NATIONAL RADIO ASTRONOMY OBSERVATORY Observing Summary - 1985 Statistics
February 1986 NATIONAL RADIO ASTRONOMY OBSERVATORY
Observing Summary - 1985 Statistics
February 1986 Some Highlights of the 1985 Research Program
A radio image of the Cassiopeia A supernova remnant showing unprecedented detail was produced, which is the most complex image yet made by a radio-interferometer. Six centimeter observations from all four VLA configurations were combined and deconvolved by means of a supercomputer in order to produce a 0.2 arcsecond resolution image of the large diameter 6.1 arcminute field. Images from future epochs will allow detailed tracking of the expansion of the remnant and monitoring of the compact knots of emission that appear throughout as a result of the catastrophic explosive event that created the remnant approximately 300 years ago.
The 1400-MHz continuum survey of the entire sky within the -5° < 6 < + 82° declination band that was carried out on the 300-ft telescope in 1983 has produced a confusion limited atlas containing approximately 3000 sources per steradian stronger than 0.15 Jy. Available on FITS tapes that can be readily displayed and analyzed with standard AIPS programs, the atlas is comparable to the Palomar Sky Survey, its optical counterpart, as a standard reference for source identifications and variability studies.
The VLA continued to participate in ongoing search for gravitational lens candidates chosen from the 6-cm MIT-Green Bank survey with the 300-ft telescope. The seventh candidate to pass all the preliminary radio and optical observational tests was identified in 1985 as the complex triple source, 0023 + 171, with z = 0.946 and total angular separation of 5 arcseconds. Although the object is the closest gravitational lens candidate yet discovered, deep optical images do not reveal the faint lensing mass.
Observations at 18.3 GHz with the 140-ft telescope were critical to the identification of the C3H2 molecule (cyclopropenylidene) in the interstellar medium. The ubiquitous occurrence of this small organic ring molecule in the Galaxy makes it an important new tracer of physical and chemical conditions. A survey of a large number of sources detected the line in emission in cold dust clouds and in absorption in the direction of the galactic center. One-hundred forty foot observations have also detected the line in absorption in Cen A, suggesting that C3H2 may be widespread enough to study in many galaxies. The first detailed maps of the distribution of OH in Halley's Comet were made by the VLA. While no OH was seen toward the coraetary nucleus, the molecular emission in the coma was non-uniformly distributed in several clumps. The detailed maps support comet models which predict the vaporization of coraetary H2O ice from the nucleus and the eventual dissociation of H2O into H and observable OH once it has been expelled from the immediate vicinity of the nucleus.
The detection rate of molecular shells surrounding Infrared, bright, evolved, red giant stars increased greatly as a result of the newly improved l-mm receiver on the 12-111 telescope. These shells provide ideal laboratories for studying the mass losing stages of stellar evolution through the measurement of mass loss rates, isotopic abundance ratios, molecular abundances, and dust-to¬ gas ratios. They contribute significant amounts of carbon and oxygen to the interstellar medium, as well. Observing Hours
30 est-jest. est, est, est, est,
1976 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 Calendar Year
1300-Foot 140-Foot ■ 12-Meter WM Interferometer W&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
1976 77 78 79 80 81 82 83 84 85 1976 77 78 79 80 81 82 83 84 85 1976 77 78 79 80 81 82 83 84 85 1981 82 83 84 85 Calendar Year Calendar Year Calendar Year Calendar Year
\NRAO Staff I Visitors IB 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
1976 1977 1978 1979 1980 1981 1982 1983 1984 1985 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 Radio Telescope Summary
1976 1977 1978 1979 1980 1981 1982 1983 1984 1985 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. Maior improvements to the telescope system include: 1977 - data processing computer and installation of the maser Cassegrain system; 1978 - tests of the deformable subreflector; 1980 - installation of the Model IV auto¬ correlation 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. 300-Foot Radio Telescope Summary 100 "S -\ A ^ A* -^ KS /^ ^^ - A A /- - ^- "\ ^ - V V V / r / ^ 80 A f V \,V - \ i- 60 vV U - V - o- 40 { - \ - / L > \ 20 A AA SS /\ /" ~N v_ / _^ ^N ^ V -J ^ >1 \_ ■—■ 7 — — s - — -^ — -—. ^< y \: ^ ^ 0 y
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, and during 1985 N-S motion was added to the traveling feed. Very Large Array Telescope Summary
1977 1978 1979 1980 1981 1982 1983 1984 1985 Calendar Year — Construction Initial Observing and Testing • Observing 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
350
300
&250 E ^ 200
150
100
50
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
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
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 89 90 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.
