PHYS 1140  

2014 Revision      

O5. 1

O5: Lenses and the refractor telescope

Introduction In this experiment, you will study converging lenses and the lens equation. You will

make several measurements of the focal length of lenses and you will construct a simple astronomical telescope. The components you will use are a kit from Learning Technologies, Inc. (www.starlab.com). At the end of the experiment the telescope is yours to keep. Theory

When a bundle of parallel light rays, called a collimated light beam, enters a converging lens, the rays are focused to a point in space a distance f, the focal length, from the surface of the lens. A converging lens is convex in shape, that is, thick in the middle and thin at the edges. A diverging lens is concave in shape, i.e. thin in the middle and thicker near the edges. Note that the diverging lens has a “virtual image” to the left of the lens, where the light rays never actually cross. The converging lens produces a “real image” where the rays do cross.

Figure 1: Basic Lenses

A converging lens can be used to form an image on a screen for an object. The lens equation relates the focal length 𝑓 of a lens, the object distance 𝑑𝑜, and the image distance 𝑑!:

(1) !!= !

!!+ !

!!

(This equation can be used for both converging and diverging lenses; the only difference is that the focal length is positive for converging lenses, negative for diverging lenses.)

Figure 2: Simple Ray-Tracing Diagram

PHYS 1140  

2014 Revision      

O5. 2

In the diagram above, the points labeled f are the focal points of the lens. The lateral magnification 𝑚 of the image is defined as: 𝑚 = ℎ! ℎ!. From the diagram above, one can show that 𝑚 can also be written as: 𝑚 = 𝑑! 𝑑!. Experimental Methods In this lab, you will use two different techniques to measure focal lengths.

Method I: You will take a collimated beam of light (parallel rays) and focus this to a point using each of the converging lenses used for your telescope. The distance from the center of the lens to the screen, when the optimal focus is achieved, tells us the focal distance of the lens. Equation [1] can also be applied to this situation. Since the incoming rays are parallel, the distance to the object is: 𝑑𝑜   =  ∞, or 1/𝑑𝑜   =  0. In this case it is clear that 𝑑𝑖 = 𝑓.

Figure 3: Converging Lens used to focus a collimated beam

To do this in the experiment you will first need to produce a collimated beam to measure the focal distances of your telescope lenses. This will be produced by the complementary collimating lens that is used to convert a point source of light (the LED at the center of the light source) into a parallel beam of light, as shown below:

Figure 4: Lens used to collimate a beam

The point source is the object and the object distance do is the focal length f. With 𝑑𝑜   =  𝑓, equation [1] predicts that 𝑑! = ∞. The rays from the lens converge "at infinity". Method II: This method uses a lens to form the real image of an object where the distances 𝑑𝑖   and 𝑑𝑜 are measured, whereupon equation [1] is used to compute 𝑓.

In the last part of this lab, you will construct a simple astronomical telescope. The

 

 

PHYS 1140  

2014 Revision      

O5. 3

astronomical telescope consists of two lenses: an objective lens with a long focal length 𝑓𝑜, and an eyepiece lens with a short focal length 𝑓𝑒. The objective lens forms the image of a distant object "at infinity". The lens equation tells us if the object distance is: 𝑑! = ∞, then the image distance is 𝑑! = 𝑓!. This image, which appears a distance 𝑓𝑜 behind the objective lens, is called an intermediate image, because it is intermediate between the objective and eyepiece lens. The observer views this image through the eyepiece lens, which acts as a magnifying glass. Note that a magnifying glass produces the largest magnification when the magnified object (i.e. the intermediate image in this case) is held a distance 𝑓𝑒 from the magnifying glass.

The angular magnification of the telescope is defined as the ratio: 𝑀 = 𝜃′ 𝜃, where (as shown in figure [5]) 𝜃′ is the angular size of the image as viewed by the observer through the telescope and 𝜃  is the angular size of the distant object as viewed without the telescope.

Figure 5: Objective and eyepiece lens ray-tracing diagram Notice that the distance between the two lenses is: ℓ = 𝑓! + 𝑓!. From the diagram above, one can show that the angular magnification can also be written as: 𝑀 = 𝑓! 𝑓!, the ratio of the focal lengths of the objective and eyepiece lenses. Experimental Procedure Part 0 Equipment Considerations (The Most Important Part)

In this lab, you will use an optics bench, which is simply a rail on which lenses are placed with a meter stick mounted on the side for measuring distances. The optics (light source, lenses, and screen) are mounted on carts that slide along the rail. The carts have markers on the side to help measure distances using the two-meter stick.

Each station has a variable intensity LED light source fixed at one end of the optics bench. There will be no need for you to slide the light source along the bench. Handle this component with care, and only make adjustments when necessary! If you need to adjust the height of the light source, turn off the power, loosen the thumbscrew on the post holder, gently slide the post attached to the LED mount up or down, and secure the thumbscrew.

In addition to the light source there are four carts with post holders that can slide along the bench. These carts should remain on the bench throughout the experiment. If the cart comes off the rail or seizes and cannot move, contact the T.A. or an 1140 staff member for assistance.

