Digital Universe Guide - Hayden Planetarium

More documents

Recommendations

Info

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
Page 1 and 2:
The Digital Universe Guide Brian Ab
Page 3 and 4:
Contents Contents 3 List of Tables
Page 5 and 6:
List of Tables 2.1 Log and Linear F
Page 7 and 8:
1.2. GETTING HELP 7 1.2 Getting Hel
Page 9 and 10:
1.5. ACKNOWLEDGMENTS 9 1.5 Acknowle
Page 11 and 12:
2.2. LAUNCHING THE MILKY WAY ATLAS
Page 13 and 14:
2.3. LEARNING TO FLY PARTIVIEW 13 T
Page 15 and 16:
2.3. LEARNING TO FLY PARTIVIEW 15 M
Page 17 and 18:
2.4. PARTIVIEW’S USER INTERFACE 1
Page 19 and 20:
Page 21 and 22:
Page 23 and 24:
2.5. DIGITAL UNIVERSE FILES 23 File
Page 25 and 26:
3.1. MILKY WAY ATLAS OVERVIEW 25 3.
Page 27 and 28:
3.2. MILKY WAY ATLAS TUTORIAL 27 3.
Page 29 and 30:
3.2. MILKY WAY ATLAS TUTORIAL 29 Wi
Page 31 and 32:
3.2. MILKY WAY ATLAS TUTORIAL 31 Yo
Page 33 and 34:
3.2. MILKY WAY ATLAS TUTORIAL 33 th
Page 35 and 36:
3.2. MILKY WAY ATLAS TUTORIAL 35 Op
Page 37 and 38:
Page 39 and 40:
3.2. MILKY WAY ATLAS TUTORIAL 39 co
Page 41 and 42:
3.2. MILKY WAY ATLAS TUTORIAL 41 li
Page 43 and 44:
Page 45 and 46:
3.2. MILKY WAY ATLAS TUTORIAL 45 In
Page 47 and 48:
3.2. MILKY WAY ATLAS TUTORIAL 47 No
Page 49 and 50:
3.2. MILKY WAY ATLAS TUTORIAL 49 Th
Page 51 and 52:
3.2. MILKY WAY ATLAS TUTORIAL 51 to
Page 53 and 54:
3.2. MILKY WAY ATLAS TUTORIAL 53 st
Page 55 and 56:
3.2. MILKY WAY ATLAS TUTORIAL 55 th
Page 57 and 58:
3.2. MILKY WAY ATLAS TUTORIAL 57 bi
Page 59 and 60:
3.2. MILKY WAY ATLAS TUTORIAL 59 in
Page 61 and 62:
Page 63 and 64:
3.2. MILKY WAY ATLAS TUTORIAL 63 mo
Page 65 and 66:
3.2. MILKY WAY ATLAS TUTORIAL 65 fa
Page 67 and 68:
3.3. MILKY WAY DATA GROUPS 67 Earth
Page 69 and 70:
3.3. MILKY WAY DATA GROUPS 69 Data
Page 71 and 72:
3.3. MILKY WAY DATA GROUPS 71 The l
Page 73 and 74:
3.3. MILKY WAY DATA GROUPS 73 3.3.3
Page 75 and 76: 3.3. MILKY WAY DATA GROUPS 75 3.3.4
Page 77 and 78: 3.3. MILKY WAY DATA GROUPS 77 If yo
Page 79 and 80: 3.3. MILKY WAY DATA GROUPS 79 lumin
Page 81 and 82: 3.3. MILKY WAY DATA GROUPS 81 not p
Page 83 and 84: 3.3. MILKY WAY DATA GROUPS 83 Two p
Page 85 and 86: 3.3. MILKY WAY DATA GROUPS 85 expre
Page 87 and 88: 3.3. MILKY WAY DATA GROUPS 87 marke
Page 89 and 90: 3.3. MILKY WAY DATA GROUPS 89 brigh
Page 93 and 94: 3.3. MILKY WAY DATA GROUPS 93 inclu
Page 95 and 96: 3.3. MILKY WAY DATA GROUPS 95 old.
Page 97 and 98: 3.3. MILKY WAY DATA GROUPS 97 centi
Page 101 and 102: 3.3. MILKY WAY DATA GROUPS 101 3.3.
Page 103 and 104: 3.3. MILKY WAY DATA GROUPS 103 heat
Page 107 and 108: 3.3. MILKY WAY DATA GROUPS 107 righ
Page 109 and 110: 3.3. MILKY WAY DATA GROUPS 109 beyo
Page 121 and 122: 3.3. MILKY WAY DATA GROUPS 121 Othe
Page 123 and 124: 3.3. MILKY WAY DATA GROUPS 123 abou
Page 125: 3.3. MILKY WAY DATA GROUPS 125 Obje
Page 141 and 142: 3.3. MILKY WAY DATA GROUPS 141 this
Page 143 and 144: 3.3. MILKY WAY DATA GROUPS 143 Not
Page 145 and 146: 4 The Extragalactic Atlas The word
Page 147 and 148: 4.1. EXTRAGALACTIC ATLAS OVERVIEW 1
Page 153 and 154: 4.2. EXTRAGALACTIC ATLAS TUTORIAL 1
Page 169 and 170: 4.3. EXTRAGALACTIC DATA GROUPS 169
Page 177 and 178:
4.3. EXTRAGALACTIC DATA GROUPS 177
Page 179 and 180:
Page 181 and 182:
Page 183 and 184:
Page 185 and 186:
Page 187 and 188:
Page 189 and 190:
Page 191 and 192:
Page 193 and 194:
Page 195 and 196:
Page 197 and 198:
Page 199 and 200:
Page 201 and 202:
Page 203 and 204:
Page 205 and 206:
4.4. OPTIMIZING THE EXTRAGALACTIC A
Page 207 and 208:
Appendix A Light-Travel Time and Di
Page 209 and 210:
Appendix B Parallax and Distance On
Page 211 and 212:
absolute magnitude M, can be calcul
Page 213 and 214:
discovered that there was a linear
Page 215 and 216:
Appendix D Electromagnetic Spectrum
Page 217 and 218:
Appendix E Constants and Units In a
Page 219 and 220:
Metric Prefixes These prefixes are
Page 221 and 222:
INDEX 221 center command, 50, 61 cl
Page 223 and 224:
INDEX 223 Earth’s radio signals,
Page 225 and 226:
INDEX 225 irregular galaxy, 147, 17
Page 227 and 228:
INDEX 227 entering, 21 every, 206 j
Page 229:
INDEX 229 stellar distance uncertai
show all

Digital Universe Guide - Hayden Planetarium

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?