Observing Nummary
2001,
■SI Scientific Highlights mSb Obtervin? Jummary zoo/j
Detection of HCN in a z=2.3 Galaxy - Hydrogen cyanide (HCN) emission has been detected in the z=2.2857 source IRAS F10214+4724 using the GBT. This is only the second detection of HCN in a high redshift galaxy. HCN is a signpost of star formation, and F10214 clearly contains a starburst that contributes, together with its embedded quasar, to its overall infrared luminosity. The peak emission of the detected spectral line is about 0.45 mjy with a noise level of -0.090 mjy. A new technique for removing spectral baselines in the search for weak, broad emission lines was utilized for this project.
New Interstellar Molecules detected with the GBT - The GBT has been used to detect two new interstellar molecules, propenal (CH2CHCHO) and propanal (CH3CH2CHO). These are the first new molecules detected with the GBT. These molecules were detected in the star-forming region Sagittarius B2 (N). The GBT was also used to observe the previously reported molecule propynal (HC2CHO). These molecules differ only in the number of hydrogen atoms present. The presence of these three molecular species in Sgr B2 (N) suggests that simple hydrogen addition on interstellar grains may account for their formation. The Sgr B2 (N) cloud appears to have ample energy sources to allow such grain reactions to proceed. This result suggests that successive hydrogen addition may be an important formation pathway for complex, interstellar molecules.
Neutral Hydrogen Emission of the Spitzer Extragalactic First-Look Survey Field - The GBT has been used to image the 21 cm Galactic HI emission over a 3° x 3° square centered on the Spitzer Extragalactic First-Look Survey field. The effective angular resolution was 9.8' and the velocity resolution was 0.62 km s1. The Galactic HI in this region was found to have a very interesting structure. There is a high-velocity cloud, several intermediate-velocity clouds, and narrow-line low velocity filaments. The HI emission shows a strong and detailed correlation with dust. Except for the high-velocity cloud, all features in the Nm map have counterparts in an E(B - V) map derived from infrared data. Relatively high E(B - V)/Nm ratios in some directions suggest the presence of molecular gas. The best diagnostic of such regions was found to be peak HI line brightness temperature, not the total NHI: directions where Tb > 12 K have E(B - V)/NHI significantly above the average value. The data corrected for stray radiation have been released via the web. Scientific Highlights im> Obtervin? Nummary zoo/,
NVSS Provides Support for Dark Energy Model - The "dark energy" presumably responsible for the acceleration of the expansion of the Universe also is believed to affect the evolution of fluctuations in the density of matter. Researchers using the NRAO VLA Sky Survey data, along with all-sky X-ray maps, have found a correlation between large-scale structure in the Universe and fluctuations in the Cosmic Microwave Background as mapped with the WMAP satellite. This correlation is consistent with the predictions of the dark-energy model, and thus provides an important independent confirmation of that model.
VLA Helps Confirm New Class of Gamma Ray Burst - Multiple flux measurements and radio light curves made with the VLA were an essential element leading to the conclusion that Gamma Ray Burst (GRB) 031203 was an intrinsically sub- energetic event compared to "classic" GRBs. Multi-wavelength studies of the afterglow suggest that GRB 031203 is an analog to GRB 980425, which was associated with supernova 1998bw. This discovery implies the existence of a new class of low- energy GRBs, most of which remain below current detection limits.
