1987 Statistics

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NATIONAL RADIO ASTRONOMY OBSERVATORY Observing Summary - 1987 Statistics

February 1988 © NRAO/AUI NATIONAL RADIO ASTRONOMY OBSERVATORY

Observing Summary 1987 Statistics

February 1988 Some Highlights of the 1987 Research Program

The first VIA radar experiment was carried out in 1987 when echoes from Saturn's Rings were received in the spectral line mode and mapped in the D array. With only 9 antennas outfitted with X-band receivers to detect the signal transmitted from the Goldstone 64-m antenna, the crude radar echo map clearly demonstrated the power of the technique. Aperture synthesis radar provides a clear advantage over conventional planetary radar by providing a direct, unambiguous mapping of the radar signal.

The existence of a very faint counterjet in the classical double-lobed radio galaxy, Cygnus A, was discovered when a significant increase in computing power was applied to existing VIA data. The counterjet is at least four times fainter than the original jet, and the radial brightness variations (knots) in both jets are not symmetric.

The sky at 6-cm wavelength was recorded at two different epochs with the Green Bank 300-ft antenna to a background noise level of 4 mJy. Over the 6 - -2° to +77° region, the maps will provide a standard reference of the radio sky for many purposes, including: multi-waveband radio identifications of discrete sources, multi-epoch radio variability surveys, detailed studies of very extended radio sources, and for studies of the isotropy and large-scale homogeneity of the Universe at large redshift.

The presence of the sulfur-containing molecules C2S and C3S in cold, dark clouds was confirmed with the 140-ft telescope. The ground-state centimeter-wavelength transitions were found in all of the dust clouds that were surveyed. The fact that C3S appears to be more abundant than C3O, even though 0 is more abundant than S, points to significant differences between oxygen and sulfur chemistry in cold clouds.

The most distant and luminous source of carbon monoxide line emission yet detected was found using the 12-m telescope and its sensitive new SIS receiver. The CO found at the redshift of the ultra-luminous IRAS galaxy 14348-1447 indicates a molecular hydrogen abundance of 6x10-'-^ solar masses, a value which is approximately 20 times that of the molecular gas content of the Milky Way.

Extensive multifrequency, multi-configuration VLA observations have mapped in detail the rotation measure across the extent of the prominent extragalactic radio source Cygnus A. The observations provide evidence for magnetic fields on scales of hundreds of kiloparsecs. The fields are thought to originate in the intracluster gas in which Cygnus A is imbedded, and simple models allow for magnetic field strengths of from 2 to 10 pG. Observing Hours

1977 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 Calendar Year

1300-Foot \MO-Foot W^12-Meter EH Interferometer \ \VLA

Fig. 1. This figure shows the hours scheduled for observing on each telescope during the last decade. Distribution of Scheduled Observing Time

12-Meter 140-Foot 300-Foot VLA

1978 79 80 81 82 83 84 85 86 87 1978 79 80 81 82 83 84 85 86 87 1978 79 80 81 82 83 84 85 86 87 1981 82 83 84 85 86 87 Calendar Year Calendar Year Calendar Year Calendar Year

\NRA0 Staff Visitors | Testing and Calibration

Fig. 2. These graphs show the number of hours scheduled for calibration and for observing by the NRAO staff and by visitors on each telescope system during the last decade. 12-Meter Radio Telescope Summary

1978 1979 1980 1981 1982 1983 1984 1985 1986 1987 Calendar Year

Observing Installation, Maintenance and Calibration Equipment Failure, Weather and Interference

Fig. 3. This summary for each quarter of the calendar year shows the percentage of time the telescope was scheduled for observing, for routine calibration, maintenance, and installation of new experiments, and the percentage of time lost due to equipment failure, bad weather, and radio interference. The telescope is removed from service for a period of 4-6 weeks each summer during the wet season. This period is used for maintenance and upgrading of the instrument. During the last half of 1982 and most of 1983, the telescope was out of service for the replacement of the reflecting surface and its backup structure. 140- Foot RadicI Telescope Summary 100

/"- ^ ^ /" ^ /\ A ^S /^ U- ^- ^ ^^ \ ^\ y \ XV , / k . /- V 1 ^v 80 V / v ) /" V ^s ^ ^ "l /- /^ V ^ / V i — 60 V v/ ^—i a> V o - - JP ^ 40 / ' A - K A / - 20 -w J -A v 7 \ ^s ^- / A 7^ \ ^ z' \^ ^\ J v y -^ V 7^ y \_ V v. ■*»< ^ ^ ^^ —<» _, ._„_ .^^^ " > xX ^^ **«» o 'N.- ^- ».•'

Calendar Year

Observing Installation, Maintenance and Calibration Equipment Failure, Weather and Interference

Fig. 4. This summary for each quarter of the calendar year shows the percentage of time the telescope was scheduled for observing, for routine calibration, maintenance, and installation of new experiments, and the percentage of time lost due to equipment failure, bad weather, and radio interference. Major improvements to the telescope system include: 1980 - installation of the Model IV autocorrelation receiver; 1982 - beam efficiency and pointing tests at 1.3 cm; 1983 - brake overhaul and installation of the second channel of the upconverter/maser receiver; 1987 - holographic surface tests and panel readjustments. 300-Foot Radio Telescope Summary 100 1 I -^ ^s ^ — s- "S r "N -i - ^-\ — /" "> x V \J _> ,/* A / J sx 80 r \y\r A \ \ - / 1 - ^ 60 1 L j - V V - 40 - - L A 20 > A N /\ k k A y ^ ^N -_ / i y V_ N \- \- —■ ^ ^ i V -■ —. ^ ^ - j *>. - ■—<—-+— ^ \ Oh^T; "1

