Digital Universe Guide - Hayden Planetarium

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124 3. THE MILKY WAY ATLAS 3.3.29 Deep-Sky Images Group Name dso Reference NOAO, see dso.speck file for image credits Prepared by Nate Greenstein, Matt Everhart, Ryan Wyatt, Brian Abbott (AMNH/Hayden) Labels Yes Files dso.speck, dso.label Dependencies Various images Census 65 images “Deep-sky object” is a term familiar to avid sky watchers as an object in the sky that is not a star or planet. These include open and globular star clusters, nebulae, supernova remnants, and even galaxies. Often invisible to the unaided eye, they require binoculars or a telescope to view them. The first list of such objects was compiled by Charles Messier (1730–1817), a French astronomer who was searching for comets. Comets resemble diffuse, fuzzy objects, and with the low-power optics of the day, star clusters, nebulae, and galaxies looked like diffuse comets too. In order to distinguish these static nebulae, clusters, and galaxies from the comets that move in the sky, Messier created a list of the stationary diffuse objects so he would not confuse them with the comets he was searching for. The resulting list contains 110 objects beginning with Messier object 1, or M1, also known as the Crab Nebula, and ending with M110, a small satellite galaxy of the Andromeda Galaxy, which itself is called M31. The dso data are 2-D images of Messier objects placed in 3-D space. Not only do we place our images at the proper location and give them the correct orientation, we also size them accurately so that you can fly to the globular cluster M13, for example, and see just how small the cluster of hundreds of thousands of stars is relative to the rest of the Galaxy. The group consists mainly of open star clusters, globular clusters, diffuse nebulae, and planetary nebulae. All together, sixty-seven of the Messier objects are represented in 65 images (M32 and M110 appear in the image for M31). We do not include galaxies outside the Local Group or objects for which we have 3-D data, which is often superior to a 2-D image. For example, you will not see the Orion Nebula (M42 and M43) because we have a 3-D Orion Nebula model (orineb group) in the atlas. Similarly, we have 3-D stars in place for M45 (Pleiades), M44, and a few other open star clusters. Below we list the Messier objects included in the dso group.
3.3. MILKY WAY DATA GROUPS 125 Object type Messier objects included Open star clusters 6, 7, 11, 16, 18, 21, 23–26, 29, 34–39, 41, 46– 48, 50, 52, 67, 93, 103 Globular star clusters 2–5, 9, 10, 12–15, 19, 22, 28, 30, 53–56, 68–72, 75, 79, 80, 92, 107 Planetary nebulae 27, 57, 76, 97 Diffuse nebulae 8, 17, 20, 78 Supernova remnants 1 Galaxies 31, 32, 33, 110 You may know some of these objects by their common names: M1 Crab Nebula M8 Lagoon Nebula M16 Open cluster (in the Eagle Nebula) M17 Omega Nebula M20 Trifid Nebula M27 Dumbbell Nebula M31 Andromeda Galaxy M57 Ring Nebula M97 Owl Nebula I Don’t See Any Images! By default, the dso data group is on when you launch the Milky Way Atlas, but you are not likely to notice them just as you don’t typically see these objects in the night sky. This is due to their size, which in most cases is quite small. One way to pick them out is to turn on the labels for the group. To see the image, you can either zoom in from your current location on Earth, or fly out to the object. To view the images from Earth’s position, you can use Partiview to simulate how we see these objects in the night sky when looking through binoculars or a telescope. Center one of the objects in your view and select fov from the Slider Menu. The default value for the Digital Universe is 60 ◦ . To zoom in, decrease the field of view by moving the slider to the left. You may need to center the object as you zoom in. The value to the left of the slider is the field of view (in degrees) of your window in the up-down direction. A value of 5–10 degrees might simulate a pair of binoculars while a value less than 0.5 replicates a telescopic 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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3.2. MILKY WAY ATLAS TUTORIAL 29 Wi
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3.2. MILKY WAY ATLAS TUTORIAL 35 Op
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3.2. MILKY WAY ATLAS TUTORIAL 51 to
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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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Page 145 and 146: 4 The Extragalactic Atlas The word
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4.3. EXTRAGALACTIC DATA GROUPS 175
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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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