Digital Universe Guide - Hayden Planetarium

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100 3. THE MILKY WAY ATLAS disk and, relative to the pulsars, lie very close to the plane of the Galaxy. Labels The labels are a hodgepodge of different catalog source names. A few are in “English,” such as the Cyg Loop for the Cygnus Loop (the Veil Nebula region). Some have names from the Third Cambridge Radio Survey Catalog that begin with 3C, while others have a W number, from the Westerlund catalog. And there are others, too numerous to discuss here.
3.3. MILKY WAY DATA GROUPS 101 3.3.15 Orion Nebula Star Cluster Group Name oricl Reference Orion Nebula Cluster Population (Hillenbrand 1997) Prepared by Brian Abbott (AMNH/Hayden) Labels No Files ori clust.speck Dependencies halo.sgi, colorbv.cmap Census 813 stars Notes The distance for each star is statistically generated. The Orion Nebula is one of the closest star-forming regions to us. About 1,500 light-years away, ultraviolet light from its young, hot stars causes the surrounding hydrogen gas to glow. Astronomers call this an H ii region (H ii is the astronomical symbol for ionized hydrogen). We built the Orion Nebula star cluster for our model of the Orion Nebula that was used in the reopened Hayden Planetarium’s premiere space show, Passport to the Universe. In creating a 3-D model of the nebula, we needed to place the stars of the cluster within it. We turned to a study of the cluster’s stellar population by Lynne Hillenbrand, who was working at the University of California, Berkeley at the time. The catalog from her paper contains more than 1,500 stars, about half the stars in the actual cluster. The cluster is very crowded, with a peak density of 10,000 stars per cubic parsec over a wide range of masses from a tenth the Sun’s mass up to 50 times its mass. We were presented with one problem: there are no distances in the catalog. For the stellar distances, we needed to deduce them by statistical methods. Knowing the size of the cluster and approximating the shape to be roughly spherical, we placed each star along a line of sight through this imaginary sphere centered on the cluster. In this sense, these data are observed data, for the view from Earth is accurate. But the distance of each star has been derived from this educated-guess approach for the cluster distribution. Viewing the Cluster Because the cluster is so small, it can be difficult to see. One way to see it is to use Partiview to simulate a telescopic view. Center your view on the cluster as best you can (the cluster is in the sword of Orion—you will see it flash as you turn it on and off). With the cluster centered, use the FOV Slider to decrease your field of view. The cluster stars should come into view.
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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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4.1. EXTRAGALACTIC ATLAS OVERVIEW 1
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4.2. EXTRAGALACTIC ATLAS TUTORIAL 1
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4.3. EXTRAGALACTIC DATA GROUPS 169
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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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