Calendar Year

Observing Installation, Maintenance and Calibration Equipment Failure, Weather and Interference

Fig. 5. This summary for each quarter of the calendar year shows the percentage of time the telescope was scheduled for observing, for routine calibration, maintenance, and installation of new experiments, and the percentage of time lost due to equipment failure, bad weather, and radio interference. During 1980 a new traveling feed was installed, in 1983 cables were replaced and the telescope was painted, during 1985 N-S motion was added to the traveling feed, and in 1986 a new 6 cm, seven-feed receiver was installed and tested. Very Large Array Telescope Summary

Construction Initial Observing and Testing Testing, Maintenance and Calibration Downtime

Fig. 6. This summary for each quarter of the calendar year shows the percentage of time the telescope was scheduled for observing, for routine system testing, maintenance, and calibration and the percentage of time lost due to hardware or software failure, power failure, or bad weather. During 1977 and 1978 no distinction was made between astronomical and test observing. Time scheduled for completion of the construction was reduced to zero after the first quarter of 1981. Full-Time Permanent Employees 450

400 ffifaVLA Construction 350 §■ Research and Operations ni\VLB/l Construction 300

&250 o g 200 .■■■I

150

100

0 I 1957 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 v w Fiscal Year Calendar Year

Fig. 7. This figure shows the total number of NRAO full-time, permanent employees at the end of each year, projected into the future. Number of People Observing With NRAO Telescopes 900

1959 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 90 91 Calendar Year

Fig. 8. This bar chart shows for each calendar year the number of NRAO permanent research staff and the number of research associates who use the telescopes. In addition, it shows the total number of visitor-users of NRAO telescopes and the number of institutions from which the NRAO visitors come. The significant jump in these last two categories for 1981 reflects the increased use of the VLA. Distribution of Telescope Time by Percent

12-m 140-ft 300-ft VLA 1987 Summary

Visitors 46Z 60% 61X 56X 56X

Students 10% 8% 16% 7X 10X

Permanent Staff 10X HZ 9Z 9% 10%

Research Associates IX 2X IX 2X 2X

Tests and Calibrations 10X 12X 4X 14X 10X

Maintenance and Installation 22X 6% 8X 11X 11X

Holidays and Unscheduled IX IX IX IX IX

10 Distribution of Scheduled Observing Programs in Various Research Areas, by Percent

12-m 140-ft 300-ft VLA Overall

I. SOLAR SYSTEM --

Sun, Planets, Satellites, and Comets IX 3X OX 5X 2X

II. STELLAR -

Pulsars, X-ray Sources, Planetary Nebulae, 11X 15X 14X 29X 17X Circumstellar Shells, Supernova Remnants, Masers, Novae, Supernovae, and Stars

III. GALACTIC

Galactic Structure, Center, Molecular 61X 31X 10X 21X 31X Clouds, HII Regions, Star Formation, Molecules, and Interstellar Medium

IV. EXTRAGALACTIC --

Normal and Active Galaxies, Radio Galaxies, 27X 51X 76X 45X SOX Clusters, Quasars, VLB Studies, Extra- galactic Molecules, and Cosmology

11 Institutions from which Visitors Came to Use NRAO Telescopes during 1987

Telescopes Institution 140-ft 12-m 300-ft VLA

1. Anglo Australian Observatory x 2. American Institute of Physics (N.Y.) x 3. Applied Research Corporation x x 4. Arcetri Astrophysical Observatory (Italy) x x 5. Arizona, U. of - Steward Obs., L & P Lab. x x x x

6. Arizona State University x x 7. Barcelona, U. of (Spain) x 8. Beijing Astronomical Observatory (P.R. of China) x 9. Bell Laboratories (New Jersey) x x 10. Bentley College (Waltham, MA) x x

11. Bologna, U. of (Italy) x x 12. Bonn U. (FRG) x 13. Bordeaux Observatory (France) x 14. Boston University x x 15. Brandeis University x x

16. British Columbia, U. of (Canada) x x 17. Brookhaven National Laboratories x 18. Bureau de Longitudes (Paris) x 19. Byurakan Astrophysical Observatory (USSR) x 20. Calgary, U. of (Canada) x

21. California, U. of, Davis x 22. California, U. of, Berkeley - Hat Creek Obs. x x x x 23. California, U. of, Los Angeles x x x 24. California, U. of, San Diego x x 25. California, U. of, Santa Cruz - Lick Obs. x — Telescopes Institution 140-ft 12-m 300-ft VLA

26. Caltech - OVRO, Mt. Palomar x x x x 27. Cambridge University - Cambridge, Mullard, IOA x x 28. Carleton College x 29. Catania University (Italy) x 30. CFA (Harvard + SAO) x x x

31. Centre National D'Etudes Spatiales (France) x 32. CNRS, France x 33. Chalmers - Onsala Space Observatory (Sweden) x x x 34. Chicago, U. of - Yerkes Observatory x x 35. CSIR (Johannesburg, South Africa) x x

