prepublication copy - The Department of Astronomy & Astrophysics ...

More documents

Recommendations

Info

FIGURE 2‐6 Top: Schematic of the evolution from left to right of an inflationary universe to recombination to reionization and first star/galaxy formation to today’s Earth‐bound telescopes. Overlaid in tiles are predicted 21cm signals from the Murchison Widefield Array. Bottom: The same signals detected at 150 MHz in an all‐sky map from the Precision Array to Probe the Epoch of Reionization. (Credit: Astro2010 RFI input on HERA for the composite, with individual images from S. Djorgovski, S. Furlanetto, J. Lazio, A. Parsons et al.) These events lie largely in the realm of theory today and existing telescopes can barely probe this mysterious era. Over the next decade, we expect this to change. A new window on the cosmos is being opened in several wavelengths: Radio astronomers are constructing telescopes that will tell us when and where the first stars in the universe formed by mapping their effect on the primordial hydrogen at the end of the dark ages and are planning those that will be able to directly observe the primordial hydrogen atoms that permeated the dark ages of the universe (Figure 2-6). Large X-ray telescopes can detect the first massive black holes and quasars at very great distances. While the “first stars” are mostly likely too faint to observe individually, they should form in the collapsing clumps of gas that are the small building blocks of future galaxies like our Milky Way. ALMA and the EVLA will detect and conduct studies of many of these protogalaxies. JWST should be able to image them as well, while the proposed next generation of giant ground-based optical/infrared telescopes would investigate these first objects in detail (measure their mass, chemical composition, and ages). There is also growing evidence that many gamma-ray bursts are the explosive deaths of very massive stars with the unusual chemical compositions expected for the first stars (nearly devoid of elements heavier than hydrogen and helium). The study of their violent deaths offers another way to learn about the first stars. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION 2-12
The Origin of Galaxies and Large-Scale Structure The small proto-galactic fragments containing the first stars were embedded in halos of dark matter, which formed first and provided most of the total mass. Through their mutual gravitational attraction, these small fragments of gas and dark matter would have slowly fallen towards other such objects, collided, and then merged into larger objects. This process continued over the entire history of the universe: in the densest regions, small objects merge to form medium-sized objects which later merge to form large objects (Figure 2-7). Over time even larger structures form: groups and clusters of galaxies, and the filaments that connect these clusters to one another in the vast cosmic web. Thanks to major surveys of the last decade, we now have a precision map of the cosmic cartography of the present-day local universe that is the result of this process of merging. Over the next decade it will be a high priority to extend such precision mapping over cosmic time: to have, in effect, a 13-billion-year-long movie that traces the build-up of structure since the universe first became transparent to light. This can be done by using radio telescopes to provide more detailed maps of the cosmic microwave background and to detect the atomic hydrogen gas all the way back into the dark ages, by using large spectroscopic surveys in the visible and near-infrared to trace the distribution of galaxies, by using gravitational lensing to trace the distribution of the dark matter halos, by ultraviolet spectroscopic surveys to map out the warm tenuous gas lying in the vast cosmic filaments, and by radio Sunyaev- Zel’dovich effect and X-ray surveys that reveal the distribution of the hot gas found in groups and clusters of galaxies. FIGURE 2‐7 This enlargement of part of the Hubble Ultra Deep Field shows distant young galaxies in the process of forming; several galaxy mergers and unusual structures are evident. Credit: NASA, ESA, S. Beckwith and the Hubble Ultra Deep Field team. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION 2-13
Page 1:
PREPUBLICATION COPY
Page 4 and 5:
THE NATIONAL ACADEMIES PRESS 500 Fi
Page 7 and 8:
COMMITTEE FOR A DECADAL SURVEY OF A
Page 9 and 10: Panel on Stars and Stellar Evolutio
Page 11 and 12: DOUGLAS FINKBEINER, Harvard Univers
Page 13: SPACE STUDIES BOARD CHARLES F. KENN
Page 16 and 17: activities 2 that have emerged from
Page 18 and 19: In addition to the 27 panel meeting
Page 20 and 21: Acknowledgment of Reviewers This re
Page 22 and 23: The Accelerating Universe 2-26 The
Page 24 and 25: APPENDIXES A Summary of Science Fro
Page 26 and 27: light up the universe, marking the
Page 28 and 29: RECOMMENDED PROGRAM Maintaining a b
Page 30 and 31: TABLE ES.4 Space: Recommended Activ
Page 32 and 33: Cosmic Dawn: Searching for the Firs
