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NATIONAL RADIO ASTRONOMY OBSERVATORY
Observing Summary - 1979 Statistics
February 1980
NATIONAL RADIO ASTRONOMY OBSERVATORY
Observing Summary - 1979 Statistics
February 1980
Some Highlights of the 1979 Research Program
By the end of the year observations had been made at the VLA site with an array of 19 antennas. The longest astronomically usable baseline was approximately 24 km between antennas at 17.2 km on the southwest arm and at 10.5 km on the east arm. The first VLA scientific spectral line research was completed during the last quarter of the year.
As part of an extensive study of the dynamical properties of spiral galaxies of all luminosities along the Hubble sequence, the 300-ft telescope was used to survey a sample of high luminosity spirals having optical rotation curves which do not decrease at large distances from the nucleus. The search was carried out in an effort to determine if neutral hydrogen exists at radial distances of two to three times the optical image and if so at what rotational velocities. The presence of significant mass located at large nuclear distances is important for an under¬ standing of galaxy formation and evolution.
Up to seven antennas have been used in conjunction with the 140-ft telescope in a VLBI experiment designed to investigate the detailed structure of the peculiar galactic source SS 433. Elongated structure on the order of an arcsecond in size is apparently roughly aligned with the bulges in the surrounding HII region, W50. The alignment suggests that the two objects are related and pose interesting parallels with extragalactic jet radio sources which are many orders of magni¬ tude larger in size and mass.
The VLA was used in a series of experiments to map the radio brightness distribution of the re¬ gion around the double quasar 0957-561. The asymmetric radio picture is more complicated than the simple two-point optical one of two quasars with identical redshifts. Ultimately, it is hoped to be able to adequately test the hypothesis that these objects are gravitational lens images of a single object. Further monitoring for variability is, however, necessary.
Studies of the distribution of 12C0 and -^CO in ^^ Galaxy have continued in order to probe in detail the association between the atomic and molecular gas distributions. Molecular cloud sizes, masses, typical separations, and radial distributions are under investigation. ^CO molecular features near the galactic center region were further studied in order to pursue several predictions of the model which confines the inner-galaxy gas to a smooth, rotating and expanding, tilted disk.
Observing Hours 40
30 est. est. est. est. est.
o o o
x 20
o in
est.
;&-ggj 'M8&
1970 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85
Calendar Year
1300-Foot 140-Foot ^M36-Foot WJ\ Interferometer ilil/Z./?
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
o o o
1970 71 72 73 74 75 76 77 78 79 1970 71 72 73 74 75 76 77 78 79 1970 71 72 73 74 75 76 77 78 79
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 tests 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
60
Q_ 40
20-
- A A 4 ^ A r A r — A / A /" ^ /"
- i /
^* A /
/**
\ A S \ A r ^ ^ 1 /
y \l
/ \
[I 1 ^
V f \
W ^
\ A,
/
- A ti / V / \ W V
A I V
A fl
-
- / \l t j
A u \ V \ ,.. y /
V \
/^
\ /
j \ \ • A \ /
A y 1 V \ I / t ̂. J. „ / \)
** V / /
f V J v.- > / >
5/ -•*>. -«*> 1 — V, rfr» 1 T 7 .y \ J / ._«' t J \.
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.
140-Foot Radio Telescope Summary 100
80
r 60
40
20
>N V, ^v r ^_
^ ^_
/ ■N
\/ /^ ̂ S v < /■ A /" ̂ A s /-
-" s~ ^
- >• A / A /
f V
V A s/ V
-
-
^ lO" f
-
- j \ / \ A V A
-
v.- S
/N CM
V- / V — ^
■— ..— ^ V
- ^\
V- ̂ / v ^7 V ̂ s V
'"v. . -*»*d - -
1970 1971 ' 1972 ' 1973 ' 1974 1975
Calendar Year
1976 1977 1978 1979
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: 1972 - new control computer and resetting surface; 1974 - installation of the cassegrain system; 1977 - data processing computer and installation of the maser cassegrain system; and 1978 - tests of the deformable subreflector.
300-Foot Radio Telescope Summary 100
80
60
CD
^ 40
20
0
\ f v ^ , / /^ ̂ ^ - ^- ^v i r — -v
S^ ^ - ^ - \^ - — "N
V /^ **s A
V - A
^ \
V \ r s/ \
V /
- I -
- / /
A \
-
-y I / A V - —- J \ v < ̂ ^ X «*•»•.. ̂ - -—.-''~" ̂ — ̂
A \^ ss
^ -— ̂ /s ̂
-•i^
Calendar Year
Installation, Maintenance and Calibration Equipment Failure, Weather and Interference Observing —
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 resurfaced in 1970 and painted in 1973.
Very Large Array Telescope Summary
During 1979 the principal activity at the VLA site in New Mexico continued to be the construc¬ tion and installation of the array. With the completed portion of the array the limited program of tests, calibrations, and observations that was begun in previous years was greatly expanded, using up to 19 antennas. Observing frequencies included 1400-1700 MHz, 5000 MHz, 15 GHz, and 22 GHz.
Throughout 1979, approximately 1209 hours were scheduled for test and calibration, and fully 2464 additional hours were scheduled for research programs involving 159 observers. A total of 136 visitors and students used the VLA during 1979.
Full-Time Permanent Employees
e
450
400
350
300
250
200
150
100
50
\\/LA Construction
| Research and Operations
1111111111111111111111111 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 \ ., /\ /
Fiscal Year Calendar Year
Fig. 6. 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
Calendar Year
Fig. 7. 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.
Distribution of Telescope Time by Per Cent (Excluding VLA)
Visitors
Students
Permanent Staff
Research Associates
Test and Calibrate
Maintenance and Installation
Holidays and Unscheduled
36-Foot 140-Foot 300-Foot 1979 Summary
56% 48% 39% 48%
8 7 21 12
11 15 17 14
0 16 8 8
7 4 6 6
17 9 7 11
10
Institutions from which Visitors Came to Use NRAO Telescopes during 1979
Telescope
Institution 36-ft 140-ft 300-ft VLA
1. Aerospace Corporation 2. American Science and Engineering 3. Arcetri Astrophysical Observatory, Italy 4. Arizona, U. of 5. Arizona State U.
6. Bell Telephone Laboratories 7. Berkeley, U. of California 8. Bo chum, U. of, W. Germany 9. Bowling Green State U.
10. Brandeis U.
x x
11. British Columbia, U. of, Canada 12. California Inst, of Technology 13. Carter Obs., New Zealand 14. Chalmers U. of Tech., Sweden 15. Chicago, U. of
x x
16. Columbia U. 17. Copernicus, U. of, Poland 18. Cornell U. 19. CSIRO, Australia 20. Davis, U. of California
x x X
X X
21. DTM, Carnegie 22. ESO, Switzerland 23. Florida, U. of 24. Fordham U. 25. George Mason U.
11
Institution 36-ft
Telescope
140-ft 300-ft VLA
26. Hale Obs. 27. Harvard, Center for Astrophysics 28. Hawaii, U. of 29. Haystack Research Facility 30. Helsinki, U. of, Finland
31. Herzberg Inst., Canada 32. Illinois, U. of 33. Institute for Advanced Study, Princeton 34. Institute for Space Research, Moscow, USSR 35. Institute of Astronomy, Cambridge, UK
36. Iowa, U. of 37. Jet Propulsion Laboratory 38. JILA, Boulder 39. Jodrell Bank, England 40. Kapteyn Lab, Groningen, Netherlands
x x
41. Kentucky, U. of 42. Kitt Peak National Observatory 43. Laboratorio di Radio Astronomy, Bologna, Italy 44. Lick Observatory 45. Leiden Observatory, Netherlands
46. Lockheed Research Lab 47. Manhattan College 48. Maryland, U. of 49. Massachusetts, U. of 50. Massachusetts Inst, of Tech.
x x X
12
Institution 36-ft
Telescope
140-ft 300-ft VLA
51. Max-Planck I.R., Bonn, W. Germany 52. Mexico, Institute of Astronomy 53. Milano, U. of, Italy 54. Minnesota, U. of 55. NASA-Goddard (Greenbelt)
x x
X X
X X
X X
56. NASA-Inst. for Space Studies (NYC) 57. National Astronomy and Ionosphere Center 58. National Bureau of Standards 59. National Geodetic Survey 60. Naval Research Lab
x
x
X
X X X X X
61. National Science Foundation (D.C.) 62. Netherlands Foundation for Radio Astronomy 63. Nevada - Las Vegas, U. of 64. New Mexico I.M.T. 65. North Carolina, U. of
x x X
66. Northwestern U. 67. Pennsylvania, U. of 68. Penn State U. 69. Pittsburgh, U. of 70. Queen's U., Canada
71. Rensselaer Polytechnic Inst. 72. Rice U. 73. San Diego, U. of California 74. Smithsonian Astrophysical Obs. 75. SUNY, Stony Brook
x x
13
Institution
76. Stockholm, U. of, Sweden 77. Tennessee, U. of 78. Texas, U. of 79. Toronto, U. of, Canada 80. Tufts U.
81. U.S. Naval Obs. 82. Virginia, U. of 83. Virginia Polytechnic Inst, and SU 84. Washington, U. of 85. Wisconsin, U. of
36-ft
x x X
Telescope
140-ft 300-ft
x x X X X
X X X X
X
X
VLA
X X X X X
No. Institutions
No. Visitors
No. Students
No. Research Associates
No. Permanent Staff
Total Observers
37
108
53
184
19
58
46
80 142 32 119
17 20 14 17
1 4 4 7
159
All told, 343 visitors, including 59 students, from 85 institutions,
14
Doctoral Theses for Which Major Work Was Done at NRAO
1962 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 Calendar Year
Fig. 8. This bar chart shows the number of doctoral dissertations produced each calendar year by Ph.D. students where the major work on the theses was done at the NRAO.
15
NRAO Student Program
100
80
£ 60 £
40
20
££| Undergraduate
WCo-op ^ Summer Graduate
MPh.D.
2Z££
est. est. est. est. est. est.
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
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.
84 85
16
NRAO Front-End Box Status
TECHNICAL DATA SHEET
NOVEMBER 1979 io. 12 PAGE 1 OF 4
Applicable Telescope
Frequency (MHz)
Amplifier Type
System Temperature
(Kelvin)
3 dB Bandwidth
(MHz)
Feed Type Polarization
Calibration Value Switching System Remarks
Person In
Charge
300-ft Fixed on Traveling Feed
140-ft CUp-On
50-80
Transistor
*450 K - * 500 K with Dicke switch.
5 « 10% Bandwidth. Tunable Crossed-
Simultaneous 0*, 45*, 90', 135* Linear, RCP and LCP. Removable quad hybrid at feed for circular.
Adjustable 30 K to 30 000 K.
Removable diode Dicke switch.
Designed for pulsar, continuum, and line work. 110-500 MHz feeds can be manually rotated 45* and 90* for polarization work. UsaUe with 4- channel multi-bandwidth receiver and all NRAO line receivers. About 2 hours to change Dicke switch and feed hybrid. Frequency switching not availaUe.
Behrens/ Atkins
110-250 * 200 K - £ 260 K with Dicke switch.
140 Broadband Crossed- Dlpole.
Adjustable 8 K to 8000 K.
250-500
> 320 K. * 200 K with removaUe 330-450 MHz amplifiers. Additional 50 K with Dicke switch.
250
Broadband Crossed- Dipole.
Adjustable 1.5 K to 1500 K.
300-ft Fixed on Traveling Feed
140-ft
515-610 Tunable Paramp Ch X
> 150 20 to 40 Broadband Crossed- Dipole
Single linear; circular with removable quad hybrid. Dual polarization at 610 MHz.
5 K or 50 K
Frequency switching. RemovaUe Dicke switch. Adds ^ 40 K to T .
sys
Traveling feed box for 300-ft. Can be used on 140- ft. No box rotation. Multiple polarization with IF polarizer on 300-ft at 610 MHz. About 2 hours to change hybrid and Dicke switch. Feed can be manu¬ ally rotated 45* and 90* on l»x. Narrowband feed required above 670 MHz for best efficiency.
Brundage
610-740 Tunable Paramp Ch Y
300-ft Fixed on Traveling Feed
140-ft
740-880 Tunable Paramp Ch X
i 150 20 to 40 Broadband Crossed- Dipole.
Single linear; circular with removable quad hybrid. Dual polarization at 835 MHz.
5 K or 50 K
Frequency switching. Removable Dicke switch. Adds •». 40 K to T
sys
Traveling feed box for 300-ft. Can be used on 140-ft. No box rotation. Multiple polariza¬ tion with IF polarizer on 300-ft at 835 MHz. About 2 hours to change hybrid and Dicke switch. Feed can be manually rotated 45* and 90* on box.
Brundage
830-1000 Tunable Paramp Ch Y
300/140-ft 1000- 1450 Dual Channel
Cooled Upconverter
45 to 70 200 Single Beam Scalar
Orth. Linear 3.4 K Frequency switching. Part of 4.5-5.1 GHz receiver listed below. Feed change required to go to 6 cm.
Coe
17
TECHNICAL DATA SHEET NOVEMBER 1979
No. 12 PAGE 2 OF H
ApplicaUe Telescope
Frequency (MHz)
Amplifier Type
System Temperature
(Kelvin)
3dB Bandwidth
(MHz)
Feed Type
Polarization Calibration
Value Switching System Remarks Person
in Charge
140/300-ft 1410 Dual Channel
Cooled Paramp
50 25 Scalar Orth. Linear 4 K Frequency switching. Can be remotely tuned anywhere in frequency range 1375-1435 MHz. Two channels can be used simultaneously at different frequencies. Six polarizations are availaUe simultaneouBly with IF polarlmeter. Will tune 1370-1440 MHz with higher noise temperature outside range 1375-1435 MHz.
Behrens
80 Zeeman Orth. Linear or Circular
140/300-ft 1610- 1720 Dual Channel
Cooled Paramp
60 30 Scalar Orth. Linear 3.4K/15K Frequency switching. Can be remotely toned anywhere in frequency range 1610-1720 MHz. Two channels can be used simultaneously at different frequencies. Six polarizations are availaUe simultaneously with IF polarlmeter. Willtune 1540-1780 MHz with higher noise temperature outside range of 1610-1720 MHz.
Wu
140/300-ft 1000 to 2000
Paramp 175 to 300 20 to 60 1-2 GHz Scalar
Linear 10 K 300 K load or frequency switching.
Set of seven tunable paramps in two receiver boxes. Paramp change 2 hours. Receiver change
Dunbrack
140/300-ft 2000 to 4000
Paramp 220 to 450 130 between 2295 to 2380 MHz.
30 to 100 2-4 GHz Scalar
Linear 10 K 300 K load or frequency switching.
4 nours. Rx 1: 1.0-1.15 Rx2: 2.0-2.54
2.1-2.4
Micromega 13 cm installed.
1.16-1.3 1.3-1.7 2.5 -3.15 3.4-3.7 2.6 -3.1 3.3-3.9
paramp (2995 MHz)
1.62-2.0 Paramps. LO Multi¬
pliers, can be
300/140-ft 2695 x 4 Degenerate Paramp
120 100 DSB
3 Horns Circular or Linear
4 K 300 K load or polarization.
Continuum receiver. On-axin horn has paramps on both polarizations. Fbur hours to change polarization.
Wu
300/140-ft 3120- 3370 Dual Channel
(9 cm)
Cooled Paramps
60 K line and load switched. 70 K polariza¬ tion switched.
250 Fixed Tuned
Single Beam, Dual Polarized
Orth. Linear or Orth. Circular 4 K
and
14 K
Cooled Dicke switches (latching ferrite) for load (20 K) switching or beam/polarization switching with noise injection for balancing, 10 Hz maximum rate.
Contiiniuni and line use. Feed change approxi¬ mately 6 hours on 300-ft and 2 hours on 140-ft.
Brundage
65 K load switched. 75 K beam switched.
250 Fixed Tuned
Dual Beams offset by
3 HPBW,
singly polarized.
Identical Linear or identical Circular or Orth. Circular
300/140-ft 4500- 5100 Dual Channel
Cooled Paramp
70 580 Orth. Circular
1.4 K Other polarization, cold load.
Includes cooled upconverter for 1.0—1.45 GHz. Coe
18
TECHNICAL DATA SHEET
NOVEMBER 1979 No. 12 PAGE 3 OF 1
Applicable Telescope
Frequency (MHz)
Amplifier Type
System Temperature
(Kelvin)
3 dB Bandwdith
(MHz)
Feed Type
Polarization Calibration
Value Switching System Remarks
Person in
Charge
Any 4800- 5100
Paramp 150 20 w 10 K Dicke switch available. Packaged in small temperature-controlled box. Can be installed on other telescopes with little effort.
140-ft 6035 Paramp « 125 120 Scalar Linear or Circular
« 10 K Frequency or polarization.
Noise adding available. Brockway
140-ft 8.2-8.5 GHz
Cooled Paramp
65 line 85 continuum
125 Conical Horn
Linear or Circular
« 9 K Frequency or off-axis beam.
Two hours to change switch; 1/2 hour to change polarization.
Brockway
140-ft 5.2-10.4 GHz
Paramps 300 to 400 40 Horn Linear ■ » 20 K Frequency switching. Set of 7 tunaUe paramps In 2 bands about 7 GHz. Paramp change 1-1/2 hours. Band change 3 hours. Band 1: 5.2-5.8 5.8-6.4 6.4-7.0 Band 2: 7.0-7.8 7.8—8.6 8.6-9.5 8.5—10.4 Circular polarization availaUe at select fre¬ quencies.
Brockway
Any 10 695 Paramp 250 20 » 10 K Dicke switch availaUe. Packaged in small temperature-controlled box. Can be installed on other telescopes with little effort.
140-ft 10 300- 11000
TRG Cooled Paramp
120 continuum 70-90 line
200 2 Horns or Scalar
Dual Linear or Orth. Linear/
Circular
« 7 K Other polarization, other beam, or 25 K load.
Two feed arrangements availaUe: (1) Scalar and (2) dual horns for beam switching. Band¬ width and noise varies with center frequency. Two hours to change switch.
Behrens
140-ft 14.4-14.9 GHz Dual Channel
Cooled Paramp
100-150 Ch. A-
500 MHz Ch. B-
100 MHz
2 Horns
or
Scalar
Orth. Linear/ Circular
or Dual Circular/
Linear
« 20 K Frequency, beam, or polarization switching.
Two feeds availaUe: Two off-axis horns or dual polarization scalar.
Ch. A - 14.36 to 14.88 GHz. Ch. B - 14.50 to 14.93 GHz.
Moore
140-ft 12.4—18 GHz
TDA's 1000 to 1300
50 Horn Linear w 10 K Off-axis beam. Contains LO system tunable 12.4—18 GHz. Three TDA's to cover the band: 12.4-14.5, 14.5-16.0, and 16.0-18.0.
Brockway
19
TECHNICAL DATA SHEET
NOVEMBER 1979 No. 12 PAGE H OF H
Applicable Telescope
Frequency (MHz)
Amplifier Type
System Temperature
(Kelvin)
Continuum Sensitivity
(Janaky^sec)
3dB Bandwidth
(MHz)
Feed Type
Polarization Calibration
Value Switching
System Remarks Person
in Charge
Freund 36-ft 31.4
GHz Mixer 600 DSB
(Each 2.3 1 GHz Cassegrain
and Horn Dual Linear
< 10 K Nutating sub- reflector or mech. switch
Continuum receiver. Four channels with two feeds each receiving orthogonal linear polarizations.
36-ft 80-120 GHz
Cooled Mixer
280-500 SSB per channel
2.8 500 MHz Cassegrain Horn and Lens
Dual Linear
* 10 K Nutating subreflector
Line or continuum. Two channels receive orthogonal linear polariza¬ tions. The second LO in one channel is variable, allowing channels to be separated by up to 500 MHz. An image rejection filter is availaUe for calibrated spectral line work. Quasi-optical polarization switching is availaUe for both line and continuum.
