NATIONAL RADIO ASTRONOMY OBSERVATORY
Observing Summary - 1982 Statistics
February 1983 NATIONAL RADIO ASTRONOMY OBSERVATORY
Observing Summary - 1982 Statistics
February 1983 Some Highlights of the 1982 Research Program
Detailed morphological and spectral VLA observations of solar active regions and solar flares have placed new constraints on our understanding of the generation and maintenance of solar flares. The VLA has provided the first observational evidence of the emergence of new magnetic flux at coronal levels before the onset of a flare, and studies of its behavior have been carried out in combination with observations from the Solar Maximum Mission Satellite.
Extremely sensitive measurements with the 140-foot telescope and the new maser-up converter receiver have detected the 8.7 QHz hyperfine transition of ^He in several regions of ionized hydrogen in the Galaxy. The derived abundances from three regions are roughly twice the ^He abundance determined in the sun. These measurements indicate that the stellar production of ^jte during the evolution of low mass stars is quite small. Furthermore, cosmological models which favor a high production rate for ^He in the early universe are severely restricted.
Radio carbon monoxide observations of many molecular clouds over the past few years have detected high velocity bulk motion of molecular gas due to energetic mass outflows from embedded young stellar objects. The frequency and large kinetic energies of these flows make them a very significant state of early stellar evolution and they may even provide sufficient mechanical energy to stabilize giant molecular clouds against gravitational collapse. Recent maps of some of these outflow regions obtained with the 36-foot telescope indicate that the flow is bipolar in nature with mass ejection occurring in opposite directions and in a few cases highly collimated similar to the jets observed near active galactic nuclei and quasars. Combined radio and optical observations of the two spectroscopically distinct classes of Seyfert galaxies have suggested fundamental physical differences between the two Seyfert types. Optical polarization vectors tend to either align with or be perpendicular to the large scale radio structure axes depending on Seyfert class. The alignments might be due to optically thin and thick electron-scattering disks surrounding the active nuclei of the galaxies•
VLA observations of six ultracompact HII regions have revealed shell or ring structures on the size scale ~0.02 to 0.1 pc in four of the objects. These objects, located in dense molecular clouds, are generated around newly formed massive stars where their properties are still characteristic of the star formation process and have not yet been severely distorted and fragmented by the surrounding material. The observed internal structures are indicative of a high-temperature, low-density cavity surrounded by a dense shell of material, which is generated by the action of a stellar wind from the centrally located, invisible, hot star. The process is apparently not uncommon among ultracompact HII regions•
VLA observations of Sgr A, the source at the center of our Galaxy, have revealed a detailed morphology and spectral index distribution which clearly separates the object into two physically distinct regions. The thermal source Sgr A West has a spiral shape with the compact point source close to, but not exactly coincident with, the peak in the thermal emission. Models for its ordered structure involve combinations of rotation together with the infall or expulsion of gas. Tangent to the spiral feature is a ring-shaped non-thermal source of much greater extent, with properties similar to galactic supernova remnants. Observing Hours 40
est. est. est est. est. est.
