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

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REFERENCES 1. Dole, Stephen H.: Habitable Planets for Man, Blaisdell (Ginn & Co.), New York. 2. Johnson, Harold L.: Interstellar Extinction in the Galaxy. Astrophysical Journal, 141, 1965, pp. 923-942. 164
14. CYCLOPS AS A RESEARCH TOOL Throughout this first cut at the Cyclops system design, the sole intent has been to optimize its performance as an initial detector of intelligent transmissions. Nevertheless, it has characteristics that may make it a particularly desirable terminal for other deep space studies. Just as the JPL 210 ft Deep Space Facility has proved very useful in certain geodetic, radio and radar astronomical studies, there are research areas where Cyclops, once built, should have such special capability that it may be worth devoting a fraction of its operating time to these secondary research possibilities. For example, consider a "3 km equivalent Cyclops." Collecting area = 7X 106 m 2 = 2200 X (area of JPL- 210 ft) = 6700 X (area of Haystack - 120 ft) Angular resolution _- 1 arc sec at X = 3 cm Instantaneous frequency bandwidths from 0.1 Hz to 100 Mz Rapid frequency-band change in the range 0.5 - 10 GHz Ability to operate in various subarray formats Three research fields where these properties should be particularly useful are discussed below. DEEP-SPACE PROBES The several-thousandfold increase in sensitivity and/ or bit rate capacity over present facilities could alter the format of deep space exploration by probes. For instance, with no appreciable change in probe design, the same total information and bit rate would obtain for observations of Uranus (mean orbital radius = 19.2 AU) as are now possible for Mars (mean orbital radius = 1.52 AU). Alternatively, lighter and faster probes, using the same launch facilities, could examine the remote planets after appreciably shorter travel times than present facilities permit (5 to 10 years, or more). This is not the place to discuss possible tradeoffs in detail, but it would seem likely that if a major consideration in probe design were to change by a factor on the order of 103 a major change in probe strategy might result. As another example, an important problem in solar system physics concerns the nature and position of the boundary between the solar wind and the interstellar plasma (ref.l). Pioneer F will be launched early in 1972 and should reach Jupiter in about 650 days. After Jupiter flyby, the probe will have a velocity sufficient to escape the solar system, drifting outward radially at about 2 AU/year. If the boundary of the heliosphere is 30-60 AU as some suspect, it will be a long time (in human terms) before we know the answers to our questions. Again, if Cyclops were available, it would seem worthwhile to consider a light, fast probe bearin_ minimal instrumentation, that could reach the heliospheric boundary in a much shorter time and relay back information for as long a time as it continued on out into the adjacent interstellar medium. Any experiment possible using the JPL 210 ft facility could be carried on at a distance (2.21X103) 1/2 ___47 times as great with Cyclops. RADAR ASTRONOMY Over the past decade, radar astronomy, using modest equipment and highly developed analytical techniques, has provided striking new data and insights in the field of solar system physics. Because of power and antenna limitations, its studies have been restricted in the main to nearby objects: the Moon, Venus, and Mars. With our 3-km assumption, using Cyclops only as a receiving terminal would extend the present radar capabilities by a factor of 7 to 9 in range, depending on whether the comparison is with the 210 ft or the 120 ft antennas. If the same total transmitter power presently used is installed in each element of the Cyclops array the range of current experiments could be extended by factors of 165
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(NASA-CR- 11_5) PROJECT CYCLOPS: A
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CR 114445 Available to the public A
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At this very minute, with almost ab
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ACKNOWLEDGMENTS The Cyclops study w
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COMMUNICATION BY ELECTROMAGNETIC WA
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APPENDIX A - Astronomical Data ....