Multiple Pulsar Detections in the Globular Cluster Terzan 5 - A single six-hour observation in July 2004 using the GBT at 2 GHz resulted in the discovery of 14 new pulsars in the rich globular cluster Terzan 5. Follow-up observations in October resulted in the discovery of at least three additional pulsars. Terzan 5, which is located near the Galactic Center, has long been suspected of harboring many millisecond pulsars (MSPs) because of its large predicted stellar interaction rate and the steep- spectrum radio emission observed in its core. However, earlier pulsar searches using the Parkes radio telescope only uncovered three pulsars. These new GBT discoveries confirm that Terzan 5 is one of the largest producers of MSPs among the Galactic globular clusters and imply that the 20+ known pulsars are but the tip of the iceberg. At least nine of the new pulsars are members of binaries. Among these new pulsars there are also two or more eclipsing systems, the third- and fourth-fastest known rotators, a rare long-orbital-period binary, and two highly eccentric systems. Timing of the eccentric binaries over the next year will provide their total masses and may (after several years) allow separation of the pulsar and companion masses. Timing observations of the ensemble of pulsars will probe stellar and binary evolutionary scenarios, the mass-to-light ratio of the cluster core (and provide evidence for or against a black hole residing there), and other aspects of globular-cluster dynamics. Scientific Highlights rnfc Ob$ervinv Nummary 200^
VLA Shows Young Galaxy with Black Hole, Almost No Stellar Bulge - VLA observations of 1148+5351, the most distant quasar yet found, at z=6.4, show that the mass of molecular gas plus the mass of the presumed supermassive black hole at the core of the AGN account for nearly the total mass of the system. This leaves little mass available for a central galactic bulge, and much less mass than standard black hole-bulge relationships predict for such a bulge. This single example from the early Universe of a young galaxy with a supermassive black hole but no significant bulge may serve as an important clue to the long-standing question of whether the black hole or the bulge formed first, or coevally as some current popular models suggest.
Cores of Extragalactic Radio Sources Shown to Contain Microarcsecond Structures - Morphologies of compact extragalactic radio sources imaged with the VLBA have been compared to their scintillation properties. The short time-scale scintillation of compact sources is thought to be caused by the interstellar medium in our own galaxy, and reveals the presence of radio- emitting structures that are only a few micro-arcseconds in size. Statistical studies show that the VLBA images of scintillating radio sources are significantly more core-dominated than images of a comparison sample of non-scintillating sources. This demonstrates conclusively that the micro-arcsecond component is directly associated with the core of the radio source, and hence with the actual nucleus of the host galaxy. At the typical large distances of the radio sources, this radio component is no more than a few thousand astronomical units in size, probably only a few hundred times the gravitational radii of the central massive black holes.
Cold Sugar Molecules near the Galactic Center - Investigators have used the GBT to detect a very cold interstellar cloud containing the simple sugar molecule glycolaldehyde (CH20HCHO) in the Sgr B2 region. Four high signal-to-noise transitions were detected between 13 and 22 GHz. The data included both emission and absorption features. An analysis of the data indicated that the cloud is at a temperature of only ~8 K. These data, together with other information on the region, suggest that the sugar molecules were formed on the surface of grains, then released into the gas phase through disruption of the grain mantles by passing shock waves. The observed molecules now exist in the cold post-shock region. The GBT proved very powerful in these observations owing to its frequency agility, wide spectral bandwidths, and small beam which coupled very efficiently to background continuum sources allowing the detection of the absorption lines. Scientific Highlights NW Ob jemn ? Jummary zoo^t
Moving Microquasar Linked to Natal Star Cluster - Using data from numerous observations with the VLBA and other telescopes, researchers have measured the proper motion of a microquasar and concluded that it was propelled out of a nearby star cluster by an asymmetric supernova explosion about a million years ago. The microquasar LSI +61 303 is moving away from a star cluster named IC 1805 at more than 25 kilometers per second, and the companion to the compact object in the microquasar shares the spectral characteristics of the cluster population. This is the first time that a binary pair has been traced to a specific natal star cluster. The microquasar, containing a compact object of about 2 solar masses and a companion of 14 solar masses, is about 130 light-years distant from the cluster.