36. Colgate University x x 37. Colorado, U. of - JILA (Boulder) x x x 38. Columbia University x 39. Computer Tech. Associates x x 40. Cornell University x x x

41. CSIRO (Australia) x x 42. CTIO (Cerro Tololo Inter. Observatory) x 43. Dartmouth College x 44. DAO (Dominion Astrophysical Observatory) x 45. DRAO (Dominion Radio Astrophysical Observatory) x x

46. Delaware, U. of x 47. Delft University of Technology (Netherlands) x x 48. DIM - Carnegie Institution x 49. Duke University x 50. Durham, U. of (U.K.) x

13 Telescopes Institution 140-ft 12-m 300-ft VLA

51. Ecole Normale Superieure (Paris) x x 52. Edinburgh, U. of (Scotland) x x 53. ESA (European Space Agency, Spain) x 54. ESO (European Southern Observatory - FRG, Chile) x x 55. ESOC (Damstadt, FRG) x

56. ESTEC (Netherlands) x 57. Florida, U. of x 58. Georgia State University x 59. Georgia Tech x 60. George Mason University x

61. Glasgow, U. of (U.K.) x 62. Grenoble, U. of x 63. Groningen, U. of - Kapteyn Lab x 64. Hamburger Sternwarte (FRG) x 65. Haverford College x

66. Hawaii, U. of - Institute of Astronomy x 67. Haystack Observatory - NEROC x x x x 68. Heidelberg Observatory x 69. High Altitude Observatory x 70. Hofstra University x

71. IBM x 72. IAR, Buenos Aires (Argentina) x 73. lAS-Frascati (Italy) x 74. Illinois, U. of - Vermillion River Observatory x x x 75. Indiana, U. of x x

14 Telescopes Institution 140-ft 12-m 300-ft VLA

76. Institut Geographique National (France) x 77. Institute of Astrophysics (Granada) x 78. Institute of Astrophysics (Paris) x 79. Institute for A & A, Andalucia x 80. Institute for Space Research (USSR) x x

81. Interferometrics, Inc. x x 82. Iowa, U. of x x 83. Iowa State University x 84. IPAC, Pasadena x 85. IRAM (France; Spain) x x x

86. Johns Hopkins University - Space Tel. Sci. Inst. x x x x 87. JPL - Goldstone x x 88. Kent, U. of (U.K.) x 89. Kentucky, U. of x x 90. Krakow, U. of (Poland) x

91. KPNO - NOAO x 92. La Plata Jr. High (New Mexico) x 93. Laguna, U. of (Spain) x 94. Laval, U. of (Canada) x x 95. Leicester, U. of (U.K.) x x

96. Leiden, U. of - Huygens Labs x x 97. Leige, U. of (Belgium) x 98. Lille, U. de (France) x x 99. Lockheed Research Laboratory x x 100. Los Alamos Scientific Laboratory (LANL) x

15 Telescopes Institution 140-ft 12-m 300-ft VLA

101. Louisiana State University x 102. Lowell Observatory x x 103. Manchester, U. of - Jodrell, Nuffield x x 104. Marseille Observatory x 105. Maryland, U. of - Clark Lake Observatory x x x x

106. Massachusetts, U. of - Five College Observatory x x x x 107. Meudon Observatory x x x 108. Mexico, U. of - Institute of Astronomy x x 109. Michigan, U. of x x x x 110. Minnesota, U. of x x

111. Missouri, U. of (at St. Louis) x x 112. MIT - Lincoln Laboratories x x x 113. MPI (Heidelberg, FRG) x 114. MPIPA (Munich, FRG) x x 115. MPIR (Bonn, FRG) x x x x

116. Mt. Stromlo Observatory (Australia) x 117. Mt. Wilson & Las Campanas - Carnegie x x 118. NAIC - Arecibo Observatory x x x 119. Nanjing Observatory x 120. Nanking, U. of (P.R. China) x

121. NASA/GSFC - Goddard x x x 122. NBS (National Bureau of Standards) x 123. NFRA (Netherlands Found, for Radio Astronomy) x x x 124. NMIMT (New Mexico Inst, of Mining & Technology) x 125. New Mexico, U. of x

16 Telescopes Institution 140-ft 12-m 300-ft VLA

126. New Mexico State University x 127. New York University x 128. Nobeyama Observatory (Japan) x x 129. Nigeria, U. of x 130. North Carolina, U. of x

131. North Carolina State University x 132. Northeastern University x 133. Northwestern University x 134. NRC - Algonquin, Herzberg x x x 135. NRL (Naval Research Laboratories) x x x x

136. Oklahoma, U. of x 137. Oregon, U. of x 138. Oxford University (U.K.) x 139. Paris Observatory x 140. Peking Observatory x

141. Penn State University x 142. Pennsylvania, U. of x 143. Pittsburgh, U. of - Allegheny Observatory x x 144. Preston/Lancashire Polytechnic (U.K.) x x 145. Princeton University - Inst, for Advanced Studies x x x x

146. Puerto Rico University x x x 147. Queen Mary College (U.K.) x x 148. Queens University (Canada) x 149. Raman Institute (India) x 150. Rensselaer Polytechnic Institute x x x

17 Telescopes Institution 140-ft 12-m 300-ft VLA

151. Rice University x 152. Rikkyo University (Japan) x 153. Rochester, U. of x 154. Royal Greenwich Observatory (U.K.) x 155. Royal Observatory - UKIRT (Scotland) x