10 Distribution of Telescope Time by Per Cent
12-meter 140-foot 300-foot VLA 1985 Summary
Visitors 50% 61% 45% 58% 54%
Students 8% 7% 17% 8% 10%
Permanent Staff 10% 17% 7% 8% 10%
Research Associates 1% 0% 7% 3% 3%
Tests and Calibrations 10% 7% 3% 13% 8%
Maintenance and Installation 20% 6% 12% 9% 12%
Holidays and Unscheduled 1% 2% 9% 1% 3%
11 Distribution of Scheduled Observing Programs in Various Research Areas, by Percent
12-meter 140-foot 300-foot VLA Overall
I. SOLAR SYSTEM --
Sun, Planets, Satellites, and Comets 3% 4% 5% 5% 4%
II. STELLAR —
Pulsars, X-ray Sources, Planetary Nebulae, 18% 7% 9% 27% 15% Circumstellar Shells, Supernova Remnants, Masers. Novae, Supernovae, and Stars
III. GALACTIC
Galactic Structure, Center, Molecular 45% 33% 5% 15% 25% Clouds, HII Regions, Star Formation, Molecules, and Interstellar Medium
IV. EXTRAGALACTIC —
Normal and Active Galaxies, Radio Galaxies, 34% 56% 81% 53% 56% Clusters, Quasars, VLB Studies, Extra- galactic Molecules, and Cosmology
12 Institutions from which Visitors Came to Use NRAO Telescopes during 1985 Telescope
Institution 12-m 140-ft 300-ft VLA
1. Anglo Australian Observatory 2. Aerospace Corp. (CA) 3. Alabama, U. of 4. Arcetri Ap. Obs. (Italy) 5. Arizona, U. of - Steward, L & P Lab.
6. Arizona State Univ. 7. Athens, U. of (Greece) 8. Beijing Ast. Obs. (P.R. of China) 9. Bell Labs. (NJ) 10. Bologna, U. of (Italy)
11. Bonn Univ. (FRG) 12. Bordeaux Obs. (France) 13. Boston Univ. (MA) 14. Brandeis Univ. (MA) 15. British Columbia, U. of (Canada)
16. Brookhaven Nat. Laboratories 17. Bureau de Longitudes (Paris) 18. Calgary, U. of (Canada) 19. California, U. of, Davis 20. California, U. of, Berkeley - Hat Creek Obs.
21. California, U. of, Irvine X 22. California, U. of, Los Angeles X 23. California, U. of, Santa Cruz - Lick Obs. X 24. Caltech - OVRA, Mt. Palomar x X 25. Cambridge Univ. - Cavendish, Mullard, IOA X X
13 Telescope
Institution 12-m 140-ft 300-ft VLA
26. Carleton College 27. Catania Univ. (Italy) 28. CFA - Harvard & SAO (MA) 29. Centre College 30. Ctr. of Nuclear Studies (Saclay, France)
31. Chalmers - Onsala Space Obs. (Sweden) x 32. Chicago, U. of - Yerkes Obs. x 33. CIerason Univ. X 34. CSIR (Johannesburg, S. Africa) X 35. Colgate Univ. (NY)
36. Colorado, U. of - JILA (Boulder) 37. Columbia Univ. (NY) 38. Computer Tech. Assoc. 39. Cornell Univ. (NY) 40. CSIRO (Australia)
41. Dartmouth College 42. DAO - Dominion Ap. Obs. (Canada) 43. DRAO - Dominion Radio Ap. Obs. (Canada) 44. DTM - Carnegie Institute 45. Edinburgh, U. of (Scotland)
46. ESO - Eur. Southern Obs. (FRG; Chile) 47. ESOC (Damstadt, FRG) 48. ESTEC (Netherlands) 49. Fairborn Observatory 50. Florida, U. of
14 Telescope
Institution 12-m 140-ft 300-ft VLA
51. George Mason Univ. (VA) x 52. Gottingen Acad. Sci. (FRG) x 53. Grenoble, U. of (France) X 54. Gronlngen, U. of - Kapteyn Lab. (Netherlands) X 55. Hamburger Stemwarte (FRG) X
56. Haverford College (PA) 57. Hawaii, U. of - Inst, of Astronomy 58. Haystack Obs. - NEROC 59. Howard Univ. (D.C.) 60. Illinois, U. of - Vermilion River Obs.