1973 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 Calendar Year
1300-Foot \MO-Foot 36-Foot \ZS\ Interferometer Hi VLA
Fig. 1. This figure shows the hours scheduled for observing on each telescope during the last decade. Distribution of Scheduled Observing Time
36-Foot 140-Foot 300-Foot VLA
1 ll
1973 74 75 76 77 78 79 80 81 82 1973 74 75 76 77 78 79 80 81 82 1973 74 75 76 77 78 79 80 81 82 1 1981 82 Calendar Year Calendar Year Calendar Year Calendar Year
\NRA0 Staff I Visitors I 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. 36-Foot Radio Telescope Summary 100 80 ' + * Y\ r\ F-"^ ^\ P\ I- 'X P*-^- ^^4- '
-£ 60 0} ,4i\lAL\L.Y..Y.\i \i ft 1 ■ ^ 40 iii_a_L_j i-J-it s r 20 i itJ-i- A-A - A 4^ ^4-lJi J I A ■ 0 1973 1974 1975 1976 1977 1978 1979 1980 1981 1982 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 calibra¬ tion, maintenance, and installation of new experiments, and the percent¬ age 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 the telescope was out of service for the replacement of the reflecting surface and its backup structure. 140-Foot Radio Telescope Summary 100
80
•£ 60 u 40
20
1973 1974 1975 1976 1977 1978 1979 1980 1981 1982 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 calibra¬ tion, maintenance, and installation of new experiments, and the percent¬ age of time lost due to equipment failure, bad weather, and radio interference. Major improvements to the telescope system include: 1974 - installation of the Cassegrain system; 1977 - data processing computer and installation of the maser Cassegrain system; 1978 - tests of the deformable subreflector; 1980 - installation of the Model IV autocorrelation receiver; and 1982 - beam efficiency and pointing tests at 1.3 cm. 300-Foot Radio Telescope Summary 100 — —• - ^ - - ^^ ^ - -\ /* SX ^S /- - "S - - — -- s^ \x V "N /- 80 \ > r V \_ ^A ' v > \ r / - 60 V y / - v - o- 40 I h \ - 20 ( \ / \ /" A ^ •\ A /^N N J —- ^ — - - ^ — -y V — -^ ^ S-. y \------v *~m ^c J V 0
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. The telescope was painted in 1973, and during 1980 a new traveling feed was installed. Very Large Array Telescope Summary 100 - 80 - /** NX ^ - -£ 60 / CD ( - -- ^. £ /— »-r 40 V- "^ "V V ^ -^ - h \^ - -
20 0* A y'"** •^s ■ar' \ - - ■*/ s^ -.--- ^^ — V -_. ._. ,-_« .-
Calendar Year Construction Initial Observing and Testing — •Observing Testing 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 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
^r 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 Pfeople 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 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
36-foot 140-foot 300-foot VLA 1982 Summary
Visitors 35% 62% 46% 47% 47%
Students 21 11
Permanent Staff 13 19 14 12
Research Associates 0
Tests and Calibrations 28 11
Maintenance and Installation 47 16
Holidays and Unscheduled 0
11 Distribution of Scheduled Observing Programs in Various Research Areas, by Percent
36-ft 140-ft 300-ft VLA Overall
I. SOLAR SYSTEM -- 6% 4% 3%
Sun, Planets, Satellites, and Comets
II. STELLAR — 7% 9% 17% 21% 17%
Pulsars, X-ray Sources, Planetary Nebulae, Circuntstellar Shells, Supernova Remnants, Masers, Novae, Supemovae, and Stars
III. GALACTIC 72% 34% 9% 18% 26%
Galactic Structure, Center, Molecular Clouds, HII Regions, Star Formation, Molecules, and Interstellar Medium