156. Rutgers State University x 157. Sandia Laboratories x 158. Shanghai Observatory x 159. South African Astron. Obs. (SAAO, Cape Town) x 160. Stanford University - Inst. Plasma Research x

161. Stockholm Observatory x 162. SUNY (all campi) x 163. SFIT - Swiss Federal Institute of Technology x 164. Sydney, U. of (Australia) x 165. Systems & Applied Science Corporation x x

166. Tata Institute - TIFR, RAC (India) x x 167. Texas, U. of - McDonald Observatory x x 168. Thessalonike University (Greece) x 169. Torino University (Italy) x 170. Toronto, U. of - David Dunlap Observatory x x

171. Trieste Astronomical Observatory x 172. Tufts University x 173. Turku, U. of (Finland) x x 174. University College London x 175. (unaffiliated) x

18 Telescopes Institution 140-ft 12-m 300-ft VLA

176. USNA - United States Naval Academy x 177. USNO - United States Naval Observatory x 178. Utrecht, U. of - Astronomical Inst. (Netherlands) x 179. Utsunomiya University (Japan) x 180. Vassar College x

181. Victoria, U. of (Canada) x 182. Virginia, U. of x x x 183. VPI & SU xx 184. Waterloo, U. of (Canada) x x 185. Wellesley College x

186. Williams College x 187. Wisconsin, U. oiof - Washburn Observatory x x x 188. Wyoming, U. of x 189. Yale University

No. of Institutions 66 53 22 165

No. of Visitors 181 120 35 545 No. of Students 21 22 10 83 No. of Research Associates 2 1 1 7 No. of Permanent Staff

Total Observers 226 152 50 666

All told, 787 visitors, including 111 students, from 189 institutions.

19 NRAO Student Program

1959 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 81 82 83 84 85 86 87 88 89 Calendar Year

Fig. 9. This figure shows for each calendar year the number of Ph.D. students (salaried and non-salaried), co-op students, and summer undergraduate and graduate students who observed or worked at the NRAO during that year. Beginning in 1987 the majority of the undergraduate summer students were funded by a separate NSF Grant for Research Experiences for Undergraduates.

20 NRAO Front-End Box Status TECHNICAL DATA SHEET No. 12 OCTOBER 1987 Page 1 of 4

SYSTEM 3 dB PERSON(S) RECEIVER APPUCABLE FREQUENCY AMPUFIER CALIBRATION SWITCHING nEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS IN NAME TELESCOPE (GH2) TYPE VALUE SYSTEM (KELVIN) (MHz) CHARGE

300 FT SINGLE 25-50 FAT DICKE SWITCH: CAN ONLY BE INSTALLED ON 300* TRAVELING 25 LINEAR MHz DIPOLE REFERENCE FEED E-W TRAVELING FEFD. HIGH TEMPERATURE ADJUSTABLE DYNAMIC OPEN 300 ORTHOGONAL FROM 50-88 RANGE SI£FVE 38 LINEAR 100 TO 100.000K MHz TRANSISTOR + Taky CROSSED FEFD CHANGES FROM 50-88 MHz TO COE 300 FT DUAL DIPOLE OB. ADJUSTABLE 110-240 MHz OR TO 450-500 MHz 25-250 MHz REMOVABLE OR TRAVEUNG CHANNEL 2 TO 2500K REQUIRE TWO HOURS ON THE 140* Rx QUAD HYBRID (OLIVER) FEED BROADBAND AND THREE HOURS ON THE 300'. 110-240 AT FEED FOR FREQUENCY MHz 130 CROSSFD SWITCH OB. DIPOLE RCP AND LCP 140 FT CAMTY RCP 450-500 FET BACKED FREQUENCY 50-80 50 AND 450-500 MHz AMP IN 25-250 MHz Rx MHz AMP CROSSFD SWITCH LCP DIPOLE

280-350 280-350 WHEN INSTALLED ON THE Xff TRAVEUNG COOLED UP- MHz 70 350-410 FEED. TWO FFFDS CAN BE USED: THE CONVERTER/ 450-500 750-1000 MHz ON THE VEST END OF THE GASFET AMP 45-85 CAVITY BOX AND ONE OF THE OTHERS ON THE EAST 350-420 DUAL BACKED END. SELECTION OF ONE OF THE TWO FEEDS 300 FT 60 MHz CHANNEL CROSSED DUAL SHOULD TAKE LESS THAN FIVE MINUTES. TO 1RAVEUN6 Dff>OLES ORTHOGONAL CHANGE A FEED REQUIRES THREE HOURS. FEED 460-500 UNEAR 300-1000 COOLED UP- 500-750 WHEN INSTAU.FD IN THE STERLING MOUNT ON COE C0NVER1ER/ 50 FREQUENCY MHz Rx flfi MHz SCALAR 5K SWITCHING THE 140* OR 300* ANTENNAS. ONLY ONE OF GASFET AMP 50-70 WITH IF POLARIMETER THE FIVE FEEDS (SHANK) OR RF HYBRID 300^140 FT 500-750 DUAL CROSSFD 280-350 MHz 250 FOR RCP STERLING MHz CHANNa DtPOLES 350-420 MHz AND LCP MOUNT 450-500 MHz COOLED UP- 750-1000 500-750 MHz OR 750-1000 CONVERTER/ SCALAR 750-1000 MHz 50-60 250 MHz GASFET AMP WITH CAN BE USED. TO CHANGE FEEDS REQUIRES DUAL CROSSED TWO HOURS ON THE 140* AND THREE HOURS CHANNa DIPOLES ON THE 300*.

