NATIONAL RADIO ASTRONOMY OBSERVATORY

Observing Summary - 1984 Statistics

February 1985 NATIONAL RADIO ASTRONOMY OBSERVATORY

Observing Summary - 1984 Statistics

February 1985 Some Highlights of the 1984 Research Program

• The 300-foot telescope was used to detect low-frequency carbon recombination lines from cold, diffuse Interstellar clouds in the direction of Cas A. Previously reported absorption lines were confirmed at 26 MHz and a number of other lines were identified in the 25 MHz to 68 MHz range. These lines promise to become an important diagnostic for the ionization conditions in cool interstellar clouds.

• Extremely painstaking observations of several Abell clusters of with the 140-foot telescope have yielded three positive detections of the Sunyaev-Zeldovich effect. The dimunition in the brightness of the microwave background in the direction of clusters is the direct result of the Inverse Compton scattering of the 3° K blackbody photons by electrons in the Intracluster gas. The observations took full advantage of the low noise temperature, broadband, and excellent stability of the Green Bank 18-26 MHz maser system.

• The J ■ 1*0 transition of the long-sought-after molecular ion, HCNff*", was detected with the 12-meter telescope at 74.1 GHz. The existence of protonated HCN is one of the prime tests of the theory of ion-molecule reaction schemes in interstellar chemistry. Virtually all CN-containing interstellar molecules, such as HCN, HNC, and many long-chain cyanopolyynes, form directly from HCNH+.

• A high-resolution VLA survey of all catalogued, high surface brightness, compact objects in the southern uncovered a few objects which are not classifiable into previously known SNR categories. The peculiar axisymmetric source morphologies exhibit filamentary, nonthermal emission and spectral indices intermediate between shell- and Crab-like remnants and seem to represent a new class of nonthermal radio sources.

• VLA monitoring of the brightest radio sources in M82 over the past three years has detected rapid luminosity decay on the scale of only a few years. The sources are interpreted as decaying supernovae associated with the starburst source of energy and massive formation in M82fs nucleus. The rate of supernova production in the inner nucleus of M82 is approximately 50 times higher than for the entire disk of our , and the individual sources are up to 150 times brighter than Cas A.

• The at the center of the cluster has been identified as the source of four jets originating from a double nucleus. Intercomparison of the high resolution VLA maps with detailed optical and X-ray images of the galaxy and cluster suggest that the jets may be powered from their interaction with the turbulent gas in the cluster as well as from an "engine" at the center of 3C 75. Observing Hours 40

est. est. est. est. est. est.

1975 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 Calendar Year

1300-Foot 140-Foot B 12-Meter WM Interferometer WhVLA

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 :y ■il I I Ill■I.

1975 76 77 78 79 80 81 82 83 84 1975 76 77 78 79 80 81 82 83 84 1975 76 77 78 79 80 81 82 83 84 1981 82 83 84 Calendar Year Calendar Year Calendar Year Calendar Year

\NRAO 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. 12-Meter Radio Telescope Summary

o 1975 1976 1977 1978 1979 1980 1981 1982 1983 1984 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 100 1 •^ ^ — - - "N r ^ / ^ 'N , /■ /\ 80 / V V.^ ys. n v. ^ "V y s^ \i ^s / \ y^ A h V 1 -^ /' s? - s/ ! V / \J V N vy v- 60 \ V - - / A 40 i\ - A - A / w A / / /*s 20 /N \< A • V X 'N s v ^N J v\ y V *s J \/ i_ ■>»< v- 7 ^ 0 rr: ^C .—^ .^'~'^. V.^'

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: 1974 - installation of the maser Cassegrain system; 1977 - data processing computer and installa¬ tion of the maser Cassegrain system; 1978 - tests of the deformable subreflector; 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. 300-Foot Radio Telescope Summary 100 A V -\ /^ N^ ^\ *- - •s " ^ ■"^ ^ ss ^ /~ A > /"" - - "S V V V Jm r V y 80 •^ A 1r \,V - - \ / ■£ 60 a> V ofc- - - a> ^ 40 { \ - - / A 20 J A s\ / "N A A /s y -/ V - .y S- —■ ^ \_ - -■ - - ^: ^ . * ^ 7 V — J, -" 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. During 1980 a new traveling feed was installed, and in 1983 cables were replaced and the telescope was painted. Very Large Array Telescope Summary