Each station has the optics mounted on posts. The lenses are mounted in lens holders along with the arrow, and the screen is a piece of paper. Place the lens and post assembly into the cart and post holder assembly by loosening the thumbscrew on the post holder (if necessary), place the lens and post into the post holder, adjust it to the necessary height, and tighten the

 

𝜃   𝜃′  

PHYS 1140  

2014 Revision      

O5. 4

thumbscrew. DO NOT remove the lens from the lens holder. Be sure not to loosen the thumbscrews too much as they are easily lost when removed from the post holder. All the optics are labeled on the posts.

When you are finished making measurements, place all of the optics back into the bin near the bench. If you are missing any components before you start the lab, contact your T.A. or 1140 staff member. DO NOT go hunting for optics at other stations.

Once finished making measurements with the main apparatus, you will construct your own telescope consisting of two cardboard “telescoping” tubes, a small eyepiece lens in grey foam, and a large objective lens in a red plastic holder. These components are found in the folder room. Find your T.A. or 1140 staff member to help you construct your telescope. Part I Use of a collimated beam

In this part you will use Method I to measure the focal length of each of your telescope lenses. On the LED power supply make sure the switch is on its left most position, then turn the dial clockwise until you have adequate brightness, approximately 2/3-3/4 of a turn. The actual LED is small enough that we can consider it to be a point source. Use the lens labeled “Collimating Lens” to form a parallel beam of light by positioning the lens so that its focus coincides with the filament of the light bulb. You can do this by studying the image of the lens on a piece of paper and moving the paper away from the lens in the direction of the beam. When the lens is positioned properly, the size of the light spot on the paper should not change with the paper position, and it should be the size of the lens. If the lens is too low, loosen the thumbscrew on the post holder, adjust the height and retighten, but try not to rotate the lens. Use the pointer on the cart and meter stick mounted beside the track to measure distances. Note that depending upon whether the paper is very close or far from the lens you may see a blue or a red “halo” around the beam spot, which has to do with chromatic aberration of the lens (different colors are focused slightly differently since they have different effective indexes of refraction in the lens). You should be working far from the lens where the halo is red.

Once a collimated beam is formed, the focal length of the objective and eyepiece lenses can be measured. These lenses are labeled “Objective Lens” and “Eyepiece Lens”. You can do this by placing one of the lenses in the collimated beam and focusing it on the screen so that a single point of light is observed. Measure the focal distance using the pointers and meter stick. Adjust the height of the lenses or screen if necessary. Make a few measurements (3-4) of the focal distance for each lens and estimate the uncertianty. For each new trial, readjust the collimation of the parallel beam of light so that any errors from this step of the measurement are averaged. Part II Images and Magnification.

In this part, you will use Method II to measure the focal length the two telescope lenses. The procedure for this is as follows:

(1) Place the arrow in front of the light source. Record the position of the arrow using the meter stick and marker.

(2) Arrange the eyepiece lens and the screen so that a sharp image of the arrow appears on the screen (the situation will be similar to the bottom figure on page 1). Measure the distances 𝑑𝑖 and 𝑑𝑜, as well as the image height ℎ! and object height ℎ!. The heights are measured with a set of plastic calipers. If you make pen/pencil marks on the image screen to

PHYS 1140  

2014 Revision      

O5. 5

measure the heights, let your T.A. or 1140 staff member know, so it can be replaced when you are finished. Compute the lateral magnification 𝑚 = ℎ! ℎ! and compare 𝑑! 𝑑! . Do the same, but for a different set of distances: 𝑑𝑖    and 𝑑𝑜, again measuring height ℎ𝑖 and height ℎ𝑜. Check how close equation [1] works for each of these cases using your measurement for the focal length from the previous part. (Hint: the overall spacing between the object, lens, and image screen is small.)

(3) Repeat step (2), but replace the eyepiece lens with the objective lens. (Hint: make sure there is ample spacing between the object, lens, and image screen.)

(4) At this point place all of the optics back in the bin, since you will not need this apparatus for Part III. Be sure to turn off the light source by turning the knob on the power supply until a “click” is heard. Part III The Astronomical Telescope In this part you will construct the telescope and estimate its magnification. In the folder room you will find all the necessary components to make your telescope. DO NOT use the lenses from the bins at the optics bench.

Choose the lens with the longest focal length. This will be the objective lens with focal length 𝑓𝑜. Also choose the lens with the shortest focal length. This will be the eyepiece with focal length 𝑓𝑒. Place the eyepiece at one of the tube in a foam mount and place the objective lens in a red plastic mount a distance ℓ = 𝑓! + 𝑓! from the eyepiece, aka. the length of the tube. Place the telescope on the rail near the two torsional pendulum stations. Aim the telescope towards the far end of the room, where there is an arrow and a graduated scale mounted on the wall, and adjust the telescope position until you can see the arrow through the telescope. It may be difficult to find the image since your telescope has a narrow field of view. Also, you may need to adjust the position of the eyepiece lens to get a sharp image. Is the final image you are looking at upright or inverted? Is it real or virtual? Explain your answers with words and diagrams.