IV. EXTRAGALACTIC — 15% 57% 74% 57% 54%
Normal and Active Galaxies, Radio Galaxies, Clusters, Quasars, VLB Studies, Extragalactic Molecules, and Cosmology
12 Institutions from which Visitors Came to Use NRAO Telescopes during 1982
Telescope
Institution 36-ft 140-ft 300-ft VLA
1. Anglo Australian Observatory 2. Alabama, U. of 3. Amsterdam, U. of - Astr. Institute (Netherlands) 4. Arcetri Astrophysical Observatory (Italy) 5. Arizona, U. of - Steward Obs., Lunar & Planetary Lab
6. Armagh Observatory (Ireland) X 7. Battelle Northwest Laboratories X 8. Bell Labs x X 9. Bologna, U. of (Italy) x X 10. Boston Univ. X
11. Brandeis Univ. x 12. British Columbia, U. of (Canada) X 13. California, U. of, Davis X 14. California, U. of, Berkeley - Hat Creek Observatory X 15. California, U. of, Los Angeles X
16. California, U. of, San Diego 17. California, U. of, Santa Cruz - Lick Observatory 18. California Institute of Technology - OVRA, Mt. Palomar 19. Cambridge Univ. - Cavendish, Mullard, I0A (England) 20. Canada-France-Hawaii Telescope
21. Carter Observatory (New Zealand) 22. Center for Astrophysics - Harvard, Smithsonian Astrophys. Obs. 23. Chalmers Univ. of Technology - Onsala Space Obs. (Sweden) 24. Chicago, U. of - Yerkes Observatory 25. Colorado, U. of - Joint Inst, for Laboratory Astrophysics
13 Telescope
Institution 36-ft 140-ft 300-ft VLA
26. Columbia Univ. 27. Copernicus Univ. - Torun Obs. (Poland) 28. Cornell Univ. 29. CSIRO, Australia 30. Cerro Tololo Inter. Obs. (Chile)
31. Dominion Radio Astrophysical Obs. (Canada) 32. Dept. of Terrestrial Magnetism - Carnegie Institution 33. European Southern Observatory (FRG; Chile) 34. ESTEC (Netherlands) 35. Florida, U. of
36. George Mason Univ. x 37. Grenoble, U. of (France) x 38. Groningen, U. of, - Kapteyn Lab (Netherlands) x 39. Haverford College 40. Hawaii, U. of - Institute for Astronomy
41. Haystack Observatory - NEROC x 42. Howard Univ. x 43. Hycel Inc. (Texas) X 44. IBM 45. Illinois, U. of - Vermilion River Observatory
46. Inst, of Astrophysics (France) 47. Inst, for Space Research (U.S.S.R.) 48. Interferometrics, Inc. 49. Iowa, U. of 50. Iowa State Univ.
14 Telescope
Institution 36-ft 140-ft 300-ft VLA
51. IRAM, France 52. Jackson State Univ. 53. Jagiellonian Univ. (Poland) 54. Johns Hopkins Univ. - Space Telescope Institute 55. Jet Propulsion Laboratory - Goldstone
56. Kansas, U. of 57. Kentucky, U. of 58. Koln, U. of (FRG) 59. Kyoto Univ. (Japan) 60. Kitt Peak National Observatory
61. Leicester, U. of (England) 62. Leiden, U. of - Huygens Lab (Netherlands) 63. Los Alamos Scientific Laboratory 64. Madrid Observatory (Spain) 65. Manchester, U. of - Jodrell Bank - ttiffield (England)
66. Maryland, U. of - Clark Lake Observatory x 67. Massachusetts, U. of - Five College Observatory X 68. Meudon Observatory (France) X 69. Mexico, U. of - Inst, of Astronomy (Mexico) 70. Michigan, U. of
71. Minnesota, U. of 72. Massachusetts Institute of Technology - Lincoln Labs x 73. Molecular Research Institute x 74. Max-Planck-Institute for Physics and Astrophysics, Munich (FRG) 75. Max-Planck-Institute for Radio Astronomy, Bonn (FRG) x
15 Telescope
Institution 36-ft 140-ft 300-ft VLA
76. Mt. Stromlo Observatory (Australia) x 77. NAIC - Arecibo Observatory x 78. Nagoya Univ. (Japan) 79. NASA, Ames 80. NASA, Goddard Space Flight Center