COOLED SINGLE FREQUENCY 1.00-1.45 FET ORTHOGONAL 35-40 450 BEAM 4K TO 6K SWITCHING (25 CM) DUAL UNFAR SCALAR CHANNa NOISE ADDING FEED CHANGE REQUIRED TO SWITCH BANDS. COE 6/25 CM ORTH CIRCULAR OTHER 300/140 FT SINGLE BEAM 1.4K THIS TAKES TWO HOURS ON THE 140* AND Rx COOLED OR ORTH LINEAR POLARIZATION THREE HOURS ON THE 300*. (SHANK) 4.47-5.05 GAShtl 50-60 580 DUAL BEAM IDENTICAL OR OR (6 CM) DUAL ORTH CIRCULAR CHANNa OFFSET BEAM SWITCHING 3 HPBW OR IDENTICAL 12.8K UNEAR

21 TECHNICAL DATA SHEET No. 12 OCTOBER 1987 Page 2 of 4

SYSTEM 3 dfl PERSON(S) RECEIVER APPUCABLE FREQUENCY AMPLIFIER CALIBRATION SWITCHING TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS IN NAME TELESCOPE (GHz) TYPE VALUE SYSTEM (KELVIN) (MHz) CHARGE

FREQUENCY THREE 2HE 2K EITHER CIRCULAR OR UNEAR POLARIZATIONS DUAL UP TO 120 SINGLE BEAM ORTHOGONAL OR ARE SELECTABLE. ORCULAR POLARIZATION LINEAR POLARIZATION NORROD 1.3-1.8 GHz 300/140 FT 1.30-1.80 CHANNa 19-25 AND REQUIRES ADJUSTMENTS FROM THE CONTROL Rx COOLED FET FEED 1.30-1.36 OR SWITCHING ROOM. BAND CHANGE REQUIRES 2 TO 3 LIMITED ORCULAR (CHESTNUT) 1.36-1.43 200K OR HOURS. OBSERVATIONS OUTSIDE STATED FEED 1.60-1.72 NOISE ADDING BANDS POSSIBLE AT REDUCED EFFICIENCIES.

UNCOOLED CIRCULAR CONTINUUM RECOVER. ON-AXIS HORN HAS 11 CM. 110 DSB 300 K LOAD OR NORROD 300/140 FT 2.64-2.75 GASFET 130 3 HORNS OR 4K POLARIZATION RECOVERS ON BOTH POLARIZATIONS. FOUR 3-FEED Rx (IF 5-55) HOURS TO CHANGE POLARIZATION. FIXED 4 CHANNEL UNEAR OR BEAM (CHESTNUT) LO AT 2.695 GHz. BAND CHANGE REQUIRES FEED CHANGE. THIS DUAL UP TO 250 TWO 2HE SINGLE BEAM TAKES 2-3 HOURS. CIRCULAR POLARIZATION 2.9-3.4 CHANNa 25-35 2.90-3.15 REQUIRES PHASE EQUALIZATION ADJUSTMENTS COOLED FET FEED LIMITED 3.15-3.40 ORTHOGONAL FROM THE CONTROL ROOM. FREQUENCY LOW 1.8 FREQUENCY SMTCHING REQUIRES 50 MS BLANKING TIME. BEHRENS 2-5 GHz 300/140 FT LINEAR SWITCHING OR Rx HIGH 150 NOISE ADDING BAND CHANGE REQUIRES FEED CHANGE. THIS UP TO 200 CIRCULAR (CHESTNUT) DUAL ONE 2HE TAKES 2-3 HOURS. LINEAR POLARIZATION 4.6-5.0 CHANNa 25-35 SINGLE BEAM FEED REQUIRES PHASE EQUAUZATION ADJUSTMENTS COOLED FET LIMITED 4.6-4.8 FROM THE CONTROL ROOM. FREQUENCY SMTCHING REQUIRES 50 MS BLANKING TIME.

COOLED DICKE IDENTICAL SWTCHES (LATCHING 65 K LOAD COOLED DUAL BEAMS LINEAR 4K FERRITE) FOR LOAD SMTCHED 250 OFFSET BY OR (20K) SMTCHING OR 9 CM Rx 300/140 FT 3.12-3.37 PARAMPS FIXED DUAL 3 HPBW IDENTICAL AND BEAM SWITCHING CONTINUUM USE. BEHRENS 75 K BEAM TUNED CHANNa SINGLY CIRCULAR WITH NOISE SWITCHED POLARIZED OR 14K INJECTION FOR ORTH CIRCULAR BALANCING; 10 Hz MAXIMUM RATE.