Once you have found a clear image looking through the telescope, open your other eye so that you can look simultaneously at the enlarged image with one eye and the un-enlarged image with the other eye. If you position the telescope just right, you can see the two scales side by side and estimate the angular magnification 𝑀 of your telescope. It may be helpful to compare the full height of the piece of paper to the distance between each of the markings (which are 1/10 of the height of the paper). Compare your answer with the theoretical value of 𝑀. Keep in mind this is a very subjective measurement. The telescope is yours to keep! Guiding Questions. 1. What is the definition of the focal length of a converging lens? Illustrate your answer with

a diagram. 2. Consider a lens with a focal length of 𝑓   = 20.0  𝑐𝑚 which is used to image an object of

height ℎ𝑜   =  4.0  𝑐𝑚, a distance 𝑑𝑜   =  40.0  𝑐𝑚 away. On graph paper, draw a diagram showing the size (ℎ𝑖) and position (𝑑𝑖) of the image formed by this lens. Check that the value of 𝑑𝑖 obtained from your graph agrees with a calculation of 𝑑𝑖   made by equation [1].

PHYS 1140  

2014 Revision      

O5. 6

3. Using figure [1] show that: 𝑑𝑖𝑑𝑜

= ℎ𝑖ℎ𝑜

.s  

4. Redo problem (2) but with the distance 𝑑𝑜 = 30.0  𝑐𝑚. What is the image distance 𝑑𝑖? What will the image height ℎ𝑖 be?

5. What is a collimated beam? Draw a sketch showing how you could produce one.

Could you make a collimated beam using only a point source and a diverging lens? 6. An astronomical telescope has an objective lens with a focal length of 600mm and an

eyepiece lens with a focal length of 30mm. What is the angular magnification of this telescope?

7. The Earth’s moon as seen from the surface of the Earth has an angular size of roughly

0.5 degrees. We say that it ‘subtends’ an angle of 0.5 degrees. What is this angle in radians? The radian angular measurement is convenient because (by definition) the angle in radians is the ratio of the length of arc subtended to the radius of the circle.

8. If the Moon is roughly 385,000 km from the Earth, what must the Moon’s diameter be to

subtend this angle? How does that diameter compare to the Earth’s diameter? How does the angle subtended by the Moon compare with the angle subtended by your thumbnail when you hold your arm straight out?

9. During a full solar eclipse, the Moon almost exactly covers the disk of the Sun. In other

words, they subtend the same angle. If the distance from the Earth to the Sun is roughly 150 million kilometers, what is the diameter of the Sun?

10. If you were to look at the moon with the telescope described in problem 6, what

effective angle would the moon subtend as viewed through the telescope?

PHYS 1140  

2014 Revision      

O5. 7

Pre-lab assignment for O5: Lenses and the Refractor Telescope.

This prelab is designed to focus your attention on what is important in the lab before you start the experiment and give you a “leg up” on writing your report. Use this template when you write your report.

1. Carefully read the lab instructions for O5

2. Using Mathematica, set up a template for your lab report. This will include:

I. Header information such as title, author, lab partner, and lab section: (to do this, In Mathematica, go to “File”, “Print Settings”, “Header and Footer” from this dialog box you can enter all of the required information.) Mathematica automatically enters the file name in the right side of the header. Leave this alone.

II. Section Headings including “Title”, “Summary of Experiment”, “Data and Calculations”, “Discussion of Uncertainty”, and specific section headings for each part of the experiment. (All of the Physics 1140 lab manuals include multiple parts.)

3. Write a Summary of the experiment. What are you going to measure and what data will you collect to make the measurement? (For example, in part one of M1, you will measure the length of a pendulum along with the period of the pendulum to determine the acceleration due to gravity.)

4. For each part of the lab do the following: A.) For Part 1, Describe the process of creating a collimated beam of light and how it

will help us to determine the focal lengths of our objective and eyepiece lenses. (Specifically talk about what is happening with the light rays through this process.)

B.) For Part 2, Are the images you observe real images or virtual images? How do you know?

C.) For Part 3, Calculate the magnification of an image given the following focal lengths: fobjective = 2.3cm, feyepiece = 0.4cm

Remember every graph in 1140 should have the following:

(There are no graphs for this Prelab)

I. Plot your theory or expectation as a line. (In Mathematica, you should define a function and plot it using the command “Plot”) Reference the Mathematica tutorial to do this.

PHYS 1140  

2014 Revision      

O5. 8

II. Label your axes, in English (not just symbols) and with units.

III. Include a brief caption (namely, a text statement of what the plot shows.)

IV. Set the x and y range of the plot to be close to what you expect for your data. For example: in M1 your longest length pendulum should be no more than 130 cm in length.

5. Write a Discussion of Uncertainty. What are the major sources of uncertainty in the experiment and how will you account for them?

6. Turn in a printout of your Mathematica document that includes 2-5 above. This document should be no more than 2 pages long.