Global VLBI Reveals Youngest Stellar Corpse - Ongoing studies of Supernova 1986J in NGC 891 have discovered a bright, compact radio component at the center of the expanding shell. This bright component has only recently become visible. New observations made using the VLBA, the GBT, the VLA and the EVN, indicate that the central component has an inverted radio spectrum different from the shell. The new component likely is either the result of accretion onto a black hole or a pulsar wind nebula. This result provides evidence for the first association of a compact object with a modem, observed supernova and makes the black hole or neutron star by far the youngest known. Observing Hours Observing iummanj 200^
2 20
1990 91 92 93 94 95 96 97 98 99 2000 01 02 03 04 05 06 Calendar Year
240 Foot GBT □ 12 Meter VLA H VLBA
Figure 1. This figure shows the hours for observing on each telescope during the last 14 years. It includes astronomical observing, testing, calibration, and commissioning. Distribution of Scheduled Observing Time Observin? Nummary zoo/,
GBT VLA VLBA
o 6 r i o T—I 11! cfl 4 m\ m o
2001 02 03 04 1995 96 97 98 99 00 01 02 03 04 1995 96 97 98 99 00 01 02 03 04 Calendar Year Calendar Year Calendar Year
NRAO Staff Visitors Testing and Calibration
Includes 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. Green Bank Telescope Summary ifffe Obtervin? Nummary zoo^
100 - 80 ^s - /" v*. / ■^ A ■g 60 > Ar u - O ^ \ / i /" l 40 1 < V \ - V A V / n 20 / / /N - *y /" ^ -- /■ / -/
Calendar Year
Observing Testing, Maintenance & Calibration Lost Time
Figure 3. This summary for each quarter of the calendar year shows the percentage of the total time in the year that the telescope was scheduled for observing; for commissioning, maintenance, and calibration; and the percentage of astronomical observing time lost due to equipment failure, bad weather, and radio interference. Very Large Array Telescope Summary Obtervin? Jummanj zooi,
J-UU - - 80 ^™ *N ^ ^* «*s ^ _X ■> S- n S^ ^ ■■■ "* ^ ■■"■ ^ ^ "^ ^ ^ ^ ^ "■* ^ c 60 0) u i-t - - p* 40 > ^ ^^ ^ ^ -v ^^■^^■^^ ' o^xr ^^^ | ^^^»^^ ■v 20 i - "^ ■ i —
^ ■_« ^ —- — «<* 1 «. — "—I —■ 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 Calendar Year
Observing Testing, Maintenance & Calibration Lost Time
Figure 4. This summary for each quarter of the calendar year shows the percentage of the total time in the year that the telescope was scheduled for observing; for routine system testing, maintenance, and calibration; and the percentage of astronomical observing time lost due to equipment failure, bad weather, and radio interference. Very Long Baseline Array Telescope Summary rritb Obtervin? Jummanj zoo/,
1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 Calendar Year
Observing Testing, Maintenance & Calibration Lost Time
Figure 5. This summary for each quarter of the calendar year shows the percentage of the total time in the year that the telescope was scheduled for observing; for routine calibration, maintenance, and installation of new experiments; and the percentage of astronomical observing time lost due to equipment failure, bad weather, and radio interference. It should be noted that about ten 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 Obfervin? Nummary zoo/,
est.—est. ■ i i i
1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 Calendar Year Research and VLBA GBT 1 ALMA EVLA Operations Construction Construction
Figure 6. This figure shows the total number of NRAO full-time employees at the end of each year, projected into the future. Number of People Observing with NRAO Telescopes irib Observin? Jummanj 200^ 11
S 700 6
1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 Calendar Year