1977 1978 1979 1980 1981 1982 1983 1984 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 ffifaVLA Construction 350 ■I Research and Operations I \VLBA Construction 300 fc250 rssst 'sw vwx.-ssss. rsssjrssss

^ 200

150

100

50

0 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 v 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 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 Per Cent

12-meter 140-foot 300-foot VLA 1984 Summary

Visitors 46% 60% 48% 56% 53%

Students 4% 9% 28% 9% 12%

Permanent Staff 10% 12% 10% 7% 10%

Research Associates 0% 1% 5% 3% 2%

Tests and Calibrations 15% 6% 0% 16% 9%

Maintenance and Installation 23% 10% 7% 8% 12%

Holidays and Unscheduled 1% 2% 2% 1% 2%

10 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% 2% 4% 5% 4%

II. STELLAR

Pulsars, X-ray Sources, Planetary Nebulae, 23% 9% 11% 22% 16% Circumstellar Shells, Supernova Remnants, Masers, Novae, Supernovae, and

III. GALACTIC

Galactic Structure, Center, Molecular 45% 22% 19% 23% 27% Clouds, HII Regions, Star Formation, Molecules, and

IV. EXTRAGALACTIC —

Normal and Active Galaxies, Radio Galaxies, 29% 67% 66% 50% 53% Clusters, , VLB Studies, Extra- galactic Molecules, and Cosmology

11 Institutions from which Visitors Came to Use NRAO Telescopes during 1984 Telescope

Institution 12-m 140-ft 300-ft VLA

1. Anglo Australian Observatory X 2. Alabama U. of X 3. Arcetri Ap. Obs. (Italy) X 4. Arizona U. of - Steward, L & P Lab. x X 5. Barcelona U. of (Spain) x

6. Battelle Northwest Labs. 7. Bell Labs. (N.J.) 8. Besancon Obs. (France) 9. Birmingham U. of (UK) 10. Bologna U. of (Italy)

11. Boston U. x 12. Brandeis Univ. x 13. British Columbia U. of (Canada) 14. Brookhaven Nat. Laboratories 15. Bureau de Longitudes (Paris)

16. Calgary U. of (Canada) 17. Calif. U. of, Davis 18. Calif. U. of, Berkeley - Hat Creek Obs. 19. Calif. U. of, L.A. 20. Caltech - OVRA, Mt. Palomar

21. Cambridge Univ. - Cavendish, Mullard, I0A 22. Catania U. of (Italy) 23. Catholic U. 24. CFA - Harvard & SAO 25. Centre College

12 Telescope

Institution 12-m 140-ft 300-ft VLA

26. Chalmers - Onsala Space Obs. (Sweden) x 27. Chicago U. of - Yerkes Obs. x 28. Chile, U. of X 29. CIDA (Venezuela) X 30. CSIR (Johannesburg, S. Africa) X

31. Colgate U. 32. Cologne U. (FRG) x 33. Colorado U. of - JILA X 34. Columbia Univ. X 35. Computer Tech. Assoc. X

36. Copernicus U. - Torun Obs. (Poland) 37. Cornell Univ. 38. CSIRO (Australia) 39. CTIO - Cerro Tololo Inter. Obs. (Chile) 40. Dartmouth College

41. DAO - Dominion Ap. Obs. (Canada) 42. DRAO - Dominion Radio Ap. Obs. (Canada) 43. ESO - Eur. Southern Obs. (FRG; Chile) 44. ESOC (Damstadt, FRG) 45. ESTEC (Netherlands)

46. Florida State Univ. 47. Florida U. of 48. George Mason Univ. 49. Grenoble U. of (France) 50. Gronlngen U. of - Kapteyn Lab. (Netherlands)

13 Telescope

Institution 12-m 140-ft 300-ft VLA

51. Hamburger Sternwarte (FRG) x 52. Haverford College x 53. Hawaii U. of - Inst, of Astronomy X 54. Haystack Obs. - NEROC X 55. Howard Univ.