81. NASA, Institute for Space Studies x 82. National Bureau of Standards x 83. Nevada, U. of 84. Netherlands Foundation for Radio Astronomy (Netherlands) 85. New Mexico Institute of Mining and Technology
86. New Mexico, U. of 87. Nobeyama Observatory (Japan) 88. North Carolina, U. of 89. Northwestern Univ. 90. National Research Council - Algonquin, Herzberg (Canada)
91. Naval Research Laboratory x 92. National Science Foundation x 93. Ohio State Univ. X 94. Oklahoma, U. of X 95. Oregon, U. of
96. Padova Observatory (Italy) 97. Paris Observatory (France) 98. Penn State Univ. 99. Pennsylvania, U. of 100. Phoenix Corporation
16 Telescope
Institution 36-ft 140-ft 300-ft VLA
101. Pittsburgh, U. of - Allegheny Observatory 102. Princeton Univ. - Institute for Advanced Studies 103. Puerto Rico Univ. 104. Queen Mary College (England) 105. Queens Univ. (Canada)
106. Radio Physics Inc. (Boulder) 107. Radio Astronomy Center - TIFR (India) 108. Rensselaer Polytechnic Institute 109. Royal Greenwich Observatory (England) 110. Royal Observatory (Scotland)
111. Sandia Labs 112. San Diego State Univ. 113. Seattle Univ. 114. Stanford Univ. - Institute for Plasma Research 115. Stockholm Observatory (Sweden)
116. SUNY, Stony Brook 117. Sydney, U. of (Australia) 118. Systems and Applied Science Corporation 119. Tennessee, U. of 120. Texas, U. of - McDonald Observatory
121. Tokyo Univ. - Tokyo Astronomical Observatory (Japan) 122. Toronto, U. of - David Dunlap Observatory (Canada) 123. Tufts Univ. 124. Turku, U. of (Finland) 125. (Unaffiliated)
17 Telescope
Institution 36-ft 140-ft 300-ft VLA
126. U.S. Naval Observatory 127. Utsunomiya Univ. (Japan) 128. Vermont, U. of 129. Victoria, U. of (Canada) 130. Villanova Univ.
131. Virginia, U. of 132. VPI & SU 133. Washington, U. of x 134. Wisconsin, U. of - Washburn Observatory x 135. Wyoming, U. of X
No. of Institutions 43 55 23 111
No. Visitors 81 151 36 349
No• Students 11 25 15 71 No. Research Associates 0 1 3 7
No. Permanent staff
Total Observers 96 191 63 452
All told, 567 visitors, including 97 students, from 135 institutions.
18 NRAO Student Program
est. est. est. est. est, est 120
100 I Undergraduate \Co-op 80 I Summer Graduate \Ph.D.
E 60
40
20
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.
19 DOX TECHNICAL DATA SHEET INIIttU rroni-tn a a laius No. 12 NOVEMBER 1982 PAGE 1 OF 4 System 3 dB Person Applicable Frequency Amplifier Feed Calibration Temperature Bandwidth Polarization Switching System Remarks in Telescope (MHz) Type Type Value (Kelvin) (MHz) Charge
300-ft &0-S0 * 450 K " * 10* Simultaneous Adjustable Removable diode Designed for pulsar, continuum, and line work. Brundage Fixed on > 500 K with 5 Bandwidth. 0*. 45\ 90', 30 K to Dicke switch 110-500 MHz feeds can be manually rotated 45* Traveling Dicke switch. TunaWe 135* Linear, 30 000 K. and 90* for polarization work. Usable with 4- Feed Crossed- RCP and LCP. channel multi-bandwidth receiver and all NRAO Dipole. Removable line receivers. About 2 hours to change Dicke 140-ft quad hybrid switch and feed hybrid. Frequency switching * 200 K - Broadband Adjustable Clip-On at feed for not available. 110-250 i 260 K with 140 Crossed- 8 K to circular. Dicke switch. Dipole. 8000 K. Transistor Z 320 K. Broadband Adjustable > 200 K with Crossed- 1.5 K to removable Dipole. 1500 K. 250-500 330-450 MHz 250 amplifiers. Additional 50 K with Dicke switch.