Figure 7. The bar chart shows for each calendar year the number of NRAO research staff and the number of 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 IRK> Obiervin ? Jummanj zoo/j 12
In Various Research Areas, by Percent
GBT VLA VLBA Overall I. SOLAR SYSTEM- 4% 5% 1% 3% Sun, Planet, Satellites, and Comets II. STELLAR- 13% 19% 15% 16% Pulsars, X-ray Sources, Planetary Nebulae, Circumstellar Shells, Supernova Remnants, Masers, Novae, Supemovae, and Stars III. GALACTIC - 43% 19% 7% 23% Galactic Structure, Center, Molecular Clouds, HII Regions, Star Formation, Molecules, and Interstellar Medium IV. EXTRAGALACTIC - 40% 57% 77% 58% Normal and Active Galaxies, Radio Galaxies, Clusters, Quasars, VLBA Studies, Extragalactic Distribution of Telescope Time by Percent two Ob jemn ? Jummanj zoo/j 13
GBT VLA VLBA 2004 Summary
Visitors (U.S.) 26% 28% 20% 25% Visitors (Foreign) 15% 27% 30% 24%
Students 5% 5% 5% 5% NRAO Staff 13% 11% 7% 10%
Research Associates at NRAO 1% 3% 1% 2% Test and Calibration 23% 12% 13% 16%
Maintenance and Installation 17% 12% 12% 14% Institutions Whose Visitors Used NRAO Telescopes in 2004 IRE> Obtervin? Jummanj ZOOI, Vi
Institution GBT VLA VLBA 1. Agnes Scott College (GA) X X X 2. Alabama, University of (GA) X X 3. American Astronomical Association (DC) X X X 4. Amsterdam, University of (Netherlands) X X 5. Andalucia, Instituto de Astrofisica de (Spain) X X X
6. Anglo Australian Observatory (Australia) X 7. Arizona State University (AZ) X 8. Astrofisica, Optica y Electronica, Institue National de (Mexico) X X 9. Astronomy and Astrophysics, Insitute of, Academia Sinica (Taiwan) X X X 10. Astronomy and Space Physics, Insitituto de (Argentina) X
11. Astrophysical Institute Potsdam (Germany) X 12. Astrophysique de Paris, Institute d' (France) X 13. Astute Networks (CA) X 14. Australian National University (Australia) X X 15. Australian Telescope National Facility (Australia) X X X
16. Barcelona, University of (Spain) X 17. Beijing Astronomical Observatory (China) X 18. Beijing Normal University (China) X 19. Birmingham University (United Kingdom) 20. Boise State University (ID) X Institutions Whose Visitors Used NRAO Telescopes in 2004 rrib Obiemn? Jummanj zooit 15
Institution GBT VLA VLBA 21. Bologna, Osservatorio Astonomico di (Italy) X 22. Bologna, University of (Italy) X 23. Bonn University (Germany) X X X 24. Bordeaux University (France) X X 25. Boston University (MA) X X
26. Brandeis University (MA) X X 27. Brera, Osservatorio Astronomico di (Italy) X 28. British Columbia, University of (Canada) X X 29. Bucknell University (PA) X X 30. Bulgarian Institute of Science (Bulgaria) X
31. Byurakan Astrophysical Observatory (Armenia) 32. CSIRO (Australia) X 33. Cagliari, Osservatorio Astronomica di (Italy) X X X 34. California Institute of Technology (CA) X X X 35. California at Berkeley, University of (CA) X X X
36. California at Davis, University of (CA) X X 37. California at Los Angeles, University of (CA) X X X 38. California at Riverside, University of (CA) X 39. California at San Diego, University of (CA) X X 40. California at Santa Barbara, University of (CA) Institutions Whose Visitors Used NRAO Telescopes in 2004 Observin? Jummanj 200^ 16
Institution GBT VLA VLBA 41. California at Santa Cruz, University of (CA) X X X 42. Cambridge, University of (United Kingdom) 43. Canadian Institute of Theoretical Astrophysics (Canada) 44. Canarias, Instituto de Astrofisica de (Spain) 45. Cardiff University (United Kingdom) X
46. Carnegie Institute of Washington (DC) X 47. Carter Observatory (New Zealand) X 48. Catania, Universita delgi Studi di (Italy) X 49. Center for Astrophysics (MA) X 50. Central Lancashire, University of (United Kingdom)
51. Centre National de la Recherches Scientifique (France) X 52. Chalmers University of Technology (Sweden) X X 53. Chicago, University of (IL) X X 54. Chinese Academy of Sciences (China) X 55. Colgate University (NY) X