61. Imperial College (London) 62. Inst, of Astrophy. (Paris) 63. Inst, for Space Res. (USSR) 64. Inst, for A & A (Berlin, FRG) 65. Inst. Molecular Science (Okazaki, Japan)
66. Interferometrics, Inc. x 67. Iowa, U. of (Iowa City) x X 68. Iowa State Univ. (Ames) X 69. IRAM (France) X 70. Itapetinga Obs. (Brazil)
71. Johns Hopkins Univ. - Space Tel. Inst. x 72. JPL - Goldstone (CA) x 73. Kent, U. of (England) 74. Kentucky, U. of X 75. KPNO - Kitt Peak Nat. Obs. X
15 Telescope
Institution 12-m 140-ft 300-ft VLA
76. Kyoto Univ. (Japan) 77. Leicester, U. of (England) 78. Leiden, U. of - Huygens Lab. (Netherlands) 79. Los Alamos Scientific Lab. 80. Louisiana State Univ.
81. Maine, U. of x 82. Manchester, U. of - Jodrell, Nuffield X 83. Marseille Obs. (France) X 84. Maryland, U. of - (Hark Lake Obs. X 85. Massachusetts, U. of - Five College Obs. X
86. Meudon Obs. (France) x 87. Mexico, U. of - Inst, of Ast. (Mexico) x 88. Michigan, U. of (Ann Arbor) 89. Milano (Italy) X 90. Minnesota, U. of X
91. Missouri, U. of (St. Louis) 92. MIT - Lincoln Labs. 93. Monash Univ. (Australia) 94. Montreal, U. of (Canada) 95. MPI (Heidelberg, FRG)
96. MPIPA (Munich, FRG) 97. MPIR (Bonn, FRG) 98. Mt. Stromlo Obs. (Australia) 99. Mt. Wilson & Las Campanas - Carnegie 100. Nagoya Univ. (Japan)
16 Telescope
Institution 12-m 140-ft 300-ft VLA
101. NAIC - Arecibo Obs. (P.R.) x 102. Nanking, U. of (China) x 103. NASA, Ames (CA) X 104. NASA, Goddard - GSFC (Greenbelt, MD) X 105. NASA, Inst, for Space Studies (NY)
106. NBS - National Bureau Stds. 107. NFRA (Netherlands) 108. NMIMT - New Mexico Inst. Mining Tech. 109. New Mexico, U. of (Albuquerque) 110. New York Univ.
111. Nobeyama Observatory (Japan) 112. North Carolina, U. of 113. NRC - Algonquin, Herzberg (Canada) 114. NRL - Naval Research Labs. 115. NSF - National Science Foundation
116. Ohio State Univ. 117. Oklahoma, U. of 118. Oregon, U. of 119. Oxford, U. of (England) 120. Padova Observatory (Italy)
121. Peking Obs. (P.R. of China) x 122. Penn State Univ. x 123. Pittsburgh, U. of - Allegheny Obs. (PA) X 124. Princeton Univ. - Inst. Adv. Studies (NJ) X 125. Puerto Rico Univ. X
17 Telescope
Institution 12-m 140-ft 300-ft VLA
126. Queen Mary College (England) 127. Queens Univ. (Canada) 128. Raman Institute (India) 129. Rensselaer Polytech Inst. (NY) 130. Rice Univ. (TX)
131. Royal Greenwich Obs. (England) 132. Royal Obs. - UKIRT (Scotland) 133. San Diego State Univ. (CA) 134. Solar Phys. Res. Corp. 135. Southampton, U. of
136. Stockholm Observatory (Sweden) 137. SUNY (all campi) 138. Sussex, U. of (England) 139. Sys. & Appl. Sci. Corp. 140. Tata Inst. - TIFR, RAC (India)
141. Tel-Aviv Univ. - Wise Obs. (Israel) x 142. Texas, U. of, Austin - McDonald Obs. x 143. Tokyo Univ. - Tokyo Ast. Obs. (Japan) X 144. Toronto, U. of - D. Dunlap Obs. (Canada) X 145. Tufts Univ. (MA) X
146. Univ. College Cardiff (England) 147. Uppsala Astr. Obs. 148. USNO - U.S. Naval Obs. 149. Utrecht, U. of (Ast. Inst., Netherlands) 150. Utsunomiya Univ. (Japan)
18 Telescope
Institution 12-m 140-ft 300-ft VLA
151. Victoria, U. of (Canada) 152. Virginia, U. of 153. VPI & SU x 154. Washington, U. of x 155. Williams College (MA) X
156. Wisconsin, U. of - Washburn Obs. 157. Wyoming, U. of 158. Yale Univ. (CT)
No. of Institutions 51 56 21 135
No. of Visitors 97 156 35 451 No. of Students 18 29 12 80 No. of Research Associates 2 0 3 8 No. of Permanent Staff
Total Observers 128 202 55 572
All told, 675 visitors, including 110 students, from 158 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 80 81 82 83 84 85 86 87 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.