Page 34 and 35: this imprint would both probe funda
Page 36 and 37: important outcome will be to open u
Page 38 and 39: estimated to be on the order of $20
Page 40 and 41: observatories. For NASA an annual b
Page 42 and 43: surveys of large fields, enabling s
Page 44 and 45: RECOMMENDATION: U.S. investors in a
Page 46 and 47: departments and the community as a
Page 48 and 49: dominate spending; (2) private-publ
Page 50 and 51: us was certainly evident during the
Page 52 and 53: BOX 2-1 Other Worlds Around Other S
Page 54 and 55: FIGURE 2‐2 The source 3C 75, show
Page 56 and 57: FIGURE 2‐3 Numerical simulation o
Page 58 and 59: FIGURE 2‐4 Left panel: Image of t
Page 62 and 63: Most stars with masses smaller than
Page 64 and 65: BOX 2-2 The Origin of Planets After
Page 66 and 67: send material raining into the cent
Page 68 and 69: BOX 2-4 Lifecycles in Galaxies One
Page 70 and 71: Stars Stars are the most observable
Page 72 and 73: ubiquitous high-energy charged-part
Page 74 and 75: The Nature of Inflation As describe
Page 76 and 77: FIGURE 2‐11 Pie chart showing the
Page 78 and 79: An important clue to the nature of
Page 80 and 81: Studying the properties of neutron
Page 82 and 83: FIGURE 2‐14 A possible pathway is
Page 84 and 85: partners and makes recommendations
Page 86 and 87: As astronomy research has blossomed
Page 88 and 89: are increasingly relevant. The Euro
Page 90 and 91: TABLE 3-1 Currently Operating OIR F
Page 92 and 93: 29% 1990 44% US Priv US Fed Other E
Page 94 and 95: CONCLUSION: Complex and high-cost f
Page 96 and 97: Space Observatories The Laser Inter
Page 98 and 99: Physics Division (PHY); the Mathema
Page 101 and 102: 4 Astronomy in Society Astronomy of
Page 103 and 104: FIGURE 4‐2 The dust sculptures of
Page 105 and 106: FIGURE 4‐5 President Obama takes
Page 107 and 108: Astronomy Inspires in the Classroom
Page 109 and 110: teaching the scientific method. The
Page 111 and 112:
where the fraction of astronomers h
Page 113 and 114:
Percentage of AAS Membership by Fie
Page 115 and 116:
0.4 0.3 0.2 0.1 PL SO IM AG SF IN S
Page 117 and 118:
FIGURE 4‐12 Number (top panel) an
Page 119 and 120:
Professional training needs to acco
Page 121:
assistant and associate professor p
Page 124 and 125:
fluctuating level of funding for as
Page 126 and 127:
THEORY Emerging Trends in Theoretic
Page 128 and 129:
Central to the Galaxies across Cosm
Page 130 and 131:
TABLE 5‐2 Support for astrophysic
Page 132 and 133:
would normally be for a five-year p
Page 134 and 135:
FIGURE 5‐7 Highly cited HST publi
Page 136 and 137:
y optical and radio astronomers are
Page 138 and 139:
FIGURE 5‐8 Number of PhDs per yea
Page 140 and 141:
ated by the Program Prioritization
Page 142 and 143:
nulling interferometry. The appropr
Page 144 and 145:
FIGURE 5‐9 The richness of the su
Page 146 and 147:
RECOMMENDATION: NASA and NSF suppor
Page 148 and 149:
FIGURE 6‐1. All sky map as observ
Page 150 and 151:
FIGURE 6‐3 NASA mission cost over
Page 152 and 153:
FIGURE 6‐5 Gemini North with Sout
Page 154 and 155:
TOWARD FUTURE PROJECTS, MISSIONS, A
Page 156 and 157:
3. Investment in new and upgraded i
Page 158 and 159:
etween several competing elements i
Page 161 and 162:
7 Realizing the Opportunities The p
Page 163 and 164:
FIGURE 7.1 Survey time line showing
Page 165 and 166:
SCIENCE OBJECTIVES FOR THE DECADE T
Page 167 and 168:
Box 7.1 Implementing a Cosmic Dawn
Page 169 and 170:
JWST, with its superb mid-infrared
Page 171 and 172:
optical imaging of brighter galaxie
Page 173 and 174:
Box 7.3 Implementing the Physics of
Page 175 and 176:
FIGURE 7.2 Multiwavelength images o
Page 177 and 178:
Recommendations for New Space Activ
Page 179 and 180:
FIGURE 7.4 Science accomplishments
Page 181 and 182:
significance of mergers in the buil
Page 183 and 184:
independent advice committee review
Page 185 and 186:
committee review. It could range be
Page 187 and 188:
Laboratory Astrophysics As describe
Page 189 and 190:
Recommendations for New Ground-Base
Page 191 and 192:
Program for instrumentation and fac
Page 193 and 194:
excel at high spectral and spatial
Page 195 and 196:
The committee reviewed a technical
Page 197 and 198:
FIGURE 7.10 ACTA would be, like the
Page 199 and 200:
Advanced Technologies and Instrumen
Page 201 and 202:
LISA as soon as possible subject to
Page 203:
FIGURE 7.14 DOE recommended program
Page 207 and 208:
A Summary of Science Frontiers Pane
Page 209 and 210:
PLANETARY SYSTEMS AND STAR FORMATIO
Page 211 and 212:
A preliminary recommended program w
Page 213 and 214:
certified as independent work perfo
Page 215 and 216:
penalty based on an assessment of s
Page 217 and 218:
The results show excellent correlat
Page 219 and 220:
$12 MILLION TO $40 MILLION RANGE CM
Page 221 and 222:
decadal research strategy with reco
Page 223 and 224:
CFP CHIPSat CIP CGRO CMB CMU CoBRA
Page 225 and 226:
NRC NSB NSF NSF-AGS NSF-ARC NSF-AST
show all

prepublication copy - The Department of Astronomy & Astrophysics ...

Create successful ePaper yourself

Delete template?

Save as template?