Digital Universe Guide - Hayden Planetarium

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126 3. THE MILKY WAY ATLAS Of course, you can also exaggerate the size of the images by changing the polygon size of the data group, but we don’t recommend this as a means of seeing the images since it grossly misrepresents these data. However, if you do increase the polygon size by choosing polysize from the Slider Menu, a polygon size of 1.0 will bring them back to their actual size. Image Credits For information such as credits, place your mouse over an image and hit the p key. This picks an object in your view, which will be challenging if you have a lot of data in your view. For example, if you zoom in on M27, the Dumbbell Nebula, and hit the p key while your mouse is over the image, you will see the following one-line report in the Console Window: [g28]Picked -121.574 -217.853 -16.117 (w121.574 217.853 -16.117) "M27 (Joe and Gail Metcalf/Adam Block/NOAO/AURA/NSF)" @250 (of 2); texture 27 radius 0.2568 The first numbers describe the location of the object selected, followed by the object name and image credit in quotes, followed by other metadata values associated with the data point.
3.3. MILKY WAY DATA GROUPS 127 3.3.30 Galaxy Image Group Name galaxy Reference European Space Agency Prepared by Carter Emmart (AMNH/<strong>Hayden</strong>) Labels No Files mwpoly.speck Dependencies ngc1232.sgi A problem that continues to baffle astronomers today is defining the structure of our star system, the Milky Way. Because we reside within our Galaxy, we cannot see the larger picture of what the Galaxy actually looks like. Even today, astronomers continue to debate the structure of the Milky Way with more uncertainty than that of other galaxies that are millions of light-years away. In 1918 and 1919, a series of papers by Harlow Shapley were published that described the dimensions of our Galaxy. Using the distribution of globular clusters in the sky, Shapley deduced that the center of our star system was in the direction of Sagittarius and that the distance to those clusters was greater than anyone had ever proposed. A great debate had taken the astronomical world by storm. Was the Andromeda Nebula inside our own Galaxy, or was it a distant extragalactic object similar to our Galaxy? Within five years, Edwin Hubble solved the debate by observing Cepheid variable stars in the Andromeda Nebula, which allowed him to measure the distance to the star system, now called a galaxy with confidence. This debate and its outcome gave astronomers a better idea of how the Galaxy was structured. With other galaxies as examples, it soon became clear that we were inside a spiral galaxy like Andromeda. The Galaxy in 2-D The exterior view of the Milky Way is simply a two-dimensional image. The image is that of NGC 1232, a galaxy thought to resemble our Milky Way. The image has been properly sized and functions as a placeholder, allowing one to gauge the scale of the Galactic disk relative to other data sets in the Atlas. You can adjust the brightness of the Galaxy using the Alpha Slider. Its size is specified in the speck file but is also affected by commands in the mw.cf file. The features you see in the image, of course, do not represent our Galaxy but resemble similar features found in our Galaxy. The Sun is just on the inside of the smaller Orion Arm, sometimes called the Orion Spur, as it might connect the Sagittarius and Perseus arms. The features seen in this image
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The Digital Universe Guide Brian Ab
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Contents Contents 3 List of Tables
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List of Tables 2.1 Log and Linear F
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1.2. GETTING HELP 7 1.2 Getting Hel
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1.5. ACKNOWLEDGMENTS 9 1.5 Acknowle
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2.2. LAUNCHING THE MILKY WAY ATLAS
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2.3. LEARNING TO FLY PARTIVIEW 13 T
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2.3. LEARNING TO FLY PARTIVIEW 15 M
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2.4. PARTIVIEW’S USER INTERFACE 1
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2.5. DIGITAL UNIVERSE FILES 23 File
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3.1. MILKY WAY ATLAS OVERVIEW 25 3.
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3.2. MILKY WAY ATLAS TUTORIAL 27 3.
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3.2. MILKY WAY ATLAS TUTORIAL 29 Wi
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3.2. MILKY WAY ATLAS TUTORIAL 51 to
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3.2. MILKY WAY ATLAS TUTORIAL 59 in
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3.2. MILKY WAY ATLAS TUTORIAL 63 mo
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3.2. MILKY WAY ATLAS TUTORIAL 65 fa
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3.3. MILKY WAY DATA GROUPS 67 Earth
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3.3. MILKY WAY DATA GROUPS 69 Data
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3.3. MILKY WAY DATA GROUPS 71 The l
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3.3. MILKY WAY DATA GROUPS 73 3.3.3
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Page 145 and 146: 4 The Extragalactic Atlas The word
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4.3. EXTRAGALACTIC DATA GROUPS 177
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4.4. OPTIMIZING THE EXTRAGALACTIC A
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Appendix A Light-Travel Time and Di
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Appendix B Parallax and Distance On
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absolute magnitude M, can be calcul
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discovered that there was a linear
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Appendix D Electromagnetic Spectrum
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Appendix E Constants and Units In a
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Metric Prefixes These prefixes are
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INDEX 221 center command, 50, 61 cl
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INDEX 223 Earth’s radio signals,
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INDEX 225 irregular galaxy, 147, 17
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INDEX 227 entering, 21 every, 206 j
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INDEX 229 stellar distance uncertai
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Digital Universe Guide - Hayden Planetarium

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