Cochran
36-ft 140-170 GHz
Cooled Mixer
1000 SSB 15 500 MHz Cassegrain Horn and Lens
Linear < 5K Nutating subreflector
Single channel cooled mixer receiver. Quasi-optical LO injection system.
Payne
20
NRAO - Staff and Visitor Publications 1979
Altenhoff, W.J.; Oster, L.; and Wendker, H.J. "The Radio Emission of Betelgeuse." Astron. Astrophys., 73, L21-L23, 1979.
Archer, J.W. "TEon-Mode Filters for the V.L.A. Circular Waveguide System." Elec. Lett., 15, 343-345, 1979.
Avery, L.W.; Oka, T.; Broten, N.W.; and MacLeod, J.M. "Cyanodiacetylene (HC5N) in Sagittarius B2." Astrophys. J., 231, 48-54, 1979.
Baker, P.L. and Burton, W.B. "Self-Absorption and Other Characteristics of High-Angular-Resolution Emission Spectra of Galactic HI." Astron. Astrophys. Suppl. Ser., 35, 129-152, 1979.
Bania, T.M. "Carbon Monoxide and the 3-Kpc Arm Feature." IAU Symp., 84, 351-356, 1979.
Baud, B.; Habing, H.J.; Matthews, H.E.; and Winnberg, A. "A Systematic Search at 1612 MHz for OH Maser Sources I Survey Near the Galactic Centre." Astron. Astrophys. Suppl. Ser., 35, 179-192, 1979.
Baud, B.; Habing, H. J.; Matthews, H.E.; and Winnberg, A. "A Systematic Search at 1612 MHz for OH Maser Sources II. A Large-Scale Survey between 10° < Jl £150° and |fe|x4*2." Astron. Astrophys. Suppl. Ser., 36, 193-211, 1979.
Beichman, C.A.; Becklin, E.E.; and Wynn-Williams, C.G. "New Multiple Systems in Molecular Clouds." Astrophys. J., 232, L47-L51, 1979.
Benson, J.M. and Mutel, R.L. "Multibaseline VLBI Observations of the 1612 MHz OH Masers Toward NML Cygni and VY Canis Ma joris." Astrophys. J., 233, 119-126, 1979.
Benson, J.M.; Mutel, R.L.; Fix, J.D.; and Claussen, M.J. "The Spatial Structure of a New OH Maser Feature in IRC +10420." Astrophys. J., 229, L87-L90, 1979.
Bowers, P.F.; Kerr, F.J.; Rnapp, G.R.; Gallagher, J.S.; and Hunter, D.A. "Upper Limits on the Gas Content of Southern Globular Clusters." Astrophys. J., 233, 553-557, 1979.
Bowers, P.F. and Kundu, M.R. "Observations of a Orionis, R Aquilae, and R Aquarii at 14.9 GHz." Astron. J., 84, 791-795, 1979.
Bridle, A.H.; Davis, M.M.; Fomalont, E.B.; Willis, A.G.; and Strom, R.G. "Structure and Polarization of Jets in the Giant Radio Galaxy NGC 315." Astrophys. J., 228, L9-L14, 1979.
21
Bridle, A.H. and Fomalont, E.B. "Radio Structure and Optical Identification pf 3C319." Astron. J%, 84, 1679-1682, 1979.
Bridle, A.H.; Fomalont, E.B.; Miley, G.K.; and Valentijn, E.A. "The Radio Properties of the X-ray Cluster Abell 2256." Astron. Astrophys., 80, 201-211, 1979.
Broderick, J.J.; Ficenec, J.R.; Teplitz, D.C; and Teplitz, V.L. "Observational Limits on the Magnetic-Monopole Structure of Protons." Phys. Rev. D, 19, 1046-1050, 1979.
Brown, R.D.; Godfrey, P.D.; Storey, J.W.V.; Bassez, M.-P.; Robinson, B.J.; Batchelor, R.A.; McCulloch, M.G.; Rydbeck, O.E.H.; and Hjalmarson, A.G. "A Search for Interstellar Glycine." Mon. Not. Roy. Astron. Soc., 186, 5P-8P, 1979.