COOLED 7 6 CM. FET CORRUGATED 300/140 FT 4.6-5.1 60-70 500 DUAL 5K CONTINUUM USE ONLY. 7-FEEDRx FOURTEEN HORNS CIRCULAR NONE BEHRENS 3 HPBW TOTAL POWER RF DETECTION. CHANNa APART

FRfflUENQY T*]*z 4.7-7.2 UPCONVERTER 30-50 60-300 CASSEGRAIN FIXED LINEAR 3-7K FREQUENCY OR CIRCULAR VLB NUTATOR BEAM 4.7-4.9 40-50 MAStR 4.9-6.5 30-40 6.5-7.2 40-50 UPCONVERTER FIXED LINEAR 140 FT 7.6-11.2 35-80 60-300 CASSEGRAIN 3-7K FREQUENCY OR 7.6-8.5 50-80 CASSEGRAIN MASER ORCULAR VLB NUTATOR BEAM 8.5-11.2 35-45 BROCKWAY UPCONVERTER FREQUENCY OR A AND B 12-16.2 50-80 60-300 CASSEGRAIN FIXED LINEAR 3-7K 12.0-16.2 50-80 MAStR NUTATOR BEAM (DUNBRACK) RECEIVERS FIXED UNEAR FREQUENCY OR 18.2-25.2 MASER 40-70 60-300 CASSEGRAIN 2-6K 18.2-25.2 40-70 ORCULAR VLB NUTATOR BEAM

22 TECHNICAL DATA SHEET No. 12 OCTOBER 1987 Page 3 of 4

RECEIVER CONTINUUM 3 dB PERSON(S) APPUCABLE FREQUENCY AMPURER CALIBRATION SWITCHING TEMPERATURE SENSITIVITY BANDWIDTH FEED TYPE POLARIZATION REMARKS IN TELESCOPE (GHz) TYPE VALUE SYSTEM (KELVIN) [JANSKY y/SR] (MHz) CHARGE

COOLED 260-400 DUAL NUTATING 12 M 70-115 1.0 600 MHz HORN-LENS 10 K PAYNE MIXER SSB UNEAR SUBREFLECTOR

APPROX. TO BE DUAL NUTATING 12 M 90-115 SIS 600 MHz HORN-LENS 10 K LAMB 100 MEASURED UNEAR SUBREFLECTOR

COOLED 1400-2000 SINGLE NUTATING 12 M 330-360 12 600 MHz HORN-LENS PAYNE MIXER SSB UNEAR - SUBREFLECTOR

23 TECHNICAL DATA SHEET No. 12 OCTOBER 1987 Page 4 of 4

SYSTEM 3 dB PERSON(S) APPUCABLE FREQUENCY AMPURER CALIBRATION SMTCHING TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS IN TELESCOPE (MHz) TYPE VALUE SYSTEM (KELVIN) (MHz) CHARGE

3 MHz DUAL NOSE INJECTION. 308- UNCOOIED PRIME VLA 150 (LIMITED BY ORTHOGONAL 10 9.6 Hz. ON 21 ANTENNAS AS OF OCTOBER 1987. UUE 343 TRANSSTER FOCUS INTERFERENCE] ORCULAR 50 PERCENT CYCLE.

DUAL NOSE INJECTION. 1340- COOLED VLA 60 55 CASSEGRAIN ORTHOGONAL 4 9.6 Hz. UUF 1730 FET CIRCULAR 50 PERCENT CYCLE.

COOLED 4500- PARAMP OR DUAL NOSE INJECTION. VLA COOLED 60 55 CASSEGRAIN ORTHOGONAL 4 9.6 Hz. 5000 UUE PARAMP AND ORCULAR 50 PERCENT CYOF. FET

DUAL NOISF INJECTION. 8000- COOLED V1_A 45 55 CASSEGRAIN ORTHOGONAL 4 9.6 Hz. ON 14 ANTENNAS AS OF OCTOBER 1987. UUE 8800 HEMT CIRCULAR 50 PERCENT CYCLE.

DUAL NOSE INJECTION. 14400- COOLED VLA 110 55 CASSFGRA1N ORTHOGONAL 7 9.6 Hz. UUF 15400 FET ORCULAR 50 PERCENT CYCLE.

DUAL NOSE INJECTION. 22000- COOLED VLA 350 55 CASSEGRAIN ORTHOGONAL 20 9.6 Hz. UUE 24000 MIXER ORCULAR 50 PERCENT CYCLE.

24 NRAO-Staff and Visitor Publications 1987

Alexander, P. "A Study of Spectral Ageing in the Radio Galaxy 3C 234 and Its Implications." Mon. Not. Rov. Astron. Soc.. 225. 27-42, 1987.

Alexander, P. and Leahy, J. P. "Ageing and Speeds in a Representative Sample of 21 Classical Double Radio Sources." Mon. Not. Rov. Astron. Soc. 225. 1-26, 1987.

Altschuler, D. R.; Dennison, B. K.; Mitchell, K. J.; O'Dell, S. L.; Broderick, J. J.; Condon, J. J.; and Payne, H. E. "The Low Frequency Variability of Extragalactic Radio Sources." IAU Svmp.. 121. 211-214, 1987.

Altschuler, D. R. and Forkert, G. "Variable Objects in a Complete Sample of Faint Radio Sources." IAU Svmp.. 121. 207-210, 1987.

Andre, P.; Montmerle, T.; and Feigelson, E. D. "A VLA Survey of Radio-Emitting Young Stars in the Rho Ophiuchi Dark Cloud." Astron. J.. 93, 1182-1198, 1987.

Apple ton, P. N.; Ghigo, F. D.; van Gorkom, J. H.; Schombert, J. M.; and Struck-Marcell, C. "A Giant Intergalactic H I Bubble Near Arp 143." Nature. 330. 140-142, 1987.

Arendt, R. G. and Dickel, J. R. "Resolution of Compact Knots in Cassiopeia A." Astrophvs. J.. 315. 567-570, 1987.