300-ft 300-410 Cooled 300-350 Dual 5 K Frequency switching. When installed on 300-ft traveling feed, two feeds Coe New Upconverter/ 50 110 350-410 Orthogonal can be used: the 750-1000 MHz on the west end of Traveling GASKET Amp Cavity-backed Linear. the box and one of the others on the east end. Se¬ Crossed Feed lection of one of the two feeds should take less than Mount Dipoles. 5 minutes. To change a feed requires three hours 500-750 300/140-ft 500-750 Cooled When installed in the Sterling mount on the 140-ft Upconverter/ 60 250 Scalar with Sterling Crossed or 300-ft, any two of the upconverter frequency Mount GASFET Amp ranges may be used by installing the appropriate feed. To use the third frequency range, internal Cooled 750-1000 70 250 750-1000 connections in the dewar must be changed, neces¬ Upconverter/ Scalar with sitating removal of the receiver from the tele¬ GASFET Amp Crossed scope. Dipoles.
300/140-ft 1000- Cooled 35 to 40 450 Single Orthogonal 8K to Frequency switching. Part of 4. 5—5.1 GHz receiver listed below. Coe 1450 FET Beam Linear. 14 K Noise adding. Feed change required to go to 6 cm. Dual Scalar. Channel
1.3—1.5 300/140-ft Uncooled 90-100 200 max. 4 Horns. Linear. « 7 K (cal) Noise adding or Line or continuum from control room. Behrens GHz GaAsFET 77 min. « 440 K frequency switching. RF bandwidth variable from control room. (4-feed Noise 21 cm) add
20 TECHNICAL DATA SHEET No. 12 NOVEMBER 1982 PAGE 2 OF 4 Sysli'in 3 flit Appliralilc Krcqwncy Amplifier Feed Calibration Tompc'ratur*' Ifcuifiwiillh I'olari/.ation Switching System Kemarks TCN'SCOIK* (MHz) TVIM- Tvpe Value (Kelvin) (Mil/.) Charge
140/:uM>-ft 15«if.- Coolod Scalar orth. Linear .1 K KnHjuencv switching Two channels can he used .siimillancouslv al 1760 KKT or and diffcrcnl rrc<|iicncies Itoth circular or linear •.yazi Circular 200 K |N>lari-/.a(iori.s arc available. Inde|>cn'lent or Channel common first !/> selectable from conlrol room Circular |x>lari/.atioii requires adjustments from (18 cm) control room
r 140/300-ft 1000 ti> I'aramp 17. » to 300 20 to 00 1-2 Gil/. I.inear 10 K 300 K load or Set of seven tunable paramps in two receiver Dunbrack 2000 Scalar fr^iucncy switching. Itoxcs. Paramp change- 2 hours Receiver change 4 hours r 140/300-11 2000 to Paramp 220 to 4. >0 2-4 GHz Linear :IOO K load or Kx 1 1.0-1. l.r> 1.16-1.3 1.3-1.7 1 62-2.0 4000 i:t(t between Scalar fn^uency switching Kx 2 2.0-2. r.i 2.!") -3. 15 3.4-3.7 Paramps 2295 to 2.r, -3. 1 3.3 3.9 U> Multi¬ 23H0 MHz. pliers Micromega 13 cm paramp (2295 Mil/.) can be installed.
