Project Cyclops, A Design... - Department of Earth and Planetary ...

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ACKNOWLEDGMENTS The Cyclops study was greatly assisted and enriched by the informative and often inspirational contributions of a large number of people over and above those listed as participants. The opening lecture series, listed below, was particularly valuable in stimulating the group and acquainting the Fellows with the latest developments in the technologies involved in large array design. PROJECT CYCLOPS SEMINAR SERIES: What Cyclops Might See-Philip Morrison, Massachusetts Institute of Technology The Cyclops Uoncept-B.M. Oliver, Hewlett-Pacgard Design t:onstraints on Angle Pointing and Tracking Performance of Large Antennas-R.J. Wallace, Jet Propulsion Laboratory Large Orbital Antennas with Filled Apertures-//. Schuerch, Astro Research Corporation Electronics System for a Very Large Array-Sander Weinreb, National Radio Astronomy Observatory Design Concepts of the Stanford Five Element Non-Redundant Array-Ronald Bracewell, Radio Astronomy Institute, Stanford University Radio Astronomy Instrumentation Needs-Dav/d S. Heeschen, National Radio Astronomy Observatory Some New Design Principles for Large Radio Telescopes-S, yon Hoerner, National Radio Astronomy Observatory Large Ground Antennas for Space Communication- Earl Lewis, Philco-Ford Corporation Large Antenna Structures-William D. Merrick, Jet Propulsion Laboratory Radio Astronomy in NASA-William E. Brunk, National Aeronautics and Space Administration Low Noise Microwave Receivers-Walter H. Higa, Jet Propulsion Laboratory Signal Processing in Radar Astronomy-Richard Goldstein, Jet Propulsion Laboratory Advanced Radar Exploration of the Solar System- Gordon H. Pettingill, Massachusetts Institute of Technology Microwave Ground Antennas for High Efficiency Low Noise Performance-D.A. Bathker, Jet Propulsion Laboratory Array Configurations for Gathering and Processing Data-Joseph Goodman, Stanford University Radio Astronomical and Cosmological Value of a Very Large Array-Martin Rees, Cambridge University In addition to the scheduled series, the group heard talks by S.M. Katow of Jet Propulsion Laboratories and Herbert Weiss of Lincoln Laboratories. These contributed further valuable inputs on antenna design. Many private firms contributed consulting help. In particular Robert Markevitch of the Ampex Corporation and Robert Hall of the Rohr Corporation were of great assistance. The Cyclops team wishes to acknowledge this support and to thank all those who participated for their professional help. In addition we would be remiss if we did not acknowledge the hours of overtime work by Marilyn Chinn and Lorraine Welk who typed the final and earlier versions of this report. Any future job they may have will seem peaceful and simple by comparison. Finally we wish to thank the graphics department at Ames for the skillful rendering of this report and for the innumerable slides and drawings they prepared for earlier drafts and for our final briefing session. vi
TABLE OF CONTENTS Cyclops People ................................... ii PAGE Foreword ..................................... v Acknowledgements ................................. vi Chapter: 1 INTRODUCTION .............................. l LIFE 1N THE UNIVERSE .......................... 3 Converging disciplines Origin and evolution of matter Galactic evolution and stellar populations Stellar characteristics and evolution Formation and evolution of planetary systems Atmospheric evolution Ecospheres The origin of life Biological and good suns evolution Cultural evolution and development of intelligence Civilization, science and technology Concatenated probabilities The number of coexisting advanced civilizations The probability of interstellar communication References SOME REASONS FOR THE SEARCH .................... 29 Continuing adventure Bio-cosmology Our galactic heritage Possible hazards of contact POSSIBLE METHODS OF CONTACT .................... 33 Interstellar travel Interstellar probes Serendipitous contact Interstellar communication alternatives References COMMUNICATION BY ELECTROMAGNETIC WAVES ............ 37 Antenna gain and directivity The free space transmission law Noise in coherent receivers Coherent detection and matched filtering Noise in energy detection The microwave window Star noise vii
Page 1 and 2: (NASA-CR- 11_5) PROJECT CYCLOPS: A
Page 3 and 4: CR 114445 Available to the public A
Page 6 and 7: At this very minute, with almost ab
Page 10 and 11: COMMUNICATION BY ELECTROMAGNETIC WA
Page 12 and 13: APPENDIX A - Astronomical Data ....
Page 14 and 15: t _ 2
Page 16 and 17: of the living beings evolved by the
Page 18 and 19: Figure2-1. M3I,the great galaxy in
Page 20 and 21: self.Thus,wecaninterpretFigure2-2as
Page 22 and 23: magnitude (low brightness) end, the
Page 24 and 25: Red Giant. The transition from main
Page 26 and 27: tion, as the central part of the cl
Page 28 and 29: TABLE 2-4 SELECTED NEARBY STARS WIT
Page 30 and 31: tideraisingforcesasr--_ where ,v =
Page 32 and 33: 3. Is it possible that living syste
Page 34 and 35: lawsof natural selection, more like
Page 36 and 37: starsthroughout the Galaxyhave also
Page 38 and 39: if the longevity of that life is ty
Page 40 and 41: The imaginative reader will have no
Page 42 and 43: Lookingfar ahead,supposewe aresucce
Page 44 and 45: usuallyterritorial expansion by the
Page 46 and 47: IOO IO 1 [ [ J [ J I J i [ i I i I
Page 48 and 49: order with what Morrison has descri
Page 50 and 51: The quantity gtPt is often called t
Page 52 and 53: which might result from synchronous
Page 54 and 55: 1. Wewillnothavenough resolving pow
Page 56 and 57: normalwith the meanat o x/--2. When
Page 58 and 59:
Chapter11 in analyzingthe dataproce
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Therangelimitisthenfoundbyequating_
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TABLE 5-3 PARAMETER Wavelength Tran
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angeanddirectlyasthesquareof antenn
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"_ i i i i i p = STELLAR DENSITY AT
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I-- g u. O >- I--- .d tit (]O 0 0.
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andwidth that will still give near
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acquisitionphasefor otherraces.Supp
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1. They would transmit continuously
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and ¢-Ceti. No signals were detect
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vz .i g)mo PAGE NOr Ir[[,MZ 7. THE
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The price of incomplete sky coverag
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modest size.A largedatabaseontapeor
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THEAUXILIARYOPTICALSYSTEM Althoughn
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edetectedat 20,000light-years byCyc
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feeds must correct for spherical ab
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side of the dish and shade on the o
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TABLE 8-1 UNADJUSTED UNIT COST DATA
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7. Using huge specially designed ji
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9. THE RECEIVER SYSTEM The receiver
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whereP is the radiated power. Divid
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SHADOWED AREA SHADOWED AREA // // /
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Corrugatedhornssupportingbalancedhy
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o 50 ----- - _ T i 20 _,o 5 ,,,5 09
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TABLk ?- I A COMPARISON OF VARIOUS
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CENTRAL POINT STATION LSB LINE FREQ
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A02 .... + No (25) (i C 1 where No
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COAXIAL LINE DIRECTIONALCOUPLER FRE
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DeJager, J.T.:IEEETrans.onMicrowave
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pR_ING PA6E BLANK HOT FILMF_ 10. TR
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o-------------o_ _ o o o o ing of t
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addedto theother IF channel. The tw
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INPUT MHZ _PF 500 MHZ i : 575 T1 92
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azimuth _) has a delay (2a/c)sin 0
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stripline. For 2 _< k _< 6, appropr
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mation are common to all antennas i
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A cable pair costs about 20 cents/m
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11. SIGNAL PROCESSING The Cyclops s
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1.0 T t t I I r .9 -8 asynchronousl
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collimated coherent light. A simple
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power of the film and associated op
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samples simultaneously onto the sam
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outputs is assumed. COMPOSITE SIGNA
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SPECTRUM I n LINES M n LINES U SPEC
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signal andyet have a tolerable fals
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i --_- i i i i large values of n. T
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plottedin Figure11-15for various va
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All the1Fsignalswillarrivein phasei
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x:(1 +x) x 2 - _ -- (53) If we wish
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3's = unitcostof signal planelectro
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where0ma x is the maximum value of
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Roughestimates of the costs of buil
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12. CYCLOPS AS A BEACON Although th
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13. SEARCH STRATEGY The high direct
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distantgalaxies (oraninertialrefere
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wouldfollowtheuppermost linein Figu
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persquaredegreeof fieldwouldberequi
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starsfrom/'18 to G5 could support a
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14. CYCLOPS AS A RESEARCH TOOL Thro
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Only a few such galaxies have been
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15. CONCLUSIONS AND RECOMMENDATIONS
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perhapsdecadesand possiblycenturies
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APPENDIX A ASTRONOMICAL DATA DISTAN
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PLANETARY Planet ORBITS Semimajor S
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APPENDIX B SUPERCIVILIZATIONS AND C
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ABIOLOGICAL CIVILIZATIONS Many writ
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182
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tqOT APPENDIX C OPTIMUM DETECTION A
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to rmsnoise.Wenotethatthematchedfil
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APPENDIX D SQUARE LAW DETECTION THE
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If the output filter is very wide c
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if B/2 > T we can start instead wit
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Let us now introduce the normalized
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where h-- = expectation count of si
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APPENDIXE RESPONSE OF A GAUSSIAN FI
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APPENDIXF BASE STRUCTURES AZ-EL BAS
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ack,it shouldnotbenecessary to prov
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204
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206 i
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PAGE BLANK NOT APPENDIX H POLARIZAT
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APPENDIX I CASSEGRAINIAN GEOMETRY C
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APPENDIXJ PHASINGOFTHE LOCALOSCILLA
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APPENDIXK EFFECTOF DISPERSION IN CO
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APPENDIX L TUNNEL AND CABLE LENGTHS
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where r = "Ym/'rs- If we let o-_--o
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L-4 we see that the length of IF ca
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APPENDIX M PHASING AND TIME DELAY A
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andobtain V = 2 (Ps [! + _(Ar)] +Pn
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L" D 226
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APPENDIX N SYSTEM CALIBRATION The p
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APPENDIXO THE OPTICAL SPECTRUM ANAL
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232
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APPENDIX P LUMPED CONSTANT DELAY LI
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Thevalueofthefinalcoilonthelineis =
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APPENDIXQ CURVES OF DETECTION STATI
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I I I I LE :E oo
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APPENDIX R RADIO VISIBILITY OF NORM
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io 3 - l rlrllll I I I ]l+,ll_ I _f
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