Arquilla, R.; Kwok, S.; and Leahy, D. A. "CO Observations of IRAS Sources with SiC Emission Features." In: Late Stages of Stellar Evolution. Ed. S. Kwok and S. R. Pottasch. (Dordrecht: Reidel, 1987) 141-142.

Baan, W. A. and Haschick, A. D. "The 18 Centimeter Emission of IC 4553 (Arp 220)." Astrophvs. J.. 318. 139-144, 1987.

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Wehrle, A. E. and Morris, M. "An Unusual Radio Loop in the Edge-on Seyfert Galaxy NGC 5506." Astrophvs. J.. 313. IA3-L46, 1987.

Weinreb, S. "Cooled-HEMT Microwave Front-Ends for Space Astronomy." NRAO Wksp. Proc.. 18. 191-194, 1987.

Weinreb, S. "SIS Mixer to HEMT Amplifier Optimum Coupling Network." IEEE Trans. Micro. Theory Tech.. MTT-35, 1067-1069, 1987.

Weistrop, D.; Wall, J. V.; Fomalont, E. B.; and Kellermann, K. I. "A Deep 6-Centimeter Radio Source Survey: Optical Identifications." Astron. J.. 21. 805-810, 1987.

Welch, W. J.; Dreher, J. W.; Jackson, J. M.; Terebey, S.; and Vogel, S. N. "Star Formation in W49A: Gravitational Collapse of the Molecular Cloud Core Toward a Ring of Massive Stars." Science. 238. 1550-1555, 1987.

47 Welty, A. D.; Fix, J. D.; and Mutel, R. L. "The Distribution of Maser Emission in OH/IR Stars." Astrophvs. J.. 318. 852-867, 1987.

Whiteoak, J. B.; Gardner, F. F.; Forster, J. R.; Palmer, P.; and Pankonin, V. "Masers in Sgr B2: Sites of Star-Forming Regions." IAU Svmp.. 115. 161-163, 1987.

Wilking, B. A. and Claussen, M. J. "Water Masers Associated with Low-Mass Stars: A Survey of the Rho Ophiuchi Infrared Cluster." Astrophvs. J.. 320. L133-L137, 1987.

Wilkinson, A.; Browne, I. W. A.; Kotanyi, C; Christiansen, W. A.; Williams, R.; and Sparks, W. B. "Radio Emission from Shell Elliptical Galaxies." Mon. Not. Rov. Astron. Soc. 224. 895-910, 1987.

Williams, B. A. and Rood, H. J. "Neutral Hydrogen in Compact Groups of Galaxies." Astrophvs. J. SUPPI. Ser.. il, 265-294, 1987.

Willson, R. F. and Lang, K. R. "Multiple Wavelength Microwave Observations of the RS Canum Venticorum Stars UX Arietis, HR 1099, HR 5110 and II Pegasi." Astrophvs. J.. 312. 278-283, 1987.

Wilson, A. S. and Ulvestad, J. S. "A Radiative Bow Shock Wave (?) Driven by a Nuclear Ejecta in a Seyfert Galaxy." Astrophvs. J.. 319. 105-117, 1987.

Wootten, A. "Deuterated Molecules in Interstellar Clouds." IAU Svmp.. 120. 311-319, 1987.

Wootten, A. and Lor en, R. B. "L1689N: Misalignment Between a Bipolar Outflow and a Magnetic Field." Astrophvs. J.. 317. 220-230, 1987.

Wrobel, J. M. "VLA Polarimetry of the Active Galaxy 3C 371." In: Superluminal Radio Sources. Ed. J. A. Zensus and T. J. Pearson. (Cambridge: Cambridge University Press, 1987) 186-192.

Yin, Q.; Heeschen, D. S.; and Heidmann, J. "The Envelope Emission of Markarian 8." Sci. Sinica Ser. 4., 10, 1075-1080, 1987.

Yusef-Zadeh, F. and Bally, J. "A Non-Thermal Axially Symmetric Radio Wake Towards the Galactic Centre." Nature. 330. 455-458, 1987.

Yusef-Zadeh, F. and Morris, M. "GO.18-0.04: Interaction of Thermal and Nonthermal Radio Structures in the Arc Near the Galactic Center." Astron. J.. 9U, 1178-1184, 1987.

48 Yusef-Zadeh, F. and Morris, M. "The Linear Filaments of the Radio Arc Near the Galactic Center." Astrophvs. J.. 322. 721-728, 1987.

Yusef-Zadeh, F. and Morris, M. "Structural Details of the Sagittarius A Complex: Evidence for a Large- Scale Poloidal Magnetic Field in the Galactic Center Region." Astrophvs. J.. 320. 545-561, 1987.

Yusef-Zadeh, F.; Morris, M.; and van Gorkom, J. H. "Spatial and Kinematic Structure of the Thermal Components of the Galactic Center Arc." In: The Galactic Center. Ed. D. C. Backer. (New York: American Institute of Physics, 1987) 190-195.

Ziurys, L. M. "Detection of Interstellar PN: The First Phosphorus-Bearing Species Observed in Molecular Clouds." Astrophvs. J.. 321. L81-L85, 1987.

Ziurys, L. M. and Turner, B. E. "New Interstellar Molecular Detections: Implications for 'Shock Chemistry'." IAU Svmp. 120. 289-292, 1987.