20 NRAO Front-End Box Status
TECHNICAL DATA SHEET No. 12 NOVEMBER 1985 PAGE 1 OF
System 3 dB Person(s) Appllcftble Frequency Amplifier Feed Calibration Temperature Bandwidth Polarisation Switching System Remarks in 300-ft 25-50 Fat 25 Single Linear Traveling MHz > 500 K Dipole E-W. Feed (8 ■) Transistor Reaovable diode Designed for pulsar, continuua, and line Coe Dicke switch. work. About 2 hours to change Dicke switch 300-ft 50-80 Dual- « 5X Adjustable Reference tea- and feed hybrid. Frequency switching not (Oliver) Traveling MHz Channel * 450 K - Bandwidth. Orthogonal 8 K to perature adjust¬ available. Usable with 4-channel aultl- Feed i 500 Kwtth 2.5-4.0 Linear or 8000 K. able froa bandwidth receiver, all NRAO line receivers reaovable and digital continuua receiver. or (4.6 a) Dicke switch. Crossed- 300 K to 40000 K. Dtpole. quad hybrid 140-ft at feed for Clip-On 110-250 MHz 2 200 K- Broadband RCP and LCP. (1.7 ca) 2 260 K with 140 Crossed- Dicke switch. Dtpole. i 320 K. Broadband Orthogonal Adjustable Reaovable diode Designed for pulsar, continuua, and line Transistor > 200 K wtth Crosaed- 1.5 K to Dicke switch. 300-ft 250-500 MHz 250 Linear or work. About 2 hours to change Dicke switch Coe Traveling (80 ca) Dual- reaovable Dtpole. reaovable 1500 K. and feed hybrid. Frequency switching not Feed Channel 330-450 MHz quad hybrid available. Usable with 4-channel aultl- (Oliver) aapllflers. at feed for bandwidth receiver, all NRAO line receivers or RCP and LCP. and digital continuua receiver. 450-500 FCT 140-ft MHz top 50-80 K 50 Clip-On 280-350 When installed on the 300-ft traveling feed, 300-ft 5 K Frequency switching. 280-350 MHz Cooled Up- 45-85 50 350-410 Dual two feeds can be used: the 750-1000 MHz on New converter/ 450-500 Orthogonal the west end of the box and one of the others Trsveltng 350-410 MHz GASFET Aap Cavity-backed Linear. on the east end. Selection of one of the two Feed (80 ca) Dual Channel Crossed 60 IF Polariaeter feeds should take less than 5 ainutes. To Mount dlpoles. change a feed requires three hours. 500-750 or RF Hybrid Coe 450-500 MHz Cooled Up- for right and 300/140-ft (60 ca) converter/ 50-70 250 Scalar with When installed in the Sterling aount on (Shank) Sterliac GASFET Aap left circular 500-750 MHz Crossed polarization. the 140-ft or 300-ft antennas, only one Mount (48 ca) Dual Channel of the five feeds 280- 350 MHz 750-1000 MHz Cooled Up- 250 750-1000 converter/ 50-90 350- 410 MHz (34 ca) Scalar with 450- 500 MHz GASFET Aap Crossed Dual Channel 500- 750 MHz or Di poles. 750-1000 MHz can be used. To change feeds requires two hours on the 140-ft and three hours on the 300-ft. 300/140-ft 1.00-1.45 Cooled 35 to 40 450 Single Orthogonal 8K to Frequency switching. Part of 4.5-5.1 GHz receiver listed below. Coe (25 cu) FET Beam Linear. 14 K Noise adding. Feed change required to go to 6 cm. (Shank) (6/25 Rx) Dual Channel Scalar. 21 TECHNICAL DATA SHEET No. 12 NOVEMBER 1985 PAGE 2 OF 4 System 3 dB Person Applicable Frequency Amplifier Feed Calibration Temperature Bandwidth Polarization Switching System Remarks in Type Type Value Telescope (GHz) (Kelvin) (MHz) Charge 140/300-ft Dual Three 2HE 1.30-1.80 23-30 Up to 120 Orth. Linear 2 K Frequency Either circular or linear polarizations are Norrod (19 ca) Channel Single Beaa or and or Cooled FET selectable. Circular polarization requires (Chestnut) (23 ca) 1.30-1.36 Circular 200 K polarization adjustments horn the control room. Feed switching (22 ca) Liaited 1.36-1.43 Band change requires feed change, 2 to 3 (18 ca) 1.60-1.72 or noise adding. hours. 