56. Cologne, University of (Germany) 57. Columbia University (NY) X X 58. CombinatoRx (MA) X X 59. Commissariat a L'Energie Atomique (France) X 60. Consejo Superior de Investigaiones Cientificas (Spain) X Institutions Whose Visitors Used NRAO Telescopes in 2004 two Obtervin? Nummary zoo/, 17
Institution GBT VLA VLBA 61. Copernicus University (Poland) X X 62. Cork Institute of Technology (Ireland) X X 63. Cork, University College of (Ireland) X 64. Cornell University (NY) X X X 65. Cote d'Azur, Observatoire de la (France) X X
66. Crimean Astrophysical Observatory (Ukraine) X 67. Delaware, University of (DE) X 68. Denison University (OH) X X 69. Dominion Radio Astrophysical Observatory (Canada) X 70. Edinburgh, University of (United Kingdom) X X
71. European Southern Observatory (Germany) X X 72. European Space Agency - ESOC (Germany) X 73. European Space Agency - ESTEC (Netherlands) X 74. European Space Agency - Headquarters (France) X 75. Fayetteville State University (NC) X
76. Fermi National Accelerator Lab (IL) X X 77. Firenzi, Universita degli Studi Di (Italy) X X 78. Foundation for Fundamental Research on Matter (Netherlands) X 79. Geodetic Observatory (Hungary) X 80. Geografica Nacional, Insituto (Spain) X Institutions Whose Visitors Used NRAO Telescopes in 2004 NUD Obiervin? Jummanj zooi, 18
Institution GBT VLA VLBA 81. Georgia State University (GA) X 82. Gifu University (Japan) X 83. Granada, Universidad de (Spain) X X X 84. Grenoble, Laboratoire d'Astrophysique de (France) X 85. Guadalajara, Universidad de (Mexico) X
86. Hamburg University (Germany) X 87. Hartesbeesthoek Radio Astronomy Observatory (South Africa) X 88. Harvard University (MA) X 89. Haverford College (PA) 90. Hawaii at Manoa, University of (HI) X
91. Haystack Observatory - NEROC (MA) X X 92. Heidelberg University (Germany) X 93. Helsinki University (Finland) X 94. Helsinki University of Technology (Finland) 95. IBM T.J. Watson Research Center (NY) X
96. Ibaraki University (Japan) X 97. Illinois, University of (IL) X 98. Imperial College of Science, Technology and Medicine (United Kingdom) X 99. Indian Institute of Astrophysics (India) X 100. Innsbruck, Universitat (Austria) X Institutions Whose Visitors Used NRAO Telescopes in 2004 two Obtervin? Jummary 2001^ 19
Institution GBT VLA VLBA 101. Institute of Astronomy, ETH Zurich (Switzerland) X 102. Institute of Physics, Polish Academy of Science (Poland) X 103. Institute of Radio Astronomy (Italy) X X X 104. Institute of Radio Astronomy, Cagliari (Italy) X X X 105. Integral Science Data Center (Switzerland) X
106. International School for Advanced Studies (Italy) X X 107. Iowa, University of (IA) X X 108. Israel Institute of Technology (Israel) X 109. Issac Newton Group of Telescopes (Spain) X 110. Jaen, Universidad de (Spain) X
111. Jagellonian University (Poland) X 112. James Clerk Maxwell Telescope (HI) X X 113. Jena, Friedrich-Schiller-Universitat (Germany) X 114. Jet Propulsion Laboratory (CA) X X 115. Johns Hopkins University (MD) X
116. Joint Institute for VLBI in Europe (Netherlands) X X X 117. Kapteyn Astronomical Institute (Netherlands) X X X 118. Katholieke Universiteit (Netherlands) X 119. Keele University (United Kingdom) X 120. Kent, University of (United Kingdom) X Institutions Whose Visitors Used NRAO Telescopes in 2004 IRS> Obiervin? Jummanj ZOOI, 20
Institution GBT VLA VLBA 121. Kentucky, University of (KY) X 122. Korea Astronomical Observatory (Korea) X 123. Kyoto University Qapan) X 124. Laval University (Canada) X 125. Lawrence Livermore National Laboratory (CA) X
126. Lebedev Physical Institute (Russia) X 127. Leicester, University of (United Kingdom) X 128. Lisbola, Universidade de (Portugal) X X 129. Liverpool John Moores University (United Kingdom) X X 130. Los Alamos National Laboratory (NM) X X X
131. Lowell Observatory (AZ) 132. Lycoming College (PA) X 133. Madrid, Universidad Autonoma de (Spain) X 134. Manchester, University of (UK) X X 135. Marseille, Observatoire de (France) X
136. Maryland, University of (MD) X X X 137. Massachusetts Institute of Technology (MA) X X 138. Massachusetts, University of (MA) X X X 139. Max-Planck Institut fur extraterrestrische Physik (Germany) X 140. Max-Planck Institute for Radioastronomy (Germany) X X Institutions Whose Visitors Used NRAO Telescopes in 2004 IRS> Obtervin? Jummarij zoo/, 21
Institution GBT VLA VLBA 141. Max-Planck-Institut fur Astronomy (Germany) X X X 142. Melbourne, University of (Australia) X 143. Michigan, University of (MI) X X 144. Midi-Pyrenes, Observatoire de (France) X 145. Milano, Universita degli Studi di (Italy) X X
146. Minnesota, University of (MN) X X 147. Missouri, University of (MO) 148. Monash University (Australia) 149. Moscow State University (Russia) 150. Mount Tarana Observatory (Australia)
151. Mullard Space Science Laboratory (United Kingdom) X X 152. NFRA (Netherlands) X X 153. Nagoya University (Japan) X X 154. Nanjing University (China) X X X 155. National Astronomy & Ionospheric Center (NY) X X X
156. National Aeronautics and Space Administration (USA) X X 157. National Astronomical Observatories (China) X 158. National Astronomical Observatory of Japan (Japan) X X X 159. National Institute of Standards and Technology (MD) X 160. National Optical Astronomy Observatory (AZ) X Institutions Whose Visitors Used NRAO Telescopes in 2004 iwb Obtervin? Jummanj 2001, 22
Institution GBT VLA VLBA 161. National Radio Astronomy Observatory (NM, VA, WV, AZ) X X X 162. National Research Council of Canada (Canada) X X X 163. National Science Foundation (DC) X X X 164. National Taiwan University (Taiwan) X X 165. National University of Ireland (Ireland) X
166. Naval Research Laboratory (DC) X X X 167. New Mexico Institute of Mining Technology (NM) X X X 168. New Mexico, University of (NM) X 169. North Carolina School of Science and Mathematics (NC) X 170. North Carolina, U. of (NC) X
171. Northwestern University (IL) 172. Oberlin College (OH) 173. Ohio State University (OH) X 174. Ohio University (OH) X 175. Oklahoma, University of (OK) X
176. Oxford, University of (United Kingdom) X X 177. Pado, Universita degli Studi di (Italy) X 178. Paris, Observatoire de (France) X X X 179. Paris-Meudon Observatory (France) X 180. Pa via, Universita degli Studi di (Italy) X Institutions Whose Visitors Used NRAO Telescopes in 2004 gjg Obtervin? Jummanj 2001, 23
Institution GBT VLA VLBA 181. Penn State University (PA) X 182. Pennsylvania, University of (PA) X X 183. Peter Scherrer Institut (Switzerland) X 184. Princeton University (NJ) X X 185. Purdue University (IN) X
186. Queens University (Canada) X 187. Queens University (United Kingdom) X 188. Queensland, University of (Australia) X 189 Radio Astronomique Millmetrique, Institut de (France) X X 190. Raman Institute (India) X X
191. Renaissance Technologies (NY) X 192. Rice University (TX) X 193. Rio Grande do Sul, Universidad Federal do (Brazil) X 194. Roane State Community College (TN) X 195. Royal Military College (Canada) X
196. Ruhr-Universitat, Bochum (Germany) X 197. Santa Catarina, Universidade Federale de (Brazil) X 198. Sao Paulo, Universidade de (Brazil) 199. Science and Technology of China, University of (China) X 200. Shanghi Observatory (China) X X Institutions Whose Visitors Used NRAO Telescopes in 2004 trio Obtervin? Jummanj 2001, ih
Institution GBT VLA VLBA 201. Sheffield, University of (United Kingdom) X 202. Smith College - FCRAO (MA) X 203. Smithsonian Institution (DC) X X X 204. Southampton, University of (United Kingdom) X X 205. Space Telescope Science Institute (MD) X X