Brown, R.L. and Spencer, R.E. "21 Centimeter Absorption at z=0.395 in the Quasar 1229—021." Astrophys. J., 230, L1-L4, 1979.
Burns, J.0. and Owen, F.N. "Radio Sources in Zwicky Clusters of Galaxies. II. Detailed Interferometer Observations and Analysis." Astron. J., 84, 1478-1499, 1979.
Burns, J.0.; Owen, F.N.; and Rudnick, L. "The Wide-Angle Tailed Radio Galaxy 1159+583: Observations and Models." Astron. J., 84, 1683-1693, 1979.
Burton, W.B. and Liszt, H.S. "HI in the Inner Few Kiloparsecs of the Galaxy." IAU Symp., 84, 325-336, 1979.
Burton, W.B. and Moore, R.L. "The Local Nature of the Anticenter Anomalous-Velocity Streams and Their Focus." Astron. J., 84, 189-198, 1979.
Clark, B.G. "Digital Processing Methods for Aperture Synthesis Observations." IAU Colloq., 49, 113-120, 1979.
Clark, F.O.; Biretta, J.A.; and Martin, H.M. "A Rotational Explanation of the High-Velocity Molecular Emission from the Orion Molecular Cloud." Astrophys. J., 234, 922-931, 1979.
Clark, F.O.; Lovas, F.J.; and Johnson, D.R. "Dimethyl Ether in Orion." Astrophys. J., 229, 553-559, 1979.
Clark, F.O.; Martin, H.M.; and Biretta, J.A. "General Calculations of Rotational Effects on Spectral Lines." Astrophys. J., 232, 624-635, 1979.
Cohen, M.H. and Readhead, A.C.S. "Misalignment in the Radio Jets of NGC 6251." Astrophys. J., 233, L101-L104, 1979.
Condon, J.J.; Buckman, M.A.; and Machalski, J. "Optical Identifications of Flat-Spectrum Sources in the GB2 1400-MHz Survey." Astron. J., 84, 149-163, 1979.
22
Condon, J.J.; Buckman, M.A.; and Smith, M.G. "The Angular Size of the High-Redshift Quasar Q0000—398." Nature, 278, 530, 1979.
Condon, J.J.; Ledden, J.E.; O'Dell, S.L.; and Dennison, B. "318-MHz Variability of Complete Samples of Extragalactic Radio Sources." Astron. J., 84, 1-11, 1979.
Cordes, J.M. and Dickey, J.M. "Interstellar Scintillation and Compact Sources in Supernova Remnants." Nature, 281, 24-27, 1979.
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Additions to the 1978 Bibliography
Bridle, A.H. and Fomalont, E.B. "14.8-GHz Mapping of the Extended Radio Core in NGC 1167." Mon. Not. Roy. Astron. Soc, 185, 67P-71P, 1978.
Condon, J.J. "A Survey of Radio Properties of BL Lac Objects." In: Pittsburgh Conf. on BL Lac Objects. Ed. by A.M. Wolfe. (Pittsburgh: University of Pittsburgh, 1978) 21-38.
Gibson, D.M. and Hobbs, R.W. "A Search for Microwave Emission from Comet Bradfield (1978c)." Southwest Regional Conf. Astron. Astrophys. Proc, 4^ 31-40, 1978.
Gibson, D.M.; Owen, F.N.; and Hjellming, R.M. "Radio Emission from the RS Canum Venaticorum Binary RT Lacertae." Publ. Astron. Soc. Pacific, 90, 751-753, 1978.
Johnston, K.J. "Present Status of Radio Astrometry with Baselines * 35 km." IAU Colloq., 48, 175-178, 1978,
Shaffer, D.B. "VLBI Observations of BL Lacertae Objects." In: Pittsburgh Conf. on BL Lac Objects. Ed. by A.M. Wolfe. (Pittsburgh: University of Pittsburgh, 1978) 68-81.
Wardle, J.F.C. "A Survey of Radio Polarization and Variability in BL Lacertae Objects." In: Pittsburgh Conf. on BL Lac Objects. Ed. by A.M. Wolfe. (Pittsburgh: University of Pittsburgh, 1978) 39-52.
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