ObtervinfSummanj

National Radio 2000 atLsgf Astronomy Observatory

A facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

NATIONAL RADIO ASTRONOMY OBSERVATORY

Observing Summary 2000 Statistics

April 2001

Scientific Highlights ■El 0b$ervin?Jummanj2ooo i

Very Large Array (VLA) studies have revealed a paradox about pulsar ages. A multi-epoch study of pulsar B1757-24 and its associated radio supernova remnant G5.4-1.2 indicates that the pulsar may be much older than indicated by the "characteristic age" based on its spin-down rate. The pulsar has a calculated characteristic age of 16,000 years, but based on a VLA proper-motion study using 1993 and 1999 images, the pulsar appears to have taken about 39,000 years to move from the center of the supernova remnant to its present position. The result calls into question the determination of pulsar ages, with wide-ranging implications for the understanding of neutron stars, pulsars, and even particle physics.

• Powerful radio bursts from a brown dwarf have been discovered at the VLA by members of a student science project. Brown dwarfs, discovered only five years ago, are cool, dim objects with masses between that of Jupiter and the sun (about 8 percent of the solar mass). As such, their cores never become hot enough to ignite the fusion process that powers ordinary stars, so they are expected gradually to cool and fade after they form. Not only were the radio bursts from the brown dwarf much stronger than those from Jupiter, but follow-up observations showed that the object's magnetic field was surprisingly weak, since flares are normally powered by the energy in magnetic fields. These observations promise new understanding of the difference between true stars and brown dwarfs. For instance, the cooler cores of brown dwarfs might create less turbulence inside the dwarfs, and consequently weaker magnetic fields, but possibly with conformations that make them more likely to reconnect and produce flares.

• The first discovery of a simple sugar molecule in space was made by the 12 Meter Telescope. The sugar molecule glycolaldehyde was detected in a giant cloud of gas and dust near the Galactic Center where new stars are forming. This makes it likely that the chemical precursors to life

are formed in such clouds long before planets develop around stars. Glycolaldehyde is an 8-atom molecule with the structure HO-CH2-CHO, which can combine with other molecules to form the more complex sugars Ribose and Glucose. Ribose is a building block of nucleic acids such as RNA and DNA, which carry the genetic code of living organisms. Glucose is the sugar found in fruits. Glycolaldehyde contains exactly the same atoms, though in a different molecular structure, as methyl formate and acetic acid, both of which were detected previously in space. All three of these isomers are believed to catalyze on interstellar grains.

• Very Long Baseline Array (VLBA) observations of the Galactic black hole binary GRS 1915+105 have revealed the smallest synchrotron jet yet known. This compact jet, about 10 AU in length at the microquasar's core, is the first of its size imaged in any black hole binary. It is present continuously, reestablishing itself within eight hours of major radio outbursts. It increases in intensity about 30 minutes after dips in the core X-ray emission occur, suggesting that it is powered by injections of plasma from the accretion disk. The VLBA observations also show, at larger scales (~ 500 AU), superluminal motions of ejecta from outbursts associated with abrupt changes in the X-ray emission. The VLBA observations of this microquasar take advantage of its status as a unique laboratory for the study of both the plateau and flare states seen separately in other black hole binaries. Scientific Highlights Observinfiummariizooo 2

• As one of its last research projects, the 140 Foot Telescope has discovered an interstellar cloud of unprecedented size and mass which consists almost entirely of atomic hydrogen. Hydrogen in interstellar clouds quickly converts to molecular form in the presence of dust grains, so the question of how large an atomic cloud can be is important to understand basic interstellar physics. The present cloud, at longitude 28 degrees 5 in the plane, has an extent of 150 pc and a mass of 10 M0. Its core is cold and is seen in self-absorption, while the outer regions are warmer and are seen in emission. OH is seen in the core, signaling the onset of a small amount of molecular hydrogen there. It appears that the cloud is just now entering a spiral shock and has been caught in the transition between atomic and molecular phases. The peculiar nature of the OH excitation, also seen in other parts of the Milky Way, suggests that there may be about 100 other objects like this one, which could be detected if observed in HI at sufficiently high angular resolution, such as available with the Green Bank Telescope.