206. Space and Astronautical Science, Institute of Qapan) X 207. St. Andrews, University of (United Kingdom) X 208. St. Cloud State University (MN) X 209. St. Petersburg State University (Russia) X X 210. Stanford University (CA) X X
211 State College NY (NY) X 212. Stockholm Observatory (Sweden) X 213. Sweet Briar College (VA) X 214. Swibume University (Australia) X 215. Sydney, University of (Australia) X
216. Tasmania, University of (Australia) X 217. Tata Inst Fundamen Res (India) X X X 218. Tel-Aviv University (Israel) X X 219. Texas, University of (TX) X 220. Thuringer Landesstemwarte Tautenburg (Germany) X Institutions Whose Visitors Used NRAO Telescopes in 2004 rnSb Ob jemn? Jummanj zooi, 25
Institution GBT VLA VLBA 221. Tohoku University Qapan) X 222. Torino, Osservatorio Astronomico di (Italy) X 223. Trieste, Universita degli Studi di (Italy) X 224. Trinity University (TX) X X X 225. Tsinghua University (China) X
226. Tufts University (MA) X 227. Turku University (Finland) X 228. Union College (NY) X X 229. United States Naval Observatory (DC) X X 230. Univer. Nadonal Autonoma de Mexico (Mexico) X X
231. Universita di Padova (Italy) X X 232. University College of London (United Kingdom) X 233. University of Arizona (AZ) X X X 234. University of Birmingham (United Kingdom) X 235. University of Bristol (United Kingdom) X X
236. University of Calgary (Canada) X 237. University of Colorado, Boulder (CO) X X X 238. University of Durham (United Kingdom) X 239. University of Guanajuato (Mexico) X 240. University of Jaen (Spain) Institutions Whose Visitors Used NRAO Telescopes in 2004 ffOb Obtervin? Jummanj zooi, 26
Institution GBT VLA VLBA 241. University of Leeds (United Kingdom) X X 242. University of Leiden (Netherlands) X X X 243. University of McGill (Canada) X X 244. University of New South Wales (Australia) X 245. University of Oslo (Norway) X
246. University of Redlands (CA) X 247. University of Tokyo Qapan) X X 248. University of Toronto (Canada) X X 249. University of Vienna (Austria) X 250. University of Wollongong (Australia) X
251. Uppsala University (Sweden) 252. Urumqi Astronomical Observatory (China) X 253. Valencia, Universidad de (Spain) X X X 254. Vanderbilt University (TN) X 255. Victoria, University of (Canada) X
256. Villanova University (PA) 257. Virginia Tech (VA) X 258. Virginia, University of (VA) X X X 259. Washington State University (WA) X X 260. Washington, University of (WA) X Institutions Whose Visitors Used NRAO Telescopes in 2004 ■51 Ob jervin? Jummary zoo/t 27
Institution GBT VLA VLBA 261. Weizmann Institute of Science (Israel) X 262. Whittier College (PA) X X 263. Wisconsin at Madison, University of (WI) 264. Wisconsin at Whitewater, University of (WI) X 265. Wyoming, University of (WY) X
266. Yale University (CT) X 267. York University (Canada) X X
NUMBER OF INSTITUTIONS 105 211 144
NUMBER OF VISITORS 263 647 364 NUMBER OF STUDENTS 29 63 36 NUMBER OF RESEARCH ASSOCIATES AT NRAO 4 6 3 NUMBER OF PERMANENT STAFF
TOTAL OBSERVERS 332 758 435
All told, 1074 visitors, including 104 students, from 267 institutions. NRAO Student Program Obtervin? Jummanj 200^ 28
220 ^H Summer Undergraduate 200 Hi Co-op I I Summer Graduate H P/z. D. 180
160 est. 140 1 fc 120
^ 100 I ' ■ ■ " = -
80 i 'iii
60
40
20
1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 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. NRAO Front-End Status Green Bank Telescope IBJE> Obtervin? Nummary zoo/, 29
MARCH 2005