56. lAS-Frascati, Italy 57. Illinois U. of - Vermilion River Obs. 58. Indiana U. of 59. Interferometries. Inc. 60. Iowa U. of

61. Iowa State Univ. 62. TRAM (France) 63. JagielIonian Univ. (Poland) 64. Johns Hopkins Univ. - Space Tel. Inst. 65. JPL - Goldstone

66. Kansas U. of 67. Keele U. of (UK) 68. Kent U. of (UK) 69. Kentucky U. of 70. KPNO - Kitt Peak Nat. Obs.

71. Lafayette College x 72. Leicester U. of (UK) X 73. Leiden U. of - Huygens Lab. (Netherlands) X 74. Lockheed Res. Lab. X 75. Los Alamos National Lab. X

14 Telescope

Institution 12-m 140-ft 300-ft VLA

76. Louisiana State U. 77. Manchester U. of - Jodrell, Nuffield 78. Marseille Obs. (France) 79. Maryland U. of - Clark Lake Obs. 80. Massachusetts U. of - Five College Obs.

81. Meudon Obs. (France) x 82. Mexico U. of - Inst, of Ast. (Mexico) x 83. Michigan State U. X 84. Michigan U. of X 85. Milano (Italy) X

86. Minnesota U. of 87. MIT - Lincoln Labs. 88. Mbnash U. (Australia) 89. Moscow U. of - SSAI 90. MPI (Heidelberg, FRG)

91. MPIPA (Munich, FRG) 92. MPIR (Bonn, FRG) 93. Mt. Stromlo Obs. (Australia) 94. Mt. Wilson & Las Campanas - Carnegie 95. NAIC - Arecibo Obs. (P.R.)

96. Nagoya Univ. (Japan) 97. Nanking U. of (China) 98. NASA, Ames 99. NASA, Goddard - GSFC 100. NBS - National Bureau Stds.

15 Telescope

Institution 12-m 140-ft 300-ft VLA

101. NFRA (Netherlands) x 102. NMIMT - New Mexico Inst. Mining Tech. x 103. New Mexico U. of X 104. New Mexico State U. X 105. New York Univ.

106. North Carolina U. of 107. NRC - Algonquin, Herzberg (Canada) 108. NRL - Naval Research Labs. 109. NSF - National Science Foundation 110. Oklahoma U. of

111. Oregon U. of 112. Padova Observatory (Italy) x 113. Palermo U. of (Italy) x 114. Paris Observatory (France) X 115. Penn State Univ. X

116. Pittsburgh U. of - Allegheny Obs. X 117. Princeton U. - Inst. Adv. Studies x X 118. Puerto Rico Univ. x X 119. Purple Mt. Obs. (China) X 120. Queen Mary College (England) X

121. Queens Univ. (Canada) 122. Raman Institute (India) 123. Rensselaer Polytech Inst. 124. Rice U. 125. Royal Greenwich Obs. (England)

16 Telescope

Institution 12-m 140-ft 300-ft VLA

126. Royal Obs. - UKIRT (Scotland) 127. Rutgers State Univ. 128. Stanford U. - Inst. Plasma Res. 129. Stockholm Observatory (Sweden) 130. SUNY (All Campuses)

131. Sussex U. of (England) 132. Sydney U. of (Australia) 133. Tata Inst. - TIFR, RAC (India) 134. Texas U. of, Austin - McDonald Obs. 135. Toronto U. of - D. Dunlap Obs. (Canada)

136. Tufts Univ. x 137. Turku U. of (Finland) X 138. Univ. College London X 139. USNA - U.S. Naval Academy X 140. USNO - U.S. Naval Obs. X

141. Utrecht U. of (Ast. Inst. - Netherlands) 142. Victoria U. of (Canada) 143. Virginia U. of 144. VPI & SU 145. Washington U. of

146. Wellesley College 147. Williams College x 148. Wisconsin U. of - Washburn Obs. x 149. Wyoming U. of

17 Telescope

Institution 12-m 140-ft 300-ft VLA

No. of Institutions 38 57 33 133

No. of Visitors 3 143 47 445 No. of Students 5 29 17 97 No. of Research Associates 1 3 3 9 No. of Permanent Staff

Total Observers 54 192 72 587

All told, 651 visitors, including 125 students, from 149 institutions.