300/140-ft 2.695 Uneooled 130 120 3 Horns Circular or 4 K 300 K load or Continuum receiver. On-axis horn has receivers Bradley (11 ca. GaAsFET DSB Linear polarization, or on both polarizations. Four hours to change 3-feed) 4 Channel beam. polarization. (Chestnut) 300/140-ft 2.9-3.5 Dual Channel 25-35 Up to 200 Two 2HE Orthogonal Low 1.8 Frequency switching. Band change requires feed change i 2-3 hrs. Bradley Single Beaa Linear High 150 Circular polarization requires phase equaliz¬ (9 ca) Cooled FET Feed Noise adding. (Chestnut) (10 ca) liaited. 2.90-3.15 and ing adjustaents froa the control rooa. 3.15-3.40 Circular Frequency switching requires 50 as blanking tiae.. 300/140-ft Cooled 65 Kload 250 Dual Beams Identical Linear Cooled Dicke switches Continuua use. Behrens 3.12-3.37 (latching ferrite) Paraaps switched. Fixed offset by or 4 K (Jeffries) (9 ca) Dual Channel for load (20 K) 75 K beam Tuned 3 Identical switching or beaa HPBW, switched. Circular and switching with noise singly or injection for bal¬ polarized. Orth. Circular 14 K ancing; 10 Hz aaxi¬ aua rate. Single Orth. Circular 1.4 K 300/140-ft 4.47-5.05 Cooled Other polarization. Includes cooled FET's for 1.0—1.45 GHz. Coe. GaAsFET 50-60 580 or Orth. Linear or (6ca) Dual Beaa Identical or Feed change required to go to 25 cm. (Shank) Dual Channel Offset Orth. Circular 12.8 K Beam switching. (6/25 Rx) 3 HPBW or Identical Linear T 8y8 140-ft 4.7-7.2 Upconverter 30-50 60-300 Cassegrain Fixed Linear 3-7 K Frequency or Frequency z Cassegrain Maser Circular VLB Mutator Beam (5 ca) 4.7- 4.9 40-50 Two 4.9- 6.5 30-40 Brockway Receivers 6.5- 7.2 40-50 (Dunbrack) Upconverter 35-80 60-300 Cassegrain Fixed Linear Frequency or 7.8-11.2 3-7 K 7.6- 8.5 50-80 (3 ca) Maser Circular VLB Nutator Beam 8.5-11.2 35-45 12.0-16.2 Upconverter 50-80 60-300 Cassegrain Fixed Linear 3-7 K Frequency or 12.0-16.2 50-80 (2 ca) Maaer Nutator Beam 18.2-25.2 Maser 40-70 60-300 Cassegrain Fixed Linear 2-6 K Frequency or 18.2-25.2 40-70 (1.4 ca) Circular VLB Nutator Beam 22 TECHNICAL DATA SHEET No. 12 NOVEMBER 1985 PAGE 3 OF H System Continuum AppUcaUe Frequency Amplifier 3 dB Feed Calibration Switching Person Temperature Sensitivity Polarization Telescope (GHz) Type Bandwidth Type Value System Remarks in (Kelvin) (Jansky /sec) Charge 12-m 70-116 Cooled 260-400 1.0 650 MHz Horn-Lens Dual 10 K Nutating Cochran Mixer SSB Linear Subreflector 90-115 Approx. To be Nutating 12-a SIS 650 MHz Horn-Lens Dual 10 K Laab 100 Linear Subreflector 1400-2000 12-a 330-360 Cooled 12 650 MHz Horn-Lens Single Nutating Mixer SSB Linear - Subreflector Payne 6 12-m 200-270 Cooled 500-1000 600 MHz Horn-Lens Dual - Nutating at 230 GHz Range will be extended to 270- Payne Mixer SSB Linear Subreflector 300 later in 1985. 23 TECHNICAL DATA SHEET No. 12 NOVEMBER 1985 PAGE 4 OF 4 System 3dB Person Frequency Amplifler Feed Calibration Applicable Temperature Bandwidth Polarization Switching System Remarks in Telescope Type Type Value (GHz) (Kelvin) (MHz) Charge Lille VLA 308- Uneooled 250* 3 MHz Priae Dual 25* Noise injection. * Antennas 8, 12, and 15. 