Click to view NGSS connections
Supports PE HS-ESS1-2 and HS-ESS1-3 : Earth’s Place in the Universe
Supports DCI ESS1.A: The Universe and Its Stars, PS4.B: Electromagnetic Radiation
Engages in SEP 4:Analyzing and interpreting data and CCC 1:Patterns
Elements emit and absorb characteristic frequencies/wavelengths of light
Required: Pre-Flight Training – Filters: SDSS
Imagine the sky in your area on a clear night – or just look at the picture on the right. What colors do you see? If you are like most people, you see very little variation in the color of stars. It takes very dark skies, patience, and careful observation to detect the subtle color differences between stars.
It can be difficult to imagine how differences that appear so small can be so important to understanding stars and collections of stars – galaxies and clusters. Because light is the only thing that comes to us from stars, color is enormously important in astronomy. With improvements in telescope design and the invention of technologies like filters, we are able to use color as a tool for understanding size, life cycles, and distances to stars in our Milky Way. Let’s start by looking at stars through the SDSS telescope.
The picture on the left was captured by the SDSS telescope and camera. Its magnification is hundreds of times greater than your unaided eye can see. The color differences in this image are obvious because the SDSS telescope has a 2.5 meter surface that captures light which is then gathered and stored for 54 seconds before being recorded. In contrast, your eye sends picture signals to your brain at the much faster rate of once every 77 milliseconds. For astronomy purposes, however, slower is better. The SDSS telescope is best for seeing detail in the sky (whereas a picture every 54 seconds wouldn’t do you much good when trying to cross the street).
The SDSS uses the light it captures to make the beautiful images you see in SkyServer and record measurements that are used to calculate brightness and color. In this activity, we explore these measurements and learn how to interpret them. Begin by choosing a unique place in SkyServer from which to gather data.
Find a Starting Place
Space is vast and infinite, and with 500 million stars in the SDSS database, there are enough stars to go around for all researchers. Everyone should be able to start in a unique location, or Special Place (as you proceed in your experimentation and data collection, you will be able to build upon your knowledge base for your Special Place since you will continue to revisit it in other activities). If you completed the activity, My Special Place in the Database, you already have a set of coordinates as your own Special Place. Use the RA and Dec that you recorded during that activity. If you do not yet have your own Special Place, you will use RA and Dec to define a starting place (which will then become your Special Place, your very own “little plot of space real estate” to explore evermore).
If you need additional help to locate a starting place, you can choose one using the Constellations NoteBook.
Enter Your Starting Coordinates into the Navigate Tool
- Go to the SkyServer Navigate tool
- Enter the RA and Dec coordinates into the appropriate spaces in the parameters box.
- If the new location does not automatically reload, click the Get Image button.
- This is your starting place for observing star colors.
Collect Stars of Different Colors and Brightnesses
From your starting place in Navigate, zoom in until you are able to see individual stars clearly but still have approximately 20 – 30 in the image window.
- From the Navigate image window, select approximately 20 stars of different colors and apparent brightnesses.
- Add each star to your notes by selecting the Add to Notes radio button.
- View your list by clicking the Show Notes radio button
Look for Patterns
The SkyServer NoteBook allows you to look at and compare brightness information for each of the stars you selected. You should have noticed that each filter has a number associated with it. This value is calculated from the amount of light recorded by the SDSS camera in comparison with the bright star Vega. It is called magnitude. Let’s first discover a few things about what these numbers tell us.
- Click Show Notes to open your NoteBook.
- Open your collection in Images List by clicking Upload to Image List Thumbnail images of each star will be displayed the order they appear in your NoteBook.
- Drag the tabs to a position where you can see the NoteBook and Image List tool at the same time.
- Using the r column, scan the magnitude measurements, comparing them to the thumbnail images. Do you see a pattern? What can you conclude about magnitude measurements from your observations?
- Observe the magnitude measurements across the different filters. What do you notice?
We can see from our observations that only knowing how bright a star appears through a particular filter is not enough to compare the color of two stars. Consider the two stars below. These stars are obviously different colors. If you examine the magnitude of the two stars in the red filter, you find that the blue star is brighter in the red filter than the star that appears red! Examine the reported magnitudes in the remaining filters. What do you notice?
Although we can describe the color of a star using words (regardless of the overall brightness of the star), quantifying or assigning a number to the characteristic of color independent of the brightness of the object is more difficult. A measurement that is independent of the brightness of the star involves the relationship between the magnitude values of the filters. We need look no further than simple arithmetic.
Filters are windows that allow us to view portions of the energy spectrum emitted by an object. Subtraction is the mathematical tool that allows us to measure the difference between two points. Does the difference between two magnitudes provide us with a quantitative measurement that matches the color we see with our eyes? Next, we gather the data needed to answer that question.
Because of the nature of magnitude measurements (see Preflight Calculating Magnitude), astronomers can use subtraction to produce measurements that can be used to compare the color of stars. Although certain filter combinations are more common than others, you can subtract any two magnitude measurements to define color. You do need to communicate which filters you used. For example, the red star above has a u-r magnitude of 4.62. The blue star has a u-r magnitude of 2.03. Always keep in mind the inverse nature of the magnitude scale. How does this affect the interpretation of color values? Why would addition not be an effective mathematical tool for our purpose?
Explore Color Calculations
Using the same starting point in the database, gather some data about the stars in the area to demonstrate that subtracting the magnitudes in any two filters is a powerful tool for describing color in astronomy. The video below can help you get started with some ideas and procedures from which you can devise your own test of the color calculation. NOTE: When subtracting any two filters, always subtract the longer wavelength filter from the shorter. This is simply a convention (agreed upon procedure) used by astronomers. Record your procedures and your evidence in your journal.