18 NRAO Student Program 160

140

120

100 I Undergraduate I Co-op E 80 I Summer Graduate \Ph.D.

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 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.

19 NRAO Front-End Box Status TECHNICAL DATA SHEET No. 12 NOVEMBER 1984 PAGE 1 OF 4

System 3 dB Person(s) AppMcable Frequency Feed Calibration Temperature Bandwidth Polarization Switching System Remarks in (GHz) Type Type Value Tclwoope (Kelvin) (MHz) Charge

25-50 Adjustable 25 Fat Single Linear MHz Dipole E-W. 8 K to 300-ft (8 ■) 8000 K. Traveling > 450 K - i 500 Kwith Feed « 10% Orthogonal Adjustable 50-80 Dicke switch. MHz 5 Bandwidth. Linear or 30 K to Tunable removable 30 000 K. Removable diode Designed for pulsar, continuum, and line (4.6 ■) Crossed- quad hybrid Brundage Transistor Dicke switch. work. About 2 hours to change Dicke switch Dtpole. at feed for and feed hybrid. Frequency switching not (Sizeaore) Dual- RCP and LCP. available. Usable with 4-channel aultl- 110-250 i 200 K- Broadband Adjustable Channel 8 K to bandwidth receiver and all HRAO line (MHz) i 260 K with 140 Crossed- receivers. 140-ft (1.7 ■) Dicke switch. Dipole. 8000 K. Clip-On i 320 K. Broadband Adjustable or 250-500 i 200 K with Crossed- 1.5 K to 30O-ft (MHx) mnovwbtc Dipole. 1500 K. Traveling (80 cm) 330-450 MHz 250 Feed amplifiers. Additional 50 K with Dicke switch.

300-350 300-350 Dual 5 K Frequency switching. When installed on the 300-ft traveling feed, 300-ft Cooled Op- 50 50 two feeds can be used: the 750-1000 MHz on New (MHz) 350-410 Orthogonal converter/ Cavity-backed the west end of the box and one of the others Trsvellng (90 ca) GASFET Aap Linear. 35ft-M6 Crossed on the east end. Selection of one of the two Feed Dual Channel 60 feeds should take less than 5 alnutes. To (80 ca) Dlpoles. Mount change a feed requires three hours. Coe Cooled Up- 500-750 300/140-ft 500-750 (MHz) converter/ 60 250 Scalar with When installed in the Sterling mount on (Shank) Sterling (48 cir) GASFET Amp Crossed the 140-ft or 300-ft antennas, only one Mount Uual Channel of the four feeds 300- 350 MHz 750-1000 Cooled Up- 70 250 750-1000 (MHz) converter/ 350- 410 MHz Scalar with 500- 750 MHz or (34 cm) GASFET Amp Crossed Dual Channel 750-1000 MHz Dlpoles. 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.

300/140-ft 1.30-1.50 Unoooled 90-100 200 max. 4 Horns. Linear. » 7 K (cal) Noise adding or Line or continuum from control room. Behrena (21 at, GaAsFET 77 min. «440K frequency switching. RF bandwidth variable from control room. 4 feed) 4 Channel Noise (Vrable) add

20 TECHNICAL DATA SHEEI No. 12 NOVEMBER 1984 PAGE 2 OF 4 System 3 dB Person Applicable Frequency Amplifier Feed Calibration Temperature Bandwidth Polarization Switching System Remarks in Telescope Type Type Value (GHz) (Kelvin) (MHz) Charge

Dual 140/300-ft 1.30-1.80 23-30 Up to 120 Three 2HE Orth. Linear 2 K Frequency switching Either circular or linear polarizations are Channel (19 cm) or and or selectable. Circular polarization requires Cooled FET (Chestnut) (23 ca) 1.30-1.36* Circular 200 K Noise adding. adjustments from the control room. (22 cm) 1.30-1.43 Band change requires feed change, 2 to 3 (18 cm) 1.60-1.72 hours. ♦Available 1984.