343 Translator (limited by Focus*** Orthogonal 9.6 Hz. ** Six other antennas. 150** interference) Circular 10** 50 percent cycle. *** Feed is off-axis on antennas 8 and 12. Lille VLA 1340- Cooled 60 55 Cassegrain Dual 4 Noise injection. 1730 FET Orthogonal 9.6 Hz, Circular Lille VLA 4500- Cooled 60 55 Cassegrain Dual 4 Noise injection, 5000 Orthogonal 9.6 Hz. Cooled Circular 50 percent cycle. Paramp and FET 7 Lille VLA 14 400- Cooled 110 55 Cassegrain Dual Noise injection, 15 400 FET Orthogonal 9.6 Hz. Circular 50 percent cycle. Lille VLA 22 000- Cooled 350 55 Cassegrain Dual 20 Noise injection, 24 000 Mixer Orthogonal 9.6 Hz, Circular 50 percent cycle. 24 NRAO - Staff and Visitor Publications 1985 Aller, H. D. and Reynolds, S. P. "The Decrease with Time of the Radio Flux of the Crab Nebula," Astrophys. J., 293, L73-L75, 1985. Aller, H. D. and Reynolds, S« P. "Evolution of the Centimeter Flux of 3C58 and the Crab Nebula." In: The Crab Nebula and Related Supernova Remnants. Ed. M. C. Kafatos and R. B. C. Henry. (Cambridge: Cambridge University Press, 1985) 75-79. Anantharamalah, K. R.; Erlckson, W. C; and Radhakrlshnan, V. "Observations of Highly Excited Radio Recombination Lines Towards Cassiopeia A." Nature, 315, 647-649, 1985. Andrews, M. D.; Basart, J. P.; and Lamb, R. C. "Observations of the Radio Source G6.6-0.1 Positionally Coincident with the W28 SNR." Astron. J., 90, 310-314, 1985. Antonucci, R. R. J. "Extended Radio Emission Associated with Blazars." In: Active Galactic Nuclei. Ed. J. E. Dyson. (Manchester: Manchester University Press, 1985) 98-102. Antonucci, R. R. J. "VLA Maps of 41 Radio Galaxies." Astrophys. J. Suppl. Ser., 59, 499-511, 1985. Antonucci, R. R. J. and Miller, J. S. "Spectropolarimetry and the Nature of NGC 1068." Astrophys. J., 297, 621-632, 1985. Antonucci, R. R. J. and Olszewski, E. W. "Radio Observations of IRAS Extreme Infrared Galaxies." Astron. J., 90, 2203-2206, 1985. Antonucci, R. R. J. and Ulvestad, J. S. "Extended Radio Emission and the Nature of Blazars." Astrophys. J., 294, 158-182, 1985. Archer, J. W. "A High Performance, 2.5-K Cryostat Incorporating a 100-120-GHz Dual Polarization Receiver. Rev. Sci. Instrum., 56, 449-458, 1985. Archer, J. W. "Low-Noise Heterodyne Receivers for Near-MUlimeter-Wave Radio Astronomy." IEEE Proc, 73, 109-130, 1985. Archer, J. W. and Crawford, M. J. Jr. "A Synthesised 90-120 GHz Signal Source." Microwave J., 28, 227-250, 1985. 25 Archer, J. W. and Faber, M. T. "High-Output, Single- and Dual-Diode Millimeter-Wave Frequency Doublets." IEEE Trans. Micro. Theory Tech., MTT-33: 533-538, 1985. Armstrong, J. T. and Barrett, A. H. "High-Resolution Surveys of the Sagittarius A Molecular Cloud Complex in Ammonia, Carbon Monoxide, and Isocyanic Acid." Astrophys. J. Suppl. Ser., 57, 535-570, 1985. Armstrong, J. T.; Ho, P. T. P.: and Barrett, A. H. "VLA Observations of Smooth, Rapidly Rotating NH3 in the Sagittarius A '15 km s~l Cloud1." Astrophys. J., 288, 159-163, 1985. Baan, W. A. "Powerful Extragalactic Masers." Nature, 315, 26-31, 1985. Baan, W. 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