• The closest known black hole to Earth has been discovered with the VLA. Rapid response to reports of an optical and X-ray outburst from the variable V4641 Sgr showed relativistic expansion of radio jets. A presumed black hole binary system, V4641 Sgr showed the most dramatic X-ray intensity changes ever seen from such a system. The first VLA observations, made within 24 hours of the X-ray outburst, indicated that the jets had expanded sufficiently to show structure. The object's behavior makes it part of a new subclass of X-ray novae, and at a distance of 1600 light years, the black hole in this system is the closest to Earth yet discovered.

• The gas flow in the central regions of the barred galaxy NGC 1097 has been revealed by the VLA. Sensitive polarization observations have shown that shocked gas in the galaxy is diverted by nearly 90 degrees to flow directly down the bar toward the nucleus. The polarization shows the magnetic field orientation, which is a tracer of the gas velocity. The results are in general agreement with computer simulations, but show that the shock front where the diversion occurs is closer to the center of the bar, not at its edge as the simulations suggest. In addition, the observed magnetic field near the center of the galaxy indicates that magnetic stress may serve as the mechanism for feeding the central black hole with the amount of material required to account for the observed activity.

• VLBA "Movie" Shows "Missing Link" Gas Cloud Near AGN Jet. A 16-month series of VLBA images of the jet of 3C120 shows the jet colliding with a gas cloud. The cloud is intermediate in distance from the AGN core between the close, broad-line clouds and the farther narrow-line clouds. The collision caused "flickering" in the radio emission at a specific location in the jet, leading to the conclusion that the jet changed direction. Further studies of the newly-discovered cloud could yield dynamical information important to understanding the regions near galactic supermassive black holes. Observing Hours im> 0bservin;iumman)2ooo

40

30

o est. o 2 20 est.

X 10

0 1988 89 90 91 92 93 94 95 96 97 98 99 2000 01 02 03 Calendar Year

140 Foot GBT £2] 12 Meter Egg VLA Q VLBA

Figure 1. This figure shows the hours for observing on each telescope during the last decade. It includes astronomical observing, testing, and calibration. The 12 Meter Telescope closed in July of 2000, and the GBT is expected to begin operations in the spring of 2001. Distribution of Scheduled Observing Time Observinfiummanjzooo h

12 Meter VLA VLBA

o o o m® 2 v, v, v. '/, ^ MMM vmYAYAV. ™ iiMiiiiiMm 1991 92 93 94 95 96 97 98 99 00 1991 92 93 94 95 96 97 98 99 00 1993 94 95 96 97 98 99 00 Calendar Year Calendar Year Calendar Year

NRAO Staff * '/// Visitors** ^gg^Testing and Calibration

Includes NRAO Research Associates Includes Students

Figure 2. These graphs show the number of hours scheduled for testing and calibration, and for observing by the NRAO staff and by visitors on each telescope system. 12 Meter Radio Telescope Summary rttfc Observing iummari) 2000

100 - - * ^ d 4 1 f A / / /* jr JL A w, A Si- 80 / i \ i I \ n T f - 60 \ h A J \ A f 1 A f \ A r ■\ A 7 \ A f \ ft r ^ h J ^ L- - - ft £ 40 t T \ V 7 _v V V 20 i V v !» 1 VI J L i V V

1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 Calendar Year

Observing Installation, Maintenance, and Calibration Equipment Failure, Weather, and Interference

Figure3. This summary for each quarter of the calendar year shows the percentage of the total time in the year (5112 hours) that 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 closed in July 2000. Very Large Array Telescope Summary IRSD Observing (ummari) 2000 6

100 __ - -

80 k* -> ^ »■*■» ^ mt "" ^ ^ -s \* "^ 00 " S^ ^ - ' ^ V ^ ^ •* ^ ^ "^ ^ c 60 - I 40 - ^ _ ~. ..^ ^ - - ^ ^ „- m s^ 20

»*», m »^ "^« .- .*. ■ «■ 1 .. i tmt. 0 •~ ,— i^' »^ j^ ii»« 1^^ ^^ ... . - . m . „ •» ■ •« m* ■ ™ mm i ■ Ml ■ Ml ■ ^1 ... mm* ■^^i ... imm* -x' m

Calendar Year

Observing Testing, Maintenance and Calibration Downtime

Figure 4. This summary for each quarter of the calendar year shows the percentage of the total time in the year (8760 hours) that 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. Very Long Baseline Array Telescope Summary two Obwvin? Jummanj 2000 7

100 - - 80 - - 60 V *> ^v c A J 1 u - s- - r V ^. r \ *s ±j r ■> w^ ^ 1 -/ - i ^ /- - V ^ - s s^ N ^ /J ^ A r s** ^ - / V ■■ • • mtm mnmx ^Ma ■■■■

Calendar Year

Observing Installation, Maintenance, and Calibration — — Equipment Failure, Weather, and Interference

Figure 5. This summary for each quarter of the calendar year shows the percentage of the total time in the year (8760 hours) that 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. It should be noted that about 15 percent of the time cannot be scheduled as it results from the time difference across the array; this is reflected as a difference in the time between the end of one program and the start of the next. Full-Time Employees ObjervinyJummanjzooo I I

350, r.....,.

1987 1988 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 Calendar Year

Research and Operations $$% VLBA Construction GBT Construction , _ , ^ U^UJJ ' and Development

Figure 6. This figure shows the total number of NRAO full-time employees at the end of each year, projected into the future. ■El Number of People Observing with NRAO Telescopes IR&> 0bjervin?)ummanj2ooo 9

1050 1000

Si £ z3

1986 1987 1988 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 Calendar Year

Figure 7. The bar chart shows for each calendar year the number of NRAO research staff and the number of NRAO research associates who used 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 came. Distribution of Scheduled Observing Programs 0bjemn?fummanj2ooo 10

In Various Research Areas, by Percent

12 Meter VLA VLBA Overall

I. SOLAR SYSTEM- 19% 6% 2% 8% Sim, Planet, Satellites, and Comets

II. STELLAR - 11% 11% 19% 13% Pulsars, X-ray Sources, Planetary Nebulae, Circumstellar Shells, Supernova Remnants, Masers, Novae, Supemovae, and Stars

IV. EXTRAGALACTIC- 23% 63% 68% 55% Normal and Active Galaxies, Radio Galaxies, Clusters, Quasars, VLBA Studies, Extragalactic Molecules, and Cosmology ■3 Distribution of Telescope Time by Percent mSb 0b!ervin¥$umman)2ooo 11

12 Meter VLA VLBA 2000 Summary

Visitors 57% 57% 40% 51% Students 9% 7% 4% 6% NRAO Staff 15% 10% 9% 11% Jansky Research Associates 1% 2% 0% 1% Test and Calibration 15% 13% 12% 13% Maintenance and Installation 3% 10% 10% 8% Holidays and Unscheduled 0% 1% 25% 10% Institutions Whose Visitors Used NRAO Telescopes in 2000 mSb Objervin? Nummary 2000 12

GBT 12 Meter VLA VLBA

1. Academia Sinica, IAA (Taiwan) X X 2. Adelaide University (Australia) X 3. Agnes Scott College (GA) X 4. Alabama, University of (AL) X 5. Amsterdam, University of - Astronomy Institute (Netherlands) X

6. Anglo Australian Observatory - UKSTU (Australia) X X 7. Applied Physics Institute (Russia) X 8. Arcetri Astrophysical Observatory (Italy) X X 9. Arizona State University (AZ) X 10. Arizona, University of - Steward, LPL, SMTO (AZ) X X

11. Armagh Observatory (Ireland) X 12. Astronomy Institute, Slovak Academy Science - Skalnate Pleso Observatory (Slovak Republic) X 13. Astronomical Society of Rowan County (NC) X 14. Astrophysical Institute, Potsdam (Germany) X 15. Astrophysique Spatiale, Institut d' - Univ. Paris (France) X

16. Australian National University (Australia) X 17. Barcelona, University of (Spain) X 18. Beijing Astronomical Observatory (China) X X 19. Beijing Normal University (China) X 20. Beloit College - Thompson Observatory (WI) X ■El Institutions Whose Visitors Used NRAO Telescopes in 2000 mSb Obwrvin? Nummary 2000 13

GBT 12 Meter VLA VLBA

21. Birmingham, University of (UK) X 22. Bochum, Ruhr-Universitat (Germany) X 23. Bologna, Istituto di Radioastronomia, CNR - Stazione VLBI di Noto (Italy) X X 24. Bologna, Universita degli Studi Di (Italy) X X 25. Bonn University (Germany) X X

26. Bordeaux, Observatoire de (France) X 27. Boston University (MA) X X 28. Brandeis University (MA) X X 29. Bristol - Cantock Close (UK) X X 30. British Columbia, University of (Canada) X X

31. Bucknell University (PA) X 32. Byurakan Astrophysical Observatory (Armenia) X 33. Cagliari, Osservatorio Astronomico di (Italy) X 34. Calgary, University of (Canada) X X 35. California, University of, Berkeley - Hat Creek (CA) X XX

36. California, University of, Davis (CA) X X 37. California, University of, Los Angeles (CA) X 38. California, University of, San Diego (CA) X X 39. California, University of, Santa Barbara (CA) X X 40. California, University of, Santa Cruz - Lick Observatory (CA) X ■51 Institutions Whose Visitors Used NRAO Telescopes in 2000 mS) 0bseMn?}ummari)2ooo ^

GBT 12 Meter VLA VLBA

41. Caltech - OVRO, Palomar, Big Bear Solar (CA) XXX 42. Calvin College (MI) X 43. Cambridge University - Cavendish, MRAO, loA (UK) XXX 44. Canada-French-Hawaii Telescope (HI) X 45. Cantabria, Institute de Fisica (Spain) X

46. Capodimonte, Osservatorio Astronomico di (Italy) X 47. Catalunya, Universitat Politecnica de (UPC) (Spain) X X 48. Catania University (Italy) X X 49. Catholic University of America (DC) X 50. Chalmers-Onsala Space Observatory (Sweden) X X

51. Chicago, University of - Yerkes Observatory (IL) X XX 52. CNRS - CEN, Saclay (France) X X 53. Colorado, University of - JILA, CASA, LASP (CO) X 54. Columbia University (NY) X X 55. Connecticut, University of (CT) X

56. Cornell University (NY) XXX 57. CSIRO - ATNF, Parkes Observatory. (Australia) XXX 58. Delaware, University of (DE) X 59. Dominion Astrophysical Observatory (Canada) X 60. Dominion Radio Astrophysical Observatory (Canada) X Institutions Whose Visitors Used NRAO Telescopes in 2000 IR&) Observing $ummari| 2000 '5

GBT 12 Meter VLA VLBA

61. Drake University (IO) X 62. Durham, University of (UK) X 63. East Tennessee State (TN) X 64. European Southern Observatory (Chile, Germany) X 65. Florida International University (FL) X

66. Florida, University of (FL) X X 67. Gemini Observatory (USA,Brazil) X 68. George Mason University (VA) X 69. Georgia, University of (GA) X 70. Gottingen University (Germany) X

71. Groningen, University of - Kapteyn Institute (Netherlands) X X 72. Guanajuato, Universidad de (Mexico) X X 73. Hamburg University (Germany) X X 74. Hartebeesthoek Radio Astronomy Observatory (South Africa) X X 75. Harvard-Smithsonian Center for Astrophysics - Harvard, SAO, Whipple (MA) X XX

76. Harvey Mudd College (CA) X 77. Haverford College (PA) X 78. Hawaii, U. of Institute for Astronomy (HI) X X 79. Haystack Observatory - NEROC (MA) X X 80. Heidelberg Observatory (Germany) X Institutions Whose Visitors Used NRAO Telescopes in 2000 Observing Jummanj 2000 16

GBT 12 Meter VLA VLBA

81. Helsinki University of Tech. - Metsahovi Radio Observatory (Finland) X X X 82. High Altitude Observatory - NCAR (CO) X 83. Hofstra University (NY) X 84. IAFE - Buenos Aires (Argentina) X 85. IEM-CSIC (Spain)

86. Illinois, University of - Vermillion River Observatory (IL) X 87. Indiana, University of (IN) X 88. Infrared Processing/Analysis Ctr (CA) X 89. Institute Space & Aeronautical Sciences Qapan) X 90. Institute for A&A, Andalucia (Spain)

91. Institute Radio Astronomic Millimetrique (France) 92. Instituto Argentino de Radioastronomia (Argentina) 93. Inter-University Centre for Astronomy & Astrophysics (India) 94. Iowa State University (LA) 95. Iowa, University of (IA)

96. IRA/CNR (Italy) 97. Jaen University (Spain) 98. Jagellonian University (Poland) 99. Jet Propulsion Laboratory - Goldstone (CA) 100. Johns Hopkins University (MD) Institutions Whose Visitors Used NRAO Telescopes in 2000 mSb Observin? Jummanj 2000 17

GBT 12 Meter VLA VLBA

101. Joint Astronomy Center (HI) X 102. Kagoshima University (Japan) X 103. Kennesaw State College (GA) X X 104. Kent, University of (UK) X 105. Kentucky, University of (KY) X X

106. Kitt Peak National Observatory (AZ) X X 107. Laboratoire d'Astrophysique de Marseille (France) X 108. Lancashire, University of Central (UK) X X 109. Lawrence Livermore National Laboratory (CA) X X 110. Lebedev Physics Institute - ASC (Russia) X X

111. Leeds, University of (UK) X 112. Leicester, University of (UK) X 113. Leiden University/Observatory - Huygens Labs (Netherlands) X XX 114. Lisbon, University of (Portugal) X X 115. Liverpool John Moores University (UK) X X

116. Lowell Observatory (AZ) X 117. Madeira University (Portugal) X 118. Manchester, University of-Jodrell Bank, NRAL (UK) XXX 119. Maria Mitchell Observatory (MA) X X 120. Marseille Provence, Observatoire de (France) X Institutions Whose Visitors Used NRAO Telescopes in 2000 0b$emn?$ummanj2ooo 18

GBT 12 Meter VLA VLBA

121. Maryland, University of - Clark Lake Observatory (MD) X X X 122. Massachusetts Institute of Technology - Lincoln Labs (MA) X X 123. Massachusetts, University of (MA) X X 124. Mexico, University of - UNAM (Mexico) X X 125. Michigan, University of (MI) X X

126. Milano, Osservatorio Astronomico di Brera, (Italy) 127. Milano, Universita di (Italy) 128. Minnesota, University of (MN) 129. Missouri, University of (MO) 130. Montreal, University of (Canada)

131. Morehead State University (KY) X 132. Moscow State U - Sternberg State Astronomical Institute (Russia) X 133. MPIA Heidelburg (Germany) X 134. MPIAP Munich (Germany) X 135. MPIfEP Garching (Germany) X

136. MPIR Bonn (Germany) X X 137. Mt. Stromlo Observatory - ANU (Australia) X X 138. NASA/Ames Research Center (MD) X 139. NASA/Goddard Space Flight Center (MD) X X 140. National Astronomy & Ionospheric Center - Arecibo Observatory (NY) X Institutions Whose Visitors Used NRAO Telescopes in 2000 mSb Ob*ervin?JummaPj200o 19

GBT 12 Meter VLA VLBA

141. National Research Council (Canada) X 142. National Astronomical Observatory of Japan (Japan) X X 143. National Center for Radio Astrophysics (India) X X 144. National Central University, loA (Taiwan) X 145. National Institute of Standards & Technology (MD)

146. National Optical Astronomy Observatory (AZ) X 147. National Radio Astronomy Observatory (VA,NM,AZ,HI) X 148. National Science Foundation (DC) X 149. National University of Ireland, Galway (Ireland) X 150. Naval Research Laboratory (DC) X x

151. New Jersey Institute of Technology (NJ) X 152. New Mexico Institute of Mining Technology (NM) X X 153. New Mexico State University (NM) X x 154. New Mexico, University of (NM) X x 155. NFRA - JIVE, Dwingeloo, Zwiggelte, Westerbork (Netherlands) X X

156. North Carolina State University (NC) X 157. Northwestern University (IL) X 158. Observatory Carnegie Institute of Washington - Santa Barbara Street, DTM (CA, DC) X X X 159. Observatory Astronomico Nacional (Spain) X X X 160. Ohio State University (OH) X X X Institutions Whose Visitors Used NRAO Telescopes in 2000 0b$emn?Jummanj2Ooo 20

GBT 12 Meter VLA VLBA

161. Ohio University (OH) X 162. Oklahoma, University of (OK) X 163. Open University-ARC, PSRI (UK) X X 164. Oregon, University of (OR) X 165. Oxford University (UK) X X

166. Padova, University of (Italy) X 167. Paris, Observatoire de (Meudon) - DEMIRM (France) X XX 168. Paris, Observatoire de (Paris) (France) XXX 169. Pennsylvania State University (PA) X 170. Pennsylvania, University of (PA) X X

171. Pittsburgh, University of (PA) X 172. Potchefstroom, University of (South Africa) X 173. Princeton University (NJ) X 174. Puerto Rico University (Puerto Rico) X 175. Purple Mountain Observatory (China) X

176. Queens University (Canada) X 177. Raman Research Institute (India) X X 178. Renaissance Technology, Inc. (NY) X X 179. Rome Astronomical Observatory (Italy) X 180. Royal Observatory - JAC, JCMT, UKIRT (UK) X X Institutions Whose Visitors Used NRAO Telescopes in 2000 Ob*emn?Jummanj20oo 21

GBT 12 Meter VLA VLBA

181. Royal Observatory of Belgium (Belgium) X 182. Santa Maria, Universidad Federal de (Brazil) X 183. Sao Paulo, University - IAG (Brazil) X X 184. Satellite Geodetic Observatory (Hungary) X 185. Seoul National University (Korea) X

186. Shanghai Observatory (China) X 187. Sheffield, University of (UK) X 188. Southampton, University of (UK) X 189. Southwest Research Institute (TX) x 190. Space Science Institute (Boulder) (CO) X

191. Space Telescope Science Institute (MD) X XX 192. St. Cloud State University (MN) X 193. St. Petersburg State University (Russia) X X 194. Stanford University (CA) X 195. State University of New York (NY) X

196. Swiss Federal Institute of Tech - ETH (Switzerland) X X 197. Sydney, University of (Australia) X X 198. Tasmania, University of (Australia) X 199. Texas, University of - McDonald Observatory, MM-wave Observatory (TX) X 200. Thuringer Landesstemawarte - Karl Schwarzschild Observatory (Germany) X Institutions Whose Visitors Used NRAO Telescopes in 2000 0b$emnfiuminari|2ooo 22

GBT 12 Meter VLA VLBA

201. Tohoku University 0apan) X 202. Tokyo, University of - Tokyo Astronomy Observatory (Japan) X 203. Torino University/Observatory (Italy) X X 204. Toronto, University of - David Dunlap Observatory, CITA (Canada) X X 205. Toulouse, Observatoire de (France) X

206. Trinity College (TX) X 207. Tufts University (MA) X 208. Turku, University of - Tuorla Observatory (Finland) X X 209. United States Naval Academy (MD) X 210. United States Naval Observatory (DC) X X

211. University College London - MLSS (UK) X 212. Urumqi Astronomical Observatory - CAS (China) X 213. Utrecht, Universiteit (Netherlands) X X 214. Valencia, University of (Spain) X X 215. Victoria, University of (Canada) X

216. Virginia, University of (VA) XXX 217. Wales, University of, Cardiff (Wales) X X 218. Washington, University of (WA) X X 219. Wellesley College (MA) X 220. Wesleyan University (CT) X ■SI Institutions Whose Visitors Used NRAO Telescopes in 2000 two Obiervin? Nummary 2000 23

GBT 12 Meter VLA VLBA

221. Western Ontario, Univ of (Canada) 222. Wisconsin, University of - Washburn Observatory (WI) 223. Yale University (CT) 224. Yonsei University - Center for Space Astrophysics (Korea) 225. York University (Canada)

NUMBER OF INSTITUTIONS 62 187 112

NUMBER OF VISITORS 120 644 304 NUMBER OF STUDENTS 12 82 45 NUMBER OF NRAO JANSKY RESEARCH ASSOCIATES 2 4 2 NUMBER OF PERMANENT STAFF 14 47 30

TOTAL OBSERVERS 148 777 381

All told, 932 visitors, including 114 students, from 225 institutions. NRAO Student Program 0bjervin?fummanj2ooo 2^

220

200 llllllll Summer Undergraduate 180 H Co-op Summer Graduate Ea Ph. D. 160

2 100

1986 1987 1988 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 Calendar Year

