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1982 Statistics 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.
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