300/140-ft 2695 x 4 Uncooled 130 12(1 3 Horns Circular or 4 K 300 K load or Continuum receiver On-axis horn has receivers Brundage (11 cm) GaAsFET DRB Linear |x>larization or on both |x>lari/.ations Four hours to change beam. polarization
300/140-ft 3120- Cooled 60 K line and 250 Single Orth. Linear Cooled Dicke switches Continuum anil line use. Feed change approxi¬ Brundage 3370 Paramps load switched. Fixed Beam, or 4 K (latching ferritc) for mately 6 hours on 300-11 and 2 hours on 140-ft Dual 70 K polariza¬ Tuned Dual Orth. load (20 K) switching Channel tion switched. Polarized Circular or beam/polarization and (9 cm) switching with noise 65 Kload 250 Dual Beams Identical Linear 14 K injection for balanc¬ switched. Fixed offset by or ing 10 Hz maximum 75K beam Tuned 3 Identical rate switched. HPBW, Circular singly or polarized. Orth. Circular -snips Orth. Circular 1.4 K 300/140-ft 4470 - Cooled Beam or Orth. Linear ether polarization. Includes cooled FET's for 1.0-1.45 GHz. Coe 50-60 570 5040 GASFET Dual Beam laentical or or Feed change required to go to 25 cm Dual Offset Orth. Circular 12.8 K Beam switching. Channel 3 HPBW or Identical Linear
4.7—7.2 Upconvertet 30-50 Cassegrain Fixed Linear 3-7 K Frequency or Frequency GHz Maser Circular VLB Nutator Beam 4.7- 4.9 40-50 4.9- 6.5 10-40 Brockway 6.5- 7.2 40-50 7.6-11.2 Upconverter 35-80 60-300 Cassegrain Fixed Linear 3-7 K Frequency or 7.6- 8.5 50-80 GHz Maser Circular VLB Nutator Beam 8.5-11.2 J5-45
12.0-16.2 Upconverter 50-80 60-300 Cassegrain Fixed Linear 7-10 K Frequency or 12.0-16.2 GHz Maser Nutator Beam
18.2-25.2 Maser 40-70 60-300 Cassegrain Fixed Linear 3-6 K Frequency or 18.2-25.2 GHz Circular VLB Nutator Beam
Beam shift = Four hours for band change. 112.5 degrees azimuth Second channel -inder construction. 0-3 Beamwidth Ready 1983.
21 TECNICAL DATA SHEET No. 12 NOVEMBER 1982 PAGE 3 OF 4 System Continuum Person Amplifier 3 dB Feed Calibration Switching Applicable Frequency Temperature Sensitivity Polarization Remarks in Telescope fGHz) Bandwidth Type Value System Type (Kelvin) (Jansky .'sec Charge
12-m 31.4 Mixer r.oo 1 GHz Horn-Lens Dual 10 K Nutating Modified 36-ft receiver. Freund DSB Linear Sul"-':nector Completion March 1983.
12- m 70-115 Cooled 280-500 1 GHz Horn-Lens Dual 10 K Nutating Old 36-ft receiver. Payne Mixer SSB Linear Subreflector Will be updated in 1983.
12-m 140-170 Cooled WO-1000 500 MHz Horn-Lens Dual 5 K Nutating Old 36-ft receiver. Payne Mixer SSB Linear Subreflector Will be updated in 1983.
12-m 200-240 Cooled 700-1000 1 GHz Horn-Lens Single 5 K Nutating Old 36-ft receiver. Mixer SSB Linear Subreflector Back up for new 200-300 GHz. Payne
12-m 200-300 Cooled 500-1000 500 MHz Horn-Lens Dual 5 K Nutating Initially available over 200-235. Archer Mixer SSB Linear Subreflector Extendable in future to 300 GHz and and later to 345 GHz. Moorey
22 TECHNICAL DATA SHEET No. 12 NOVEMBER . 982 PAGE ** OF H System 3dB Applicable Frequency Amplifier Feed Calibration Person Temperature Bandwidth Polarization Switching System Telescope (MHz) Type Type Value Remarks in (Kelvin) (MHz) Charge
VLA 1340- Cooled 60 55 Cassegrain Dual 4 Noise injection, Upconverters to be replaced by cooled FET Lilie 1730 Upconverter Orthogonal 9.6 Hz, amplifiers 1982-83. Circular 50 percent cycle.
VLA 4500- Cooled 60 55 Cassegrain Dual 4 Noise injection, Lilie 5000 Paramp or Orthogonal 9.6 Hz, Cooled Circular 50 percent cycle. Paramp and FET
VLA 14 400- Cooled 300 55 Cassegrain Dual 20 Noise injection, Cooled FET amplifiers will be added 1982-83. Lilie 15 400 Mixer Orthogonal 9.6 Hz, Expect 170 K at 14 500, 125 K at 15 100, and Circular 50 percent cycle. 136 K at 15 400.
