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NATIONAL RADIO ASTRONOMY OBSERVATORY Observing Summary - 1985 Statistics February 1986

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  • 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

    Calendar Year

    1976 77 78 79 80 81 82 83 84 85

    Calendar Year

    \NRAO Staff I Visitors

    1976 77 78 79 80 81 82 83 84 85

    Calendar Year

    IB Testing and Calibration

    1981 82 83 84 85

    Calendar Year

    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

    Calendar Year

    1982 1983 1984 1985

    •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

    Observing

    1978 1979 1980 1981

    Calendar Year

    1982 1983 1984 1985

    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

    80

    60

    o- 40

    20

    0

    "S KS -\ V

    /^ ̂ ^ A V

    - A V /

    r A f A V /- - ̂ - ^ "\ \, / A* ̂ -^ - ^ - v V \ U i- -

    V { V - -

    / \

    L A > \ -

    v_ SS / /\ \_ _^ ̂ N ^< ■—■ y

    /" ~N 7 \: ^

    A V -J — — ̂

    A ^ s - — -^ ̂

    >1 y — -—.

    •Observing

    Calendar Year

    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

    Calendar Year

    1982 1983

    — Construction Initial Observing and Testing

    1984

    • Observing

    1985

    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 Calendar Year

    89 90

    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% Circumstellar Shells, Supernova Remnants, Masers. Novae, Supernovae, and Stars

    7% 9% 27% 15%

    III. GALACTIC

    Galactic Structure, Center, Molecular Clouds, HII Regions, Star Formation, Molecules, and Interstellar Medium

    45% 33% 5% 15% 25%

    IV. EXTRAGALACTIC —

    Normal and Active Galaxies, Radio Galaxies, Clusters, Quasars, VLB Studies, Extra- galactic Molecules, and Cosmology

    34% 56% 81% 53% 56%

    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 22. California, U. of, Los Angeles 23. California, U. of, Santa Cruz - Lick Obs. 24. Caltech - OVRA, Mt. Palomar 25. Cambridge Univ. - Cavendish, Mullard, IOA

    x X

    X X X X X

    13

  • Institution 12-m

    Telescope

    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) 32. Chicago, U. of - Yerkes Obs. 33. CIerason Univ. 34. CSIR (Johannesburg, S. Africa) 35. Colgate Univ. (NY)

    x x X X

    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

  • Institution 12-m

    Telescope

    140-ft 300-ft VLA

    51. George Mason Univ. (VA) 52. Gottingen Acad. Sci. (FRG) 53. Grenoble, U. of (France) 54. Gronlngen, U. of - Kapteyn Lab. (Netherlands) 55. Hamburger Stemwarte (FRG)

    x x X X 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. 67. Iowa, U. of (Iowa City) 68. Iowa State Univ. (Ames) 69. IRAM (France) 70. Itapetinga Obs. (Brazil)

    x x X

    X X

    71. Johns Hopkins Univ. - Space Tel. Inst. 72. JPL - Goldstone (CA) 73. Kent, U. of (England) 74. Kentucky, U. of 75. KPNO - Kitt Peak Nat. Obs.

    x x

    X X

    15

  • Institution 12-m

    Telescope

    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 82. Manchester, U. of - Jodrell, Nuffield 83. Marseille Obs. (France) 84. Maryland, U. of - (Hark Lake Obs. 85. Massachusetts, U. of - Five College Obs.

    x X X X X

    86. Meudon Obs. (France) 87. Mexico, U. of - Inst, of Ast. (Mexico) 88. Michigan, U. of (Ann Arbor) 89. Milano (Italy) 90. Minnesota, U. of

    x x

    X 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

  • Institution 12-m

    Telescope

    140-ft 300-ft VLA

    101. NAIC - Arecibo Obs. (P.R.) 102. Nanking, U. of (China) 103. NASA, Ames (CA) 104. NASA, Goddard - GSFC (Greenbelt, MD) 105. NASA, Inst, for Space Studies (NY)

    x x X X

    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) 122. Penn State Univ. 123. Pittsburgh, U. of - Allegheny Obs. (PA) 124. Princeton Univ. - Inst. Adv. Studies (NJ) 125. Puerto Rico Univ.

    x x X X X

    17

  • Institution 12-m

    Telescope

    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) 142. Texas, U. of, Austin - McDonald Obs. 143. Tokyo Univ. - Tokyo Ast. Obs. (Japan) 144. Toronto, U. of - D. Dunlap Obs. (Canada) 145. Tufts Univ. (MA)

    x x X X 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

  • Institution 12-m

    Telescope

    140-ft 300-ft VLA

    151. Victoria, U. of (Canada) 152. Virginia, U. of 153. VPI & SU 154. Washington, U. of 155. Williams College (MA)

    x x 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 No. of Students No. of Research Associates No. of Permanent Staff

    97 156 35 451 18 29 12 80 2 0 3 8

    Total Observers 128

    All told, 675 visitors, including 110 students, from 158 institutions.

    202 55 572

    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 NOVEMBER 1985

    No. 12 PAGE 1 OF

    Appllcftble Tdwoope

    Frequency 500 K 25 Fat

    Dipole Single Linear E-W.

    Adjustable 8 K to 8000 K.

    Reaovable diode Dicke switch. Reference tea- perature adjust¬ able froa 300 K to 40000 K.

    Designed for pulsar, continuua, and line work. About 2 hours to change Dicke switch and feed hybrid. Frequency switching not available. Usable with 4-channel aultl- bandwidth receiver, all NRAO line receivers and digital continuua receiver.

    Coe

    (Oliver) 300-ft Traveling Feed

    or

    140-ft Clip-On

    50-80 MHz

    (4.6 a)

    * 450 K - i 500 Kwtth Dicke switch.

    2.5-4.0

    « 5X Bandwidth.

    Crossed- Dtpole.

    Orthogonal Linear or reaovable quad hybrid at feed for RCP and LCP. 110-250 MHz

    (1.7 ca) 2 200 K- 2 260 K with Dicke switch.

    140 Broadband Crossed- Dtpole.

    300-ft Traveling Feed

    or

    140-ft Clip-On

    250-500 MHz (80 ca)

    Transistor Dual- Channel

    i 320 K. > 200 K wtth reaovable 330-450 MHz aapllflers.

    250

    Broadband Crosaed- Dtpole.

    Orthogonal Linear or reaovable quad hybrid at feed for RCP and LCP.

    Adjustable 1.5 K to 1500 K.

    Reaovable diode Dicke switch. Designed for pulsar, continuua, and line work. About 2 hours to change Dicke switch

    and feed hybrid. Frequency switching not available. Usable with 4-channel aultl- bandwidth receiver, all NRAO line receivers and digital continuua receiver.

    Coe

    (Oliver)

    450-500 MHz

    FCT top 50-80 K 50

    300-ft New Trsveltng Feed Mount

    300/140-ft Sterliac Mount

    280-350 MHz Cooled Up- converter/ GASFET Aap Dual Channel

    45-85 50 280-350 350-410 450-500

    Cavity-backed Crossed dlpoles.

    Dual Orthogonal Linear. IF Polariaeter or RF Hybrid for right and left circular polarization.

    5 K Frequency switching. When installed on the 300-ft traveling feed, two feeds can be used: the 750-1000 MHz on the west end of the box and one of the others on the east end. Selection of one of the two feeds should take less than 5 ainutes. To change a feed requires three hours. Coe

    (Shank)

    350-410 MHz (80 ca) 60

    450-500 MHz (60 ca)

    Cooled Up- converter/ GASFET Aap Dual Channel

    50-70 250 500-750 Scalar with Crossed

    When installed in the Sterling aount on the 140-ft or 300-ft antennas, only one of the five feeds

    280- 350 MHz 350- 410 MHz 450- 500 MHz 500- 750 MHz or 750-1000 MHz

    can be used. To change feeds requires two hours on the 140-ft and three hours on the 300-ft.

    500-750 MHz (48 ca)

    750-1000 MHz (34 ca)

    Cooled Up- converter/ GASFET Aap Dual Channel

    50-90 250 750-1000

    Scalar with Crossed Di poles.

    300/140-ft 1.00-1.45 (25 cu)

    (6/25 Rx)

    Cooled FET Dual Channel

    35 to 40 450 Single Beam Scalar.

    Orthogonal Linear.

    8K to 14 K

    Frequency switching. Noise adding.

    Part of 4.5-5.1 GHz receiver listed below. Feed change required to go to 6 cm.

    Coe

    (Shank)

    21

  • TECHNICAL DATA SHEET

    NOVEMBER 1985 No. 12 PAGE 2 OF 4

    Applicable Telescope

    Frequency (GHz)

    Amplifier Type

    System Temperature

    (Kelvin)

    3 dB Bandwidth

    (MHz)

    Feed Type

    Polarization Calibration

    Value Switching System Remarks Person

    in Charge

    140/300-ft 1.30-1.80 (19 ca) (23 ca) (22 ca) (18 ca)

    Dual Channel Cooled FET

    23-30 Up to 120

    Feed Liaited

    Three 2HE Single Beaa

    1.30-1.36 1.36-1.43 1.60-1.72

    Orth. Linear or Circular

    2 K and 200 K

    Frequency or polarization switching or noise adding.

    Either circular or linear polarizations are selectable. Circular polarization requires adjustments horn the control room. Band change requires feed change, 2 to 3 hours.

    Norrod

    (Chestnut)

    300/140-ft 2.695 (11 ca. 3-feed)

    Uneooled GaAsFET 4 Channel

    130 120 DSB

    3 Horns Circular or Linear

    4 K 300 K load or polarization, or beam.

    Continuum receiver. On-axis horn has receivers on both polarizations. Four hours to change polarization.

    Bradley

    (Chestnut)

    300/140-ft 2.9-3.5 (9 ca)

    (10 ca)

    Dual Channel Cooled FET

    25-35 Up to 200 Feed liaited.

    Two 2HE Single Beaa 2.90-3.15 3.15-3.40

    Orthogonal Linear and Circular

    Low 1.8 High 150

    Frequency switching. Noise adding.

    Band change requires feed change i 2-3 hrs. Circular polarization requires phase equaliz¬ ing adjustaents froa the control rooa. Frequency switching requires 50 as blanking tiae..

    Bradley

    (Chestnut)

    300/140-ft 3.12-3.37

    (9 ca)

    Cooled Paraaps Dual Channel

    65 Kload switched. 75 K beam switched.

    250 Fixed

    Tuned

    Dual Beams offset by

    3 HPBW, singly

    polarized.

    Identical Linear or Identical Circular or Orth. Circular

    4 K

    and

    14 K

    Cooled Dicke switches (latching ferrite) for load (20 K) switching or beaa switching with noise injection for bal¬ ancing; 10 Hz aaxi¬ aua rate.

    Continuua use. Behrens (Jeffries)

    300/140-ft 4.47-5.05 (6ca)

    (6/25 Rx)

    Cooled GaAsFET Dual Channel

    50-60 580 Single Orth. Circular

    or Orth. Linear 1.4 K or 12.8 K

    Other polarization. Includes cooled FET's for 1.0—1.45 GHz. Feed change required to go to 25 cm.

    Coe.

    (Shank) Dual Beaa Offset 3 HPBW

    Identical or Orth. Circular or Identical Linear

    Beam switching.

    140-ft Cassegrain

    Two Receivers

    4.7-7.2

    (5 ca)

    Upconverter Maser

    30-50 60-300 Cassegrain Fixed Linear Circular VLB

    3-7 K Frequency or Mutator Beam

    T Frequency 8y8z

    4.7- 4.9 40-50 4.9- 6.5 30-40 6.5- 7.2 40-50

    Brockway

    (Dunbrack)

    7.8-11.2 (3 ca)

    Upconverter Maser

    35-80 60-300 Cassegrain Fixed Linear Circular VLB 3-7 K

    Frequency or Nutator Beam

    7.6- 8.5 50-80 8.5-11.2 35-45

    12.0-16.2 (2 ca)

    Upconverter Maaer

    50-80 60-300 Cassegrain Fixed Linear 3-7 K Frequency or Nutator Beam

    12.0-16.2 50-80

    18.2-25.2 (1.4 ca)

    Maser 40-70 60-300 Cassegrain Fixed Linear Circular VLB

    2-6 K Frequency or Nutator Beam

    18.2-25.2 40-70

    22

  • TECHNICAL DATA SHEET

    NOVEMBER 1985 No. 12 PAGE 3 OF H

    AppUcaUe Telescope

    Frequency (GHz)

    Amplifier Type

    System Temperature

    (Kelvin)

    Continuum Sensitivity

    (Jansky /sec)

    3 dB Bandwidth

    Feed Type Polarization

    Calibration Value

    Switching System Remarks

    Person in

    Charge

    12-m 70-116 Cooled Mixer

    260-400 SSB

    1.0 650 MHz Horn-Lens Dual Linear

    10 K Nutating Subreflector

    Cochran

    12-a 90-115 SIS Approx. 100 To be 650 MHz Horn-Lens Dual

    Linear 10 K Nutating Subreflector Laab

    12-a 330-360 Cooled Mixer

    1400-2000 SSB 12 650 MHz Horn-Lens

    Single Linear -

    Nutating Subreflector Payne

    12-m 200-270 Cooled Mixer

    500-1000 SSB

    6 at 230 GHz

    600 MHz Horn-Lens Dual Linear

    - Nutating Subreflector

    Range will be extended to 270- 300 later in 1985.

    Payne

    23

  • TECHNICAL DATA SHEET

    NOVEMBER 1985 No. 12 PAGE 4 OF 4

    Applicable Telescope

    Frequency (GHz)

    Amplifler Type

    System Temperature

    (Kelvin)

    3dB Bandwidth

    (MHz)

    Feed Type Polarization

    Calibration Value Switching System Remarks

    Person in

    Charge

    VLA 308- 343

    Uneooled Translator

    250*

    150**

    3 MHz (limited by

    interference)

    Priae Focus***

    Dual Orthogonal Circular

    25*

    10**

    Noise injection. 9.6 Hz. 50 percent cycle.

    * Antennas 8, 12, and 15. ** Six other antennas. *** Feed is off-axis on antennas 8 and 12.

    Lille

    VLA 1340- 1730

    Cooled FET

    60 55 Cassegrain Dual Orthogonal Circular

    4 Noise injection. 9.6 Hz,

    Lille

    VLA 4500- 5000

    Cooled

    Cooled Paramp and FET

    60 55 Cassegrain Dual Orthogonal Circular

    4 Noise injection, 9.6 Hz. 50 percent cycle.

    Lille

    VLA 14 400- 15 400

    Cooled FET

    110 55 Cassegrain Dual Orthogonal Circular

    7 Noise injection, 9.6 Hz. 50 percent cycle.

    Lille

    VLA 22 000- 24 000

    Cooled Mixer

    350 55 Cassegrain Dual Orthogonal Circular

    20 Noise injection, 9.6 Hz, 50 percent cycle.

    Lille

    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.

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    Waak, J. A.; Spencer, J. H.; Johnston, K. J.; and Simon, R. S. "Superluminal Re supply of a Stationary Spot in 3C 395?" Astron. J., 90, 1989-1991, 1985.

    Wadiak, E. J.; Wilson, T. L.; Rood, R. T.; and Johnston, K. J. "VLA Observations of Formaldehyde Emission from Rho Ophiuchi B." Astrophys. J., 295, 463-465, 1985.

    Walsh, D.; Lebofsky, M. J.; Rleke, G. H.; Shone, D.; and Elston, R. "Infrared Study and Classification of Optically Faint Steep-Spectrum Radio Sources." Mon. Not. Roy. Astron. Soc, 212, 631-643, 1985.

    Weiler, K. W. "Radio and X-ray Observations of Extragalactic Supernovae." In: Supernovae, Their Progenitors and Remnants. Ed. G. Srinivasan and V. Radhakrlshnan. (Bangalore: Indian Academy of Sciences, 1985) 23-45.

    Weinreb, S. "Analog-Filter Digital-Correlator Hybrid Spectrometer." IEEE Trans. Instrum. Meas., IM-34, 670-675, 1985.

    Weinreb, S. and Pospieszalski, M. "X-Band Noise Parameters of HEMT Devices at 300K and 12.5K." IEEE MTT-S Internat. Microwave Symp., 539-542, 1985.

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  • Wells, D. C. "NRAO's Astronomical Image Processing System." In: Data Analysis in Astronomy. Ed. V. Di Gesu et al. (New York: Plenum Press, 1985) 195-209.

    White, R. L. and Becker, R. H. "MWC 349: A Bipolar Nebula with a Very Hot Central Star." Astrophys. J., 297, 677-685, 1985.

    Williams, B. A. "MKW 10: A Group of Galaxies with a Compact Core." Astrophys. J., 290, 462-476, 1985.

    Willson, R. F. "VLA Observations of Solar Active Regions at Closely Spaced Frequencies: Evidence for Thermal Cyclotron Line Emission." Astrophys. J., 298, 911-917, 1985.

    Wilson, A. S.; Baldwin, J. A.; and Ulvestad, J. S. "Kinematics and Ionization of Extended Ionized Gas in Active Galaxies. I. The X-ray Luminous Galaxies NGC 2110, NGC 5506 and MCG -5-23-16." Astrophys. J., 291, 627-654, 1985.

    Wilson, A. S.; Samarasinha, N. H.; and Hogg, D. E. "Magnetic Fields in the 'Jet' of the Crab Nebula." Astrophys. J., 294, L121-L124, 1985.

    Windhorst, R. A.; Miley, G. K.; Owen, F. N.; Kron, R. G.; and Koo, D. C. "Sub-Millijansky 1.4 GHz Source Counts and Multicolor Studies of Weak Radio Galaxy Populations." Astrophys. J., 289, 494-513, 1985.

    Winnberg, A.; Baud, B.; Matthews, H. E.; Habing, H. J.; and Olnon, F. M. "OH/IR Stars Within 50 Parsecs of the Galactic Center." Astrophys. J., 291, L45-L50, 1985.

    Woodward, C. E.; Heifer, H. L.; and Pipher, J. L. "VLA Continuum Observations of Compact H II Regions." Astron. Astrophys., 147, 84-88, 1985.

    Wrobel, J. M.; Jones, D. L.; and Shaffer, D. B. "Parsec-Scale Radio Emission from the E/SO Galaxy NGC 3894." Astrophys. J., 289, 598-602, 1985.

    Wynn-Williaras, C. G. and Becklin, E. E. "The Infrared and Radio Morphology of the 'Hot-Spot' Galaxy NGC 2903." Astrophys. J., 290, 108-115, 1985.

    Wynn-Williams, C. G.; Becklin, E. E.; and Scoville, N. Z. "The 3 Kiloparsec Radio Disk and Halo of NGC 1068." Astrophys. J., 297, 607-610, 1985.

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  • Zheng, X. W.; Ho, P. T. P.; Reid, M. J.; and Schneps, M. H. "Molecular Clouds Associated with Compact H II Regions. II. The Rapidly Rotating Condensation Associated with ONI." Astrophys. J., 293, 522-529, 1985.

    Ziurys, L. M. and Turner, B. E. "Detection of Interstellar Rotationally Excited CH." Astrophys. J., 292, L25-L29, 1985.

    Ziurys, L. M. and Turner, B. E. "Detection of Interstellar Rotationally-Excited CH." In: Molecular Astrophysics. Ed. G. H. F. Diercksen, W. F. Huebner, P. W. Langhoff. (Dordrecht: Reidel, 1985) 591-601.

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  • Additions to the 1984 Bibliography

    Archer, J.W. and Faber, M.T. "Low-Noise, Fixed Tuned, Broadband Mixer for 200-270 GHz." IEEE MTT-S Int. Microwave Symp. Digest, 557-559, 1984.

    Green, D.A. and Gull, S.F. "Two New Young Galactic Supernova Remnants." Nature, 312, 527-529, 1984.

    Rodriguez, L.F. and Garcia-Barreto, J.A. "On the Abundance of Atomic and Molecular Hydrogen in the Outer Parts of Young Planetary Nebulae." Rev. Mexicana Astron. Astrof., J9, 153-157, 1984.

    Turner, B.E. "How Stars Form: A Synthesis of Modern Ideas." Vistas Astron., 27, 303-332, 1984.

    Yin, Q.; Heeschen, D.S.; and Heidmann, J. "VLA Observations of Markarian 8 at 6 cm Wavelength." Scientia Sinica A, 7, 750-756, 1984.

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