Hands-on Activity: Using Spectral Data to Explore Saturn and Titan
Contributed by: Laboratory for Atmospheric and Space Physics (LASP), University of Colorado Boulder

 (left) A missions operations specialist at the University of Colorado's Laboratory for Atmospheric and Space Physics controls a spacecraft to collect data to further understand planetary science. (right) The Cassini orbiter carries specially-designed spectral filters that can pierce Titan's veil and capture an image of Saturn's moon.copyright
 SummaryStudents use authentic spectral data from the Cassini mission of Saturn and Saturn's moon, Titan, gathered by instrumentation developed by engineers. Taking these unknown data, and comparing it with known data, students determine the chemical composition of Saturn's rings and Titan's atmosphere.
 Engineering Connection Relating science and/or math concept(s) to engineering The instruments aboard Cassini were engineered to gather data about Saturn and Saturn's moons and rings. Mechanical and electrical engineers designed and built these instruments to help advance our knowledge of planetary science.

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 Grade Level: 8 (7-9) Group Size: 1 Time Required: 45 minutes Activity Dependency :None Expendable Cost Per Group Keywords: My Rating: Avg Rating: Not Yet Rated.Teacher Experiences  |  Share your experience!

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Educational Standards :

•   Common Core State Standards for Mathematics: Math
•   International Technology and Engineering Educators Association: Technology

Students should have some understanding of the nature of light (such as, rainbows are formed with light). Students should also be familiar with graphical representations of data, such as line plots.

After this activity, students should be able to:
• Explain that spectral data correlates to chemical compositions.
• Match plots of real data to experimentally known data.
• Describe how engineers design tools to help advance our knowledge of planetary science.

Each student needs:

In 1997, NASA launched the Cassini spacecraft, the first spacecraft to orbit Saturn. Since June 30, 2004, Cassini has been sending back images and data from Saturn, its rings, and its Moons, including Saturn's largest moon, Titan. Engineers collaborated with scientists to create instrumentation that sits onboard Cassini. Mechanical, electrical and aerospace engineers made sure the components of Cassini work properly and could withstand the launch and rigors of space travel. The spacecraft must be able to communicate with people on Earth, operate in very cold and harsh conditions, and travel in the right direction! All of these things require engineering to make sure the spacecraft is healthy, going the right way, and able to send data back to Earth.
Cassini carries 12 different data collection instruments, including optical and microwave cameras and spectrometers. One of these instruments is the ultraviolet imaging spectrograph (UVIS). Spectrographs measure the wavelengths and intensities of light coming from objects in space. Every chemical element emits light at a characteristic set of light wavelengths. By looking at the spectral 'fingerprints' of an object, like those generated from UVIS data, scientists can determine an object's chemical composition.
Today, we will look at two spectra from the ultraviolet imaging spectrograph (UVIS) that traveled to Saturn aboard the Cassini spacecraft. After you look at these images (on the first page), you will look at the known spectra of four elements, hydrogen (H), helium (He), nitrogen (N) and krypton (Kr) (on the second page).
Match the patterns of peaks and valleys in the known spectra with those you see on the UVIS spectra to determine what elements UVIS is seeing in Saturn's rings and on Titan.

 spectrum (plural: spectra): The pattern light produces as can be seen through a spectrograph. spectrometer (also spectroscope, spectrograph): A tool that allows the components of light to be seen easily with the eye. Titan: A moon of Saturn that has an incredibly thick atmosphere. microwave: A type of light that can be detected with a microwave camera. ultraviolet: A type of light that can be detected with an ultraviolet detector.

Background

It is highly recommended that you read the following articles:
http://www.pbs.org/wgbh/nova/titan/atmosphere.html
http://planetquest.jpl.nasa.gov/science/
Light is sometimes called the electromagnetic (E-M) spectrum, of which visible light is only a small portion. Other types of E-M radiation include gamma rays, x-rays, UV, infrared, microwave and radio. Light can be thought of as both a wave and a particle in all cases. The more energetic the particle of light, the shorter wavelength, and hence, smaller frequency, it will have. Gamma rays are the most energetic, and radio are the least.
Spectral patterns of a gas can be shown on a plot such that the x-axis is the wavelength of the light, and the y-axis is the intensity of the light. Plotted in this way, scientists can determine if laboratory measurements of a gas match with data obtained elsewhere because every element has a unique signature. In this activity, students compare the spectral lines in Titan's and Saturn's atmosphere with laboratory measurements of spectra.
Titan has a thick atmosphere consisting mostly of nitrogen, similar to the Earth's. The gravitational properties of a large moon like Titan are very different from those of a debris field like the rings. Titan's gravity captures atoms like nitrogen that would otherwise escape to space. Unlike Titan's atmosphere, Earth's atmosphere contains oxygen, mostly a result of photosynthesis. Before plants, the Earth did not have oxygen in its atmosphere (see Figure 1). We might speculate that Titan has no plant life (at least as we know it) because Titan's atmosphere lacks oxygen.
 Figure 1. A timeline shows creation oxygen in the the Earth's atmosphere.copyright

Before the Activity

With the Students

1. Hand out the worksheets.
2. Today, we will look at two spectra from the ultraviolet imaging spectrograph (UVIS) that traveled to Saturn aboard the Cassini spacecraft.
3. After you look at these images (on the first page), look at the known spectra of four elements (H), helium (He), nitrogen (N) and krypton (Kr) (on the second page).
4. Match the patterns of peaks and valleys in the known spectra with those you see on the UVIS spectra to determine what elements UVIS is seeing in Saturn's rings and on Titan. Enter your answers on the worksheet.
5. Roam around the room to talk to individual students about the graphs.
6. Ask students questions about what they see in the plots and why the pictures correspond to a graph.
7. Have students answer the remaining questions on the worksheet.
8. Conclude with a class discussion of the worksheet answers.

Severely vision-impaired and blind children will have difficulty with this activity. Students with corrective lenses will not have difficulty. Pair students with them to assist them with the activity.

Pre-Lesson Assessment

Accessing Prior Knowledge: Ask students what they can tell you about light. Probe them for what they already know and understand. Ask students if they are familiar with any devices that people use as tools to help them determine values that they cannot "see," such as thermometers, barometers, radon detectors, x-ray machines, etc.

Post-Introduction Assessment

Class Brainstorm: Ask students why they think instrumentation is needed to get this type of data, and for what the data could be used. Honor creative answers.

Post-Activity Assessment

Worksheet Discussion: Review and discuss the worksheet answers with the entire class. Use the answers to gauge students' mastery of the subject.

Complete the Building a Fancy Spectrograph activity.

Fisher, Diane. "Taking Apart the Light." "The Technology Teacher." March 2002.

Contributors

Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder