National Rcufio ** Astronomy Observing iumman) Observatory 2002

NATIONAL RADIO ASTRONOMY OBSERVATORY

Observing Jummanj 2002 5tatiitio

April 2003 (Revised 05/01/03)

Scientific Highlights m Observing 5ummarij 2002 i

• THE DEFLECTION OF RADIO WAVES CAUSED BY A MOVING OBJECT-On September 8,2002, when Jupiter passed within 3.7' of a strong quasar, astronomers used the VLBA and Effelsberg to measure the deflection of the quasar produced by the gravitational field of Jupiter. By alternating observations of the quasar with two other nearby calibrators, the position of the quasar on September 8, compared with that on four other days, was measured to an accuracy less than 10 microarcsec. This accuracy is a factor of three better than previous VLBI observations, and much more accurate than any other astrometric method. By using a similar technique, the determination of the parallax of objects more than 10 kpc distant, the tracking of spacecraft to an accuracy of 30 meters near Jupiter, and the measurement of the proper motion of objects in M31 to 5 km/sec over 10 years, can be obtained. The measurement confirmed that the deflection of the quasar is associated with the retarded position of Jupiter, and the result is in agreement with the prediction of General Relativity (GR). There is lively discussion among physicists about which parameters(s) of GR are measured by this experiment: the speed of gravity, the speed of light, or the post-parameterized Newtonian parameter Ot,. The interpretation depends on how GR is generalized in order to incorporate a speed of gravity which is not equal to the speed of light. However this experiment, as well as those associated with the binary pulsar and lunar laser ranging, are consistent with the speed of gravity equal to the speed of light.

• DISCRETE HI CLOUDS IN THE GALACTIC HALO-GBT observations of the Galactic HI halo in the inner Galaxy show that in many directions the halo consists of previously unresolved clouds, some of which are more than 2 kpc from the Galactic plane, corotating with the disk below. These clouds provide evidence that supernova- powered "galactic fountains" continually blast superheated gas into the halo. In previous, lower-resolution 21 cm observations the cloud ensemble appeared nearly continuous, suggesting incorrectly that the HI halo was diffuse. It now appears that much if not all of the HI halo is concentrated into clouds with sizes of a few tens of parsecs, and masses of 50 to 100 solar masses. The clouds were discovered about 5 kpc from the Earth toward the galactic center.

• THE NATURE OF THE FAINTEST GALAXIES - Surveys of the faintest radio objects using the VLA and optical images from HST, Keck and Subaru show that most of these objects are galaxies with redshifts greater than one. The nature of their emission is important in determining the evolution and interaction of galaxies at early cosmological epochs. Two processes are believed important to their radiative properties: massive star formation, and active galactic nuclei. One of the best discriminators between these processes is the angular size of the emission regions: if less than -0.1 arcsec (-50 pc at z=l), then their radiative temperature exceeds 106 degrees and the emission cannot be produced by star formation. In March 2002, the VLBA+GBT+Effelsberg imaged at 1.4 GHz a 6'x6' region in the field SA13 with 0.02" resolution. Within this region, -100 objects above 50 ujy had already been detected with the VLA, and optical images down to 26-mag identified > 90% of the objects. The combination of radio telescopes achieved an rms image noise of 7 ujy. Analysis of the images suggests that less than 10% of the radio sources contain emission within 0.04 arcsec components—the size expected for AGN activity. Thus, the early evolution of galaxies appears to be driven mostly by starburst phenomena rather than the AGN phenomenon. Scientific Highlights Nub Observin? Jummanj 2002

NVSS SHOWS