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t _ 2
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of the living beings evolved by the
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Figure2-1. M3I,the great galaxy in
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self.Thus,wecaninterpretFigure2-2as
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magnitude (low brightness) end, the
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Red Giant. The transition from main
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tion, as the central part of the cl
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TABLE 2-4 SELECTED NEARBY STARS WIT
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tideraisingforcesasr--_ where ,v =
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3. Is it possible that living syste
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lawsof natural selection, more like
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starsthroughout the Galaxyhave also
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if the longevity of that life is ty
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The imaginative reader will have no
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Lookingfar ahead,supposewe aresucce
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usuallyterritorial expansion by the
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IOO IO 1 [ [ J [ J I J i [ i I i I
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order with what Morrison has descri
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The quantity gtPt is often called t
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which might result from synchronous
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1. Wewillnothavenough resolving pow
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normalwith the meanat o x/--2. When
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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
Page 125 and 126: INPUT MHZ _PF 500 MHZ i : 575 T1 92
Page 127 and 128: azimuth _) has a delay (2a/c)sin 0
Page 129 and 130: stripline. For 2 _< k _< 6, appropr
Page 131 and 132: mation are common to all antennas i
Page 133 and 134: A cable pair costs about 20 cents/m
Page 135 and 136: 11. SIGNAL PROCESSING The Cyclops s
Page 137 and 138: 1.0 T t t I I r .9 -8 asynchronousl
Page 139 and 140: collimated coherent light. A simple
Page 141 and 142: power of the film and associated op
Page 143 and 144: samples simultaneously onto the sam
Page 145 and 146: outputs is assumed. COMPOSITE SIGNA
Page 147 and 148: SPECTRUM I n LINES M n LINES U SPEC
Page 149 and 150: signal andyet have a tolerable fals
Page 151 and 152: i --_- i i i i large values of n. T
Page 153 and 154: plottedin Figure11-15for various va
Page 155 and 156: All the1Fsignalswillarrivein phasei
Page 157 and 158: x:(1 +x) x 2 - _ -- (53) If we wish
Page 159 and 160: 3's = unitcostof signal planelectro
Page 161 and 162: where0ma x is the maximum value of
Page 163 and 164: Roughestimates of the costs of buil
Page 165 and 166: 12. CYCLOPS AS A BEACON Although th
Page 167 and 168: 13. SEARCH STRATEGY The high direct
Page 169 and 170: distantgalaxies (oraninertialrefere
Page 171 and 172: wouldfollowtheuppermost linein Figu
Page 173 and 174: persquaredegreeof fieldwouldberequi
Page 175: starsfrom/'18 to G5 could support a
Page 179 and 180: Only a few such galaxies have been
Page 181 and 182: 15. CONCLUSIONS AND RECOMMENDATIONS
Page 183 and 184: perhapsdecadesand possiblycenturies
Page 185 and 186: APPENDIX A ASTRONOMICAL DATA DISTAN
Page 187 and 188: PLANETARY Planet ORBITS Semimajor S
Page 189 and 190: APPENDIX B SUPERCIVILIZATIONS AND C
Page 191 and 192: ABIOLOGICAL CIVILIZATIONS Many writ
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Page 195 and 196: tqOT APPENDIX C OPTIMUM DETECTION A
Page 197 and 198: to rmsnoise.Wenotethatthematchedfil
Page 199 and 200: APPENDIX D SQUARE LAW DETECTION THE
Page 201 and 202: If the output filter is very wide c
Page 203 and 204: if B/2 > T we can start instead wit
Page 205 and 206: Let us now introduce the normalized
Page 207 and 208: where h-- = expectation count of si
Page 209 and 210: APPENDIXE RESPONSE OF A GAUSSIAN FI
Page 211 and 212: APPENDIXF BASE STRUCTURES AZ-EL BAS
Page 213 and 214: ack,it shouldnotbenecessary to prov
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Page 219 and 220: PAGE BLANK NOT APPENDIX H POLARIZAT
Page 221 and 222: APPENDIX I CASSEGRAINIAN GEOMETRY C
Page 223 and 224: APPENDIXJ PHASINGOFTHE LOCALOSCILLA
Page 225 and 226: 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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