Figure 8. This figure shows for each calendar year the number of PhD students (salaried at NRAO and non-salaried), co-op students, and summer undergraduate and graduate students who observed or worked at the NRAO during that year. Beginning in 1987 the majority of the undergraduate summer students were funded by a separate NSF Grant for Research Experience for Undergraduates. ■51 NRAO Front-End Status - Very Long Baseline Array rrfb 0bjervin?Jummanj2ooo 25

APRIL 2001 PERSON(S) FREQUENCY SYSTEM 3db AMPLIFIER CALIBRATION SWITCHING IN TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS (MHz) TYPE VALUE SYSTEM (KELVIN) (MHz) CHARGE DUAL NOISE INJECTION UNCOOLED PRIME MERTELY 312-342 200 30 ORTHOGONAL 10 80 Hz FET FOCUS CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION UNCOOLED PRIME MERTELY 596 - 622 200 30 OR 4 ORTHOGONAL 80 Hz FET FOCUS CIRCULAR 50 PERCENT CYCLE

COOLED DUAL NOISE INJECTION 1350-1750 MERTELY FET 30 128 CASSEGRAIN ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 2150-2350 35 MERTELY FET 128 CASSEGRAIN ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE

COOLED DUAL NOISE INJECTION 4600-5100 MERTELY FET 40 128 CASSEGRAIN ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION 8000 - 8800 COOLED MERTELY FET 37 128 CASSEGRAIN ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 12000- 15400 60 128 CASSEGRAIN MERTELY FET ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE

COOLED DUAL NOISE INJECTION 21700-24100 100 MERTELY FET 128 CASSEGRAIN ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 41000-45000 120 128 CASSEGRAIN MERTELY FET ORTHOGONAL 80 Hz CIRCULAR 50 PERCENT CYCLE COOLED DUAL NOISE INJECTION 82000 - 89000 MERTELY FET 140 128 CASSEGRAIN ORTHOGONAL 50 80 Hz PT, LA, FD, KP, OV & NL CIRCULAR 50 PERCENT CYCLE NRAO Front-End Status - Very Large Array mSb Ohervin? Nummary 2000 26

APRIL 2001 SYSTEM 3db PERSON(S) FREQUENCY AMPLIFIER CALIBRATION SWITCHING TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION (MHz) TYPE VALUE SYSTEM REMARKS IN (KELVIN) (MHz) CHARGE DUAL NOISE INJECTION UNCOOLED PRIME 74 -1200 0.8 ORTHOGONAL FET FOCUS 120 9 6 Hz INSTALLED BETWEEN 001208-010313 MERTELY CIRCULAR 50 PERCENT CYCLE 3 MHz DUAL UNCOOLED PRIME NOISE INJECTION 308 - 343 150 (LIMITED BY ORTHOGONAL FET FOCUS 10 9 6 Hz MERTELY INTERFERENCE) CIRCULAR 50 PERCENT CYCLE DUAL COOLED NOISE INJECTION 1340- 1730 35 55 CASSEGRAIN ORTHOGONAL 4 FET 9.6 Hz MERTELY CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 4500 - 5000 60 55 CASSEGRAIN ORTHOGONAL 4 FET 9 6 Hz MERTELY CIRCULAR 50 PERCENT CYCLE DUAL COOLED NOISE INJECTION 8000 - 8800 35 55 CASSEGRAIN ORTHOGONAL 4 FET 9.6 Hz MERTELY CIRCULAR 50 PERCENT CYCLE DUAL COOLED NOISE INJECTION 14400- 15400 110 55 CASSEGRAIN ORTHOGONAL 7 FET 9 6 Hz MERTELY CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 130/35 55 CASSEGRAIN 35K Tsys ON ANTENNAS 1, 2. 5. 9,10, 22000 - 24000 ORTHOGONAL 10/4 9.6 Hz MERTELY FET 11,17,18,19, 20, 21, 23, 24, 25,26 & 28 CIRCULAR 50 PERCENT CYCLE EH NRAO Front-End Status - Green Bank Telescope rrfb Obwvin? Jummari) 2000 2]

APRIL 2001 PERSON(S) SYSTEM TEMP MAXIMUM CALIBRATION SWITCHING RECEIVER FREQUENCY AMPLIFIER REMARKS IN KELVIN BANDWIDTH FEED TYPE POLARIZATION VALUE SYSTEM CHARGE NAME (GHZ) TYPE (ESTIMATED) (MHz) (APPROXIMATE) ANDERSON PRIME PFI COOLED DUAL POLARIZATION ELLISON 290 • 395 MHz 70 SHORT LIN/CIRC 2/40K FREQUENCY 342 5 MHz HFET BACKFIRE ANDERSON PRIME PFI COOLED DUAL POLARIZATION ELLISON 385 - 520 MHz 57 80 SHORT UN/CIRC 2M0K FREQUENCY 450 MHz HFET BACKFIRE ANDERSON PRIME PFI COOLED DUAL POLARIZATION ELLISON 510-690 MHz 48 80 SHORT LIN/CIRC 2/40K FREQUENCY 600 MHz HFET BACKFIRE ANDERSON PFI COOLED PRIME DUAL POLARIZATION ELLISON 680 - 920 MHz 25 240 LIN/CIRC 2/40K FREQUENCY 800 MHz HFET CONICAL ANDERSON COOLED PRIME UNDER CONSTRUCTION ELLISON PF2 0.910-1.23 240 UN/CIRC 2M0K FREQUENCY HFET CONICAL STENNES COOLED DUAL POLARIZATION DUNBRACK L-BAND 1.15-1 73 18 580 GREGORIAN LIN/CIRC 2/20K FREQUENCY HFET STENNES COOLED DUAL POLARIZATION DUNBRACK S-BAND 1.73-2.60 20 870 GREGORIAN LIN/CIRC 2/20K FREQUENCY HFET NORROD COOLED DUAL POLARIZATION SIMON C-BAND 3.95 - 5 85 25 2000 GREGORIAN LIN/CIRC 3/30K FREQUENCY HFET STENNES COOLED DUAL POLARIZATION X-BAND 8-10.1 25 2100 GREGORIAN CIRC 2.5/25K FREQUENCY DUNBRACK HFET STENNES FREQUENCY, 2 BEAMS, SEPARATED BY 5 AMIN COOLED DUNBRACK Ku-BAND 12-15.4 30 3500 GREGORIAN CIRC 3/30K DUAL POLARIZATION HFET BEAM STENNES 2 BEAMS. SEPARATED BY 4 AMIN COOLED FREQUENCY, DUNBRACK K-BAND 18-26 5 40 4000 GREGORIAN CIRC 4/40K DUAL POLARIZATION HFET BEAM 4 BEAMS ON 1 AMIN SQUARE, NORROD COOLED FREQUENCY, Q-BAND 40-52 50 4000 GREGORIAN CIRC 5K DUAL POLARIZATION WATTS HFET BEAM NRAO Front-End Status -12 Meter Telescope

0bjemn?Jummanj2ooo 28

APRIL 2001 RECEIVER CONTINUUM 3db PERSON(S) FREQUENCY AMPLIFIER CALIBRATION SWITCHING TEMPERATURE SENSITIVITY BANDWIDTH FEED TYPE POLARIZATION REMARKS IN (GHz) TYPE VALUE SYSTEM (KELVIN) (JANSKYv^SEC) (MHz) CHARGE

60-100 COOLED HORN-LENS DUAL NUTATING SIS MIXER 1.0 600 6K SINGLE - SIDEBAND MIXERS PERFETTO 65-118 SSB + OFFSET PARABOLA LINEAR SUBREFLECTOR DUAL 30 NOT NUTATING UNDER CONSTRUCTION 70-115 SIS MIXER 600 8 CHANNEL POLARIZATION 6K SHILLUE DSB MEASURED SUBREFLECTOR COMPLETED DECEMBER 97 4 BEAMS

100-180 NOT COOLED HORN-LENS DUAL NUTATING 130-170 SIS MIXER 600 — SINGLE - SIDEBAND MIXERS PERFETTO SSB MEASURED + OFFSET PARABOLA LINEAR SUBREFLECTOR

150-400 NOT DUAL NUTATING SINGLE - SIDEBAND FILTER 200-300 SIS MIXER 600 COOLED HORN-LENS — PERFETTO SSB MEASURED LINEAR SUBREFLECTOR IMAGE TERMINATED IN COLD LOAD NRAO - Staff and Visitor Publications 2000 Observing tammarfi 2000 29

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