CALIBRATION PERSON(S) SYSTEM TEMP MAXIMUM SWITCHING RECEIVER FREQUENCY AMPLIFIER REMARKS IN KELVIN BANDWIDTH FEED TYPE POLARIZATION VALUE SYSTEM NAME (GHz) TYPE CHARGE (ESTIMATED) (MHz) (APPROXIMATE) PRIME ANDERSON PFI COOLED 2/40K FREQUENCY DUAL POLARIZATION 290-395 MHz 70 80 SHORT LIN/CIRC BAUSERMAN 340 MHz HFET BACKFIRE PRIME ANDERSON PFI COOLED 2/40K FREQUENCY DUAL POLARIZATION 385 - 520 MHz 57 80 SHORT LIN/CIRC BAUSERMAN 450 MHz HFET BACKFIRE PRIME ANDERSON PFI COOLED 2/40K FREQUENCY DUAL POLARIZATION 510-690 MHz 48 80 SHORT LIN/CIRC BAUSERMAN 600 MHz HFET BACKFIRE ANDERSON PFI COOLED PRIME 2/40K FREQUENCY DUAL POLARIZATION 680 -920 MHz 25 240 LIN/CIRC BAUSERMAN 800 MHz HFET CONICAL ANDERSON COOLED PRIME 2/40K FREQUENCY DUAL POLARIZATION 0.910-1.23 22 240 LIN/CIRC BAUSERMAN PF2 HFET CONICAL ANDERSON COOLED 2/20K FREQUENCY DUAL POLARIZATION 1.15-1.73 18 580 GREGORIAN LIN/CIRC BAUSERMAN L-BAND HFET SIMON COOLED 2/20K FREQUENCY DUAL POLARIZATION 1.73-2.60 20 870 GREGORIAN LIN/CIRC GUTHRIE S-BAND HFET SIMON COOLED 3/30K FREQUENCY DUAL POLARIZATION 3.95-5.85 25 2000 GREGORIAN LIN/CIRC GUTHRIE C-BAND HFET SIMON COOLED FREQUENCY DUAL POLARIZATION 25 2100 GREGORIAN CIRC 2.5/25K GUTHRIE X-BAND 8-10.1 HFET
FREQUENCY, 2 BEAMS, SEPARATED BY 5 AMIN STENNES COOLED 3/30K 12-15.4 30 3500 GREGORIAN CIRC BEAM DUAL POLARIZATION GUTHRIE Ku-BAND HFET
FREQUENCY, 2 BEAMS. SEPARATED BY 4 AMIN STENNES COOLED 4/40K 18-26.5 40 4000 GREGORIAN CIRC DUAL POLARIZATION GUTHRIE K-BAND HFET BEAM
FREQUENCY, 2 BEAMS ON 1 AMIN SEP. NORROD/ COOLED 5K 40-52 50 4000 GREGORIAN CIRC BEAM DUAL POLARIZATION BAUSERMAN Q-BAND HFET NRAO Front-End Status Very Large Array Telescope Obtervin? Jummanj zooi, }o
MARCH 2005
SYSTEM 3db PERSON(S) FREQUENCY AMPLIFIER CALIBRATION SWITCHING TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS IN (MHz) TYPE VALUE SYSTEM (KELVIN) (MHz) CHARGE DUAL NOISE INJECTION UNCOOLED PRIME 74 -1200 0.8 ORTHOGONAL 120 9.6 Hz TYPICALLY INSTALLED DURING A-ARRAY FET FOCUS MERTELY CIRCULAR 50 PERCENT CYCLE 3 MHz DUAL NOISE INJECTION UNCOOLED PRIME 308 - 343 150 (LIMITED BY ORTHOGONAL 10 9.6 Hz MERTELY FET FOCUS INTERFERENCE) CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 1340-1730 35 55 CASSEGRAIN ORTHOGONAL 2 9.6 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 4500 - 5000 60 55 CASSEGRAIN ORTHOGONAL 4 9.6 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 8000 - 8800 35 55 CASSEGRAIN ORTHOGONAL 3 9.6 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 14400-15400 140 55 CASSEGRAIN ORTHOGONAL 7 9.6 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION 20500 - 25000 COOLED 50 55 CASSEGRAIN ORTHOGONAL 2 9.6 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE NRAO Front-End Status Very Long Baseline Array Telescope tnb Obtervin? Nummary zooi, }i
MARCH 2005
SYSTEM 3db PERSON(S) FREQUENCY AMPLIFIER CALIBRATION SWITCHING TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS IN (MHz) TYPE VALUE SYSTEM (KELVIN) (MHz) CHARGE DUAL NOISE INJECTION UNCOOLED 312 - 342 200 30 PRIME ORTHOGONAL 10 80 Hz MERTELY FET FOCUS CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION UNCOOLED PRIME 596-622 200 30 OR 4 ORTHOGONAL 5 80 Hz MERTELY FET FOCUS CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 1350-1750 30 128 CASSEGRAIN ORTHOGONAL 2 80 Hz MERTELY hbl CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 2150-2350 35 128 CASSEGRAIN ORTHOGONAL 2 80 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 4600-5100 40 128 CASSEGRAIN ORTHOGONAL 2 80 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 8000 - 8800 37 128 CASSEGRAIN ORTHOGONAL 3 80 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION 12000-15400 COOLED 60 128 CASSEGRAIN ORTHOGONAL 4 80 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 21700-24100 100 128 CASSEGRAIN ORTHOGONAL 5 80 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 41000-45000 120 128 CASSEGRAIN ORTHOGONAL 8 80 Hz MERTELY FET CIRCULAR 50 PERCENT CYCLE NRAO - Staff and Visitor Publications rrib Obtervin; Nummary zoo/, 32
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