VLA 22 000- Cooled 350 55 Cassegrain Dual 20 Noise injection, Lilie 24 000 Mixer Orthogonal 9.6 Hz, Circular 50 percent cycle.
23 NRAO - Staff and Visitor Publications 1982
Aaronson, M.; Huchra, J.; Mould, J. R.; Ttally, R. B.; Fisher, J. R.; van Woerden, H.; Goss, W. M.; Chamaraux, P.; Mebold, U.; Slegman, B.; Berrlman, G.; and Persson, S. E. "k Catalog of Infrared Magnitudes and H I Velocity Widths for Nearby Galaxies." Astrophys. J. Suppl. Ser., 50, 241-262, 1982.
Aarseth, S. J. and Saslaw, W. C. "Formation of Voids in the Galaxy Distribution." Astrophys. J., 258, L7-L10, 1982.
Abbott, D. C.; Bieging, J. H.; and Churchwell, E. "Radio Continuum Measurements of Mass Loss from Wolf-Rayet Stars." IAU Symp., 99, 215-220, 1982.
Archer, J. W. "A High Performance Frequency Doubler for 80 to 120 GHz." IEEE Trans. Micro. Theory Tech., MTT-30, 824-825, 1982.
Archer, J. W. "All Solid-State Low-Noise Receivers for 210-240 GHz." IEEE Trans. Micro. Theory Tech., MTT-30, 1247-1252, 1982.
Armstrong, J. W. and Sramek, R. A. "Observations of Tropospheric Phase Scintillations at 5 GHz on Vertical Paths." Radio Sci., 17, 1579-1586, 1982.
Avery, L. W.; MacLeod, J. M.; aud Broten, N. W. "A Model of Taurus Molecular Cloud 1 Based on HC3N Observations." Astrophys. J., 254, 116-125, 1982.
Backer, D.; Kulkarni, S.; and Hetles, C. "Millisecond Pulsar in 4C 21.53." IAU Circ, 3743, 12 November 1982.
Backer, D. C. and Sramek, R. A. "Apparent Proper Motions of the Galactic Center Compact Radi" Source PSR 1929+10." Astrophys. J., 260, 512-519, 1982.
Backus, P. R.; Taylor, J. H.; and Damashek, M. "Improved Parameters for 67 Pulsars from Timing Observations." Astrophys. J., 255, L63-L67, 1982.
Ballck, B.; Heckman, T. M.; and Crane, P. C. "The Large-Scale Radio Structure of 3C 120." Astrophys. J., 254, 483-488, 1982.
24 Bartel, N.; Shapiro, I. I.; Corey, B. E.; Marcaide, J. M.; Rogers, A. E. E.; Whitney, A. R.; Cappallo, R. J.; Graham, D. A.; Romney, J. D.; and Preston, R. A. "The Nucleus of M81: Simultaneous 2.3 and 8.3 GHz Mark III VLB I Observations." Astrophys. J., 262, 556-563, 1982.
Benson, J. M. and Mutel, R. L. "VLBI Observations of the Main Line OH Masers in VY Canis Majoris." Astrophys. J., 253, 199-207, 1982.
Bieging, J. H.; Abbott, D. C.; and Churchwell, E. B. "Mass Loss Rates for Wolf-Rayet Stars from Radio Continuum Observations." Astrophys. J., 263, 207-214, 1982.
Blandford, R. D.; Begelman, M. C.; and Rees, M. J. "Cosmic Jets." Sci. Am., 246, 124-142, 1982 (May).
Bothun, G. D.; Ballck, B.; and Skillman, E. "VLA Observations of the Giant Cluster Spiral UGC 12423." Astron. J., 87, 1098-1105, 1982.
Bregman, J. N.; Glassgold, A. E.; Huggins, P. J.; Pollock, J. T.; Pica, A. J.; Smith, A. G.; Webb, J. R.; Ku, W. H.-M.; Rudy, R. J. LeVan, P. D.; Williams, P. M.; Brand, P. W. J. L.; Neugebauer, G.; Balonek, T. J.; Dent, W. A.; Aller, H. D.; Aller, M. F.; and Hodge, P. E. "Simultaneous Observations of the BL Lacertae Object I Zw 187." Astrophys. J., 253, 19-27, 1982.
