telescopes are used to in astronomy. Telescopes, too, can work using convex lenses. Telescopes are an upgrade from microscopes. The camera is an everyday item. Used to store photos in it's memory, the camera also uses magnification to zoom in to take a picture. Every magnified image from convex lens has something in common. First of all, it magnifies an image. But the main thing is that the image seen is a trick of the eye. Light bounces off an object until it travels to the eye, and those light rays are parallel, so the convex lens bend them so they converge. Clarity is important in magnification. Without the clear picture, things can get confusing. For example, when looking through a telescope, someone might not be able to tell the difference between a cloud and a galaxy. Color has been found to increase the clarity and contrast in glasses, which leads to the though that color can increase the clarity and contrast of a convex glass lens. Contrast is what helps people distinguish one color from another. It is the difference between two different intensities of light. It makes things appear brighter than other things. Without contrast, people wouldn’t be able to tell the difference between a person and a wall

Catadioptric telescopes are those that use both mirrors and lenses to produce an image. The most common or popular type of catadioptric telescope is the Schmidt-Cassegrain telescope. Schmidt-Cassegrain telescopes (SCT) are a catadioptric design, meaning they use both lenses and mirrors. SCTs are primarily reflecting telescopes, but they use a corrector lens to eliminate aberrations that would result from the mirror design alone. In an SCT the incoming light passes through the Schmidt corrector lens (also called a corrector plate) at the front of telescope. It is reflected from a concave primary mirror at the back of the scope which focuses the light to the front of the telescope where it is reflected again by a smaller, convex secondary mirror. Finally, the light travels back through a hole in the primary mirror to the rear of the scope where an eyepiece is located for visual observing. (Starizona.com, 2015)

The light enters through the objective lense and meets at a focal point. That is then magnified through an eyepiece where we see the image. The effects of light passing through lenses are different depending on which lense it is passed through. Double convex lenses works by refracting light rays that are travelling parallel to the principal axis towards the normal surface. When it hits the boundary the light is passing to a more dense medium which is usually glass or plastic. Since the light rays are passing from a medium that it travels fast in to a medium that they travel slow in, it will bend towards the normal line. Which is shown on this diagram. An image is formed in a refracting telescope because the first lense (objective lense) is convex and when the light travels through the lense because the surface is transparent the light travels through the lense and meets a focal point on the other side to create an image that is real, magnified(compared to when viewing with the naked eye) and inverted because the image is formed by real rays that refract and go through the lense instead of reflecting like a mirror. For example if an astronomer is looking at the moon through a refractor telescope the image he will see is real but smaller. The eyepiece lense is also inverted (convex) because this allows the image to be ‘inverted’ again so it is the right way up for our eyes to see. This formula lets us find the distance of image1/f=1/do+1/di. An example of using this formula is if a 4 cm object is placed 12 cm in front with a focal length of 8cm. 1/f=1/do+1/di, ⅛=1/12+1/di, ⅛-1/12 =1/di, 1/24=1/di, di = 24 this equation allows us to find the distance of