49 ADDITIONS TO THE 1986 BIBLIOGRAPHY

Comwell, T.J.; Saikia, D.J.; Shastri, P.; Feretti, L.; Giovannini, G.; Parma, P.; and Salter, C.J. "Extragalactic Sources with Asymmetric Radio Structure. II. Further Observations of the Quasar B2 1320 + 299." J. Astrophys. Astron., 2» 119-129, 1986.

Dickey, J.M. and Garwood, R.W. "Cold Atomic Hydrogen in the Inner Galaxy." In: Interstellar Processes: Abstracts of Contributed Papers. Ed. D.J. Hollenbach and H.A. Thronson, Jr. (Moffett Field: NASA, 1986) 79-80.

Gary, D.E. "The Microwave Structure of Quiescent Solar Filaments at High Resolution." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 121-125.

Habbal, S.R. and Harvey, K.L. "Simultaneous Observations of Changes in Coronal Bright Point Emission at the 20 cm Radio and He X 10830 Wavelengths." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 343-347.

Harvey, K.L.; Tang, F.; and Gaizauskas, V. "The Association of Chromospheric and Coronal Phenomena with the Evolution of the Quiet Sun Magnetic Fields." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 359-363.

Hjellming, R.M. and Johnston, K.J. "Radio Emission from X-ray Binaries and the Proto-Type Jets of 88433." In: Physics of Accretion onto Compact Objects. Ed. K.O. Mason, M.G. Watson, and N.E. White. (Berlin: Springer-Verlag, 1986) 287-301.

Kinney, A.L.; Huggins, P.J.; Glassgold, A.E.; and Bregman, J.N. "High Signal-to-Noise Spectra of Two Intermediate Redshift Quasars." In: New Insights in Astrophysics. Ed. E.J. Rolfe. (Paris: European Space Agency, 1986) 610-612.

Kundu, M.R. "High Spatial Resolution Microwave Observations of Solar Flares." In: Solar Terrestrial Physics. Ed. M.R. Kundu et al. (New Delhi: National Physical Laboratory (CSIR), 1986) 159-173.

Kundu, M.R. "Three Dimensional Structures of Solar Active Regions." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 291-295.

Kundu, M.R. "VLA Observations of Coronal Bright Points at 6 and 20 cm Wavelengths." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 349-351.

Kundu, M. "VLA Observations of Solar Filaments at 6 and 20 cm Wavelengths." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 117-120.

50 Lang, K.R. "Coronal Diagnostics." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 279-289.

Lang, K.R. "Coronal Plasmas on the Sun and Nearby Stars." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 309-317.

Lang, K.R. and Willson, R.F. "Compact, Variable, Moving Sources Observed on the Sun at 2 Centimeters Wavelength." In: Coronal and Prominence Plasmas. Ed. A.I. Poland. (Washington: NASA, 1986) 353-357.

Martin, B. and Lada, E. "Pervasive Small-Scale Structure in Molecular Clouds." In: Interstellar Processes: Abstracts of Contributed Papers. Ed. D.J. Hollenbach and H.A. Thronson, Jr. (Moffet Field: NASA, 1986) 23-24.

Moore, P. "An Indexing Algorithm for Large Multidimensional Arrays." In: Data Analysis in Astronomy II. Ed. V. Dl Gesu et al. (New York: Plenum, 1986) 187-192.

Moore, P. "VLA: Methodological and Computational Requirements." In: Data Analysis in Astronomy II. Ed. V. Dl Gesu et al. (New York: Plenum, 1986) 119-126.

Parma, P.; de Ruiter, H.R.; Fanti, C; and Fanti, R. "VLA Observations of Low Luminosity Radio Galaxies. I. Sources with Angular Size Smaller than Two Arcminutes." Astron. Astrophys. SuppI., 64, 135-171, 1986.

Rickett, B.J. and Coles, W.A. "Solar Cycle Evolution of the Solar Wind in Three Dimensions." In: Solar Terrestrial Physics. Ed. M.R. Kundu et al. (New Delhi: National Physical Laboratory (CSIR), 1986) 337-347.

Rodriguez, L.F.; Canto, J.; Escalante, V.; and Moran, J.M. "The Asymmetric Profile of the H76a Line Emission from MWC349." In: Interstellar Processes: Abstracts of Contributed Papers. (Moffett Field: NASA, 1986) 17-18.

Schloerb, P.P.; Claussen, M.J.; and Tacconi-Garman, L. "OH Radio Observations of Comet Halley." In: Exploration of Halley's Comet. Ed. B. Battrick et al. (Noordwijk: European Space Agency, 1986) 583-587.

Schmahl, E.J.; Kundu, M.R.; and Dennis, B.R. "Possible Evidence for Beaming in Flares from Microwave and Hard X-ray Imaging and Spectra." In: The Lower Atmosphere of Solar Flares. Ed. D.F. Neidig. (Sunspot: National Solar Observatory/Sacramento Peak, 1986) 396-408.

Wells, D. "Vector Computers in Astronomical Data Analysis." In: Data Analysis in Astronomy II. Ed. V. Dl Gesu et al. (New York: Plenum, 1986) 315-323.

Willson, R.F. and Lang, K.R. "Simultaneous IDE and VLA Observations of YZ Canis Mlnoris, AD Leonis and Lambda Andromedae." In: New Insights in Astrophysics. Ed. E.J. Rolfe. (Paris: European Space Agency, 1986) 57-60.