Bridle, A. H. "Interferometry of Extragalactic Radio Sources." Phys. Can., 38, 59-64, 1982.
Bridle, A. H. "Systematics of Large-Scale Radio Jets." IAU Symp., 97, 121-128, 1982.
Brown, R. L. "Precessing Jets in Sagittarius A: Gas Dynamics in the Central Parsec of the Galaxy." Astrophys. J., 262, 110-119, 1982.
Brown, R. L. "Radio Observations of the Galactic Center: Future Directions." AIP Conf. Proc, 83, 204-207, 1982. —
Brown, R. L. and Lo, K. Y. "Variability of the Compact Radio Source at the Galactic Center." Astrophys. J., 253, 108-114, 1982.
Bums, J. 0.; Christiansen, W. A.; and Hough, D. H. "Multifrequency VLA Observations of 3C 388: Evidence for an Intermittent Jet?" Astrophys. J. > 257, 538-558, 1982.
25 Burns, J. 0.; Eilek, J. A.; and Owen, F. N. "What Bends Wide-Angle Tailed Radio Sources?" IAU Symp., 97, 45-46, 1982.
Bums, J. 0. and Gregory, S. A. "The Structure of 4C Radio Galaxies in Poor Clusters." Astron. J., 87, 1245-1265, 1982.
Bursteln, D. "Mass and Luminosity in Spiral Galaxies and the Tully-Fisher Relation." Astrophys. J., 253, 539-551, 1982.
Burstein, D. and Heiles, C. "Reddening Derived from H I and Galaxy Counts: Accuracy and Maps." Astron. J., 87, 1165-1189, 1982.
Burstein, D.; Rubin, V. C.; Thonnard, N.; and Ford, W. K., Jr. "The Distribution of Mass in Sc Galaxies." Astrophys. J., 253, 70-85, 1982.
Calamai, G.; Fell!, M.; and Giardinelli, S. "Star Formation in the NH3 Cloud in the NGC 2071 Region." Astron. Astrophys., 109, 123-130, 1982.
Chanmugam, G. and Dulk, G. A. "Radio Emission from AM Herculis-Type Binaries." Astrophys. J., 255, L107-L110, 1982.
Chiuderi-Drago, F.; Bandiera, R.; Falciani, R.; Antonucci, E.; Lang, R.; Willson, R. F.; Shibasaki, K.; and Slottje, C. "Multiple Wavelength Observations of a Solar Active Region." Sol. Phys., 80, 71-85, 1982.
Churchwell, E. and Bieging, J. H. "CN Line Emission from the Molecular Clouds Associated with S106 and NGC 7538." Astrophys. J., 258, 515-532, 1982.
Clark, F. 0. and Johnson, D. R. "The Velocity Gradient of B361." Astrophys. J., 263, 160-165, 1982.
Clark, F. 0.; Troland, T. H.; and Johnson, D. R. "Polarization Properties of the 86 GHz SiO Maser Emission for the R Cassiopeiae." Astrophys. J., 261, 569-575, 1982.
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39 Sopka, R. J.; Herbig, G.; Kafatos, M.; and Michalitsianos, A. G. "Radio and Optical Observations of the R Aquaril Jet." Astrophys. J., 258, L35-L39, 1982.
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44 Additions to the 1981 Bibliography
Bujarrabal, V.; Guelin, M.; Morris, M.; and Thaddeus, P. "The Abundance and Excitation of the Carbon Chains in Interstellar Molecular Clouds." Astron. Astrophys., 99, 239-247, 1981.
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Ulich, B.L. "Millimeter Wave Radio Telescopes: Gain and Pointing Characteristics." Int. J. Infrared Millim. Waves, 2, 293-310, 1981.
45