300/140-ft 2.695 Uncooled 130 120 3 Horns Circular or 4 K 300 K load or Brundage (11 cm, polarization, or GaAsFET DSB Linear on both polarizations. Four hours to change (Chestnut) 3-feed) 4 Channel beam. polarization.

300/140-ft 3.12-3.37 Cooled 60 K line and 250 Single Orth. Linear Cooled Dicke switches Continuum and line use. Feed change approxi¬ Brundage Paraaps load switched. Fixed Beam, or (latchliig ferrite) for mately 6 hours on 300-ft and 2 hours on 140-ft (9 cm) 4 K (Chestnut) Dual Channel 70 K polariza¬ Tuned Dual Orth. load (20 K) switching tion switched. Polarized Circular or beam/polarization and switching with noise 65 Kload 250 Dual Beams Identical Linear 14 K injection for balanc¬ switched. Fixed offset by or ing 10 Hz maximum 75 K beam Tuned 3 Identical rate. switched. HPBW, Circular stagy or polarized. Orth. Circular Orth. Circular 300/140-ft 4.47-5.04 Cooled Beam 1.4 K Other polarization. Includes cooled FET's for 1.0-1.45 GHz. Coe. GaAsFET 50-60 570 Identical or or (6 cm) Dual Beam Feed change required to go to 25 cm. (Shank) Dual Channel Offset Orth. Circular 12.8 K Beam switching. (6/25 Rx) or Identical 3 HPBW 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 Nutator Beam (5 cm) 4.7- 4.9 40-50 Two 4.9- 6.5 30-40 Receivers 6.5- 7.2 40-50 (Dunbrack)

7,6-11.2 Upconverter 35-80 60-300 Cassegrain Fixed Linear 3-7 K Frequency or 7.6- 8.5 50-80 (3 cm) Maser Circular VLB Nutator Beam 8.5-11.2 35-45

12.0-16.2 Upconverter 50-80 60-300 Cassegrain Fixed Linear 7-10 K Frequency or 12.0-16.2 50-80 (2 cm) Maser Nutator Beam

18.2-25.2 Maser 40-70 60-300 Cassegrain Fixed Linear 3-6 K Frequency or 18.2-25.2 40-70 (1.4 cm) Circular VLB Nutator Beam

21 TECHNICAL DATA SHEET No. 12 NOVEMBER 1984

System Continuum Applicable Frequency Amplifier 3 dB Feed Calibration Switching Person Telescope (GHz) Type Temperature Sensitivity Polarization 0Celvin) (Jansky Vsec) Bandwidth Type Value System Remarks in Charge

12-m 70-115 Cooled 280-500 3 650 MHz Horn-Lens Dual 10 K Nutating Mixer SSB Cochran Linear Subreflector

12-m 200-270 Cooled 500-1000 5 600 MHz Horn-Lens Dual - Mixer SSB at 230 GHz Nutating Range will be extended from 270- Payne Linear Subreflector 300 later in 1984.

22 TECHNICAL SATA SHEET No. 12 NOVEMBER 1984 PAGE 4 OF 4

System 3dB Person Applicable Frequency Amplifier Feed Calibration Temperature Bandwidth Polarization Switching System Remarks in Telescope Type Type Value (GHz) (Kelvin) (MHz) Charge

VLA 300— Uncooled 250 3 MHz Prime Dual 25 Noise injection, On antennas 8, 12, and 15 only. LUie 350 Transistor limited by Focus Orthogonal 9.6 Hz, This system is a prototype undergoing interference) (offset) Circular 50 percent cycle. development.

VLA 1340- Cooled 60 55 Cassegrain Dual 4 Noise injection, Lilie 1730 FET Orthogonal 9.6 Hz, Circular 50 percent cycle.

VLA 4500- Cooled 60 55 Cassegrain Dual 4 Noise injection, LUie 5000 Paramp or Orthogonal 9.6 Hz, Cooled Circular 50 percent cycle. Paramp and FET

VLA 14 400- Cooled 110 55 Cassegrain Dual 7 Noise injection, LiUe 15 400 FET Orthogonal 9.6 Hz, Circular 50 percent cycle.

VLA 22 000- Cooled 350 55 Cassegrain Dual 20 Noise injection, LUie 24 000 Mixer Orthogonal 9.6 Hz, Circular 50 percent cycle.

23 NRAO - Staff and Visitor Publications 1984

Abbott, D. C; Bieging, J. H.; and Churchwell, E. "The Detection of Variable, Nonthermal Radio Emission from TWo 0 Type Stars." Astrophys. J., 280, 671-678, 1984.

Altschuler, D. R.; Broderick, J. J.; Condon, J. J.; Dennison, B.; Mitchell, K. J.; (VDell, S. L.; and Payne, H. E. "Multifrequency Light Curves of Low-Frequency Variable Radio Sources." Astron. J., 89, 1784-1798, 1984.

Altschuler, D. R.; Glovanardi, C; Glovanelli, R.; and Haynes, M. P. "A 1405-MHz Continuum Survey of Dwarf Galaxies." Astron. J., 89, 224-230, 1984.

Andrews, M. D. and Basart J. P. "High-Resolution Radio Observations of Nonthermal Sources in the Rho Ophiuchus Dark Cloud." Astron. J., 89, 417-420, 1984.

Antonucci, R. R. J. "A Statistical Study of the Properties of Radio Galaxies." Astrophys. J., 281, 112-125, 1984.

Antonucci, R. R. J. "Optical Spectropolarimetry of Radio Galaxies." Astrophys. J., 278, 499-520, 1984.

Antonucci, R. R. J. and Ulvestad, J. S. " Can Have Double Radio Sources." Nature, 308, 617-619, 1984.

Archer, J. W. "An Efficient 200-290-GHz Frequency Tripler Incorporating a Novel Stripline Structure." IEEE Trans. Micro. Theory Tech., MTT-32, 416-420, 1984.

Archer, J. W. "A Novel Quasi-optical Frequency Multiplier Design for Millimeter and Submillimeter Wavelengths." IEEE Trans. Micro. Theory Tech., MTT-32, 421-427, 1984.

Archer, J. W. and Faber, M. T. "A Very Low-Noise Receiver for 80-120 GHz." Int. J. Infrared Mm. Waves, _5, 1069-1081, 1984.

Baan, W. A. and HaSchick, A. D. "The IC 4553: VLA-A Observations of the OH Megamaser." Astrophys. J., 279, 541-549, 1984.

Bania, T. M. and Lockman, F. J. "A Survey of the Latitude Structure of Galactic H I on Small Angular Scales." Astrophys. J. Suppl. Ser., 54, 513-545, 1984.

24 Bartel, N.; Shapiro, I. I.; Corey, B. E.; Marcaide, J. M.; Rogers, A. E. E.; Whitney, A. R.; Cappallo, R. J.; Ruhr, H.; Graham, D. A.; and Baath, L. "The Compact Radio Source 2021+614: Simultaneous 2.3 and 8.3 GHz Mark III VLBI Observations." Astrophys. J., 279, 116-121, 1984.

Barthel, P. D.; MLley, G. K.; Schilizzi, R. T.; and Preuss, E. "Compact Radio Cores in Extended Quasars." Astron. Astrophys., 140, 399-404, 1984.

Barvainls, R. and Clemens, D. P. "A Search for SiO Masers in Orion-Like Regions." Astron. J., 89, 1833-1835, 1984.

Becker, R. H. and Helfand, D. J. "New Radio Observations of the Composite Supernova Remnant G29.7-0.3." Astrophys. J., 283, 154-157, 1984.

Bennett, C. L.; Lawrence, C. R.; and Burke, B. F. "5 GHz Source Variability and the Gain of the NRAO 300-foot Telescope." Astrophys. J. Suppl. Ser., 54, 211-227, 1984.

Benson, J. M. and Johnston, K. J. "Arc-Second Resolution Maps of the Compact Sources in Sagittarius B2 and G34.3+0.2." Astrophys. J., 277, 181-188, 1984.

Benson, J. M.; Mutel, R. L.; and Gaume, R. A. "High Angular Resolution Observations of the OH Masers in W51 (Main)." Astron. J., 89, 1391-1397, 1984.

Bertola, F.; Casini, C; Bettoni, D.; Galletta, G.; Noreau, L.; and Kronberg, P. P. "NGC 3448 Revisited: A Combined Optical, Radio, and UV Investigation." Astron. J., 89, 350-355, 1984.

Bieging, J. H.; Cohen, M.; and Schwartz, P. R. "VLA Observations of T Tauri Stars. II. A Luminosity Limited Survey of Taurus-Auriga." Astrophys. J., 282, 699-708, 1984.

Bothun, G. D.; Margon, B.; and Balick, B. "An Unsuccessful Search for Very Extended Halos Around NGC 1300 and M 61." Publ. Astron. Soc. Pacific, 96, 583-587, 1984.

Bowers, P. F. "OH Maser Emission as a Probe of Circumstellar Envelope Structure." Cambridge Workshop on Cool Stars, 3, 356-358, 1984.

25 Bowers, P. F. "VLA Observations of 1612 and 1667 MHz OH Masers Associated with IRC +10420." Astrophys. J., 279, 350-357, 1984.

Bowers, P. F. and Hagen, W. "Luminosities and Mass Loss Rates of OH/H2O Maser Stars." Astrophys. J., 285, 637-647, 1984.

Bowers, P. F. and Morris, M. "The Three-Dimensional Structure of a Circumstellar Maser." Astrophys. J., 276, 646-652, 1984.

Bridle, A. H. "Sidedness, Field Configuration, and Collimation of Extragalactic Radio Jets." Astron. J., 89, 979-986, 1984.

Bridle, A. H. and Perley, R. A. "Extragalactic Radio Jets." Ann. Rev. Astron. Astrophys., 22, 319-358, 1984.

Broten, N. W.; MacLeod, J. M.; Avery, L. W.; Irvine, W. M.; Hoglund, B.; Friberg, P.; and Hjalmarson, A. "The Detection of Interstellar Methylcyanoacetylene." Astrophys. J., 276, L25-L29, 1984.

Brown, R. L. and Liszt, H. S. "Sagittarius A and Its Environment." Ann. Rev. Astron. Astrophys., 22, 223-265, 1984.

Bums, J. 0.; Basart, J. P.; De Young, D. S.; and Ghiglia, D. C. "Radio Jets in Classical Double Radio Jets in Classical Double Radio Sources with Strong Cores." Astrophys. J., 283, 515-528, 1984.

Campbell, B. "New Radio Sources at AFGL 2591: Young Cluster or Single Star?" Astrophys. J., 287, 334-337, 1984.

Campbell, B. "VLA Observations of Collimated Outflow at NGC 7538 IRS 1." Astrophys. J., 282, L27-L30, 1984.

Campbell, B. and Thompson, R. I. "Star Formation in the NGC 7538 Molecular Cloud: Near-Infrared and Radio Spectroscopy." Astrophys. J., 279, 650-663, 1984.

26 Canto, J.; Rodriguez, L. F.; Calvet, N.; and Levreault, R. M. "Stellar Winds and Molecular Clouds: Herbig Be and Ae Type Stars." Astrophys. J., 282, 631-640, 1984.

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Chanan, G. A.; Helfand, D. J.; and Reynolds, S. P. "An Optical Synchrotron Around the X-ray Pulsar 0540-693 in the Large Magellanic Cloud." Astrophys. J., 287, L23-L26, 1984.

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45 Additions to the 1983 Bibliography

Calvet, N.; Canto, J.; and Rodriguez, L. F. "Stellar Winds and Molecular Clouds: T Tauri Stars." Astrophys. J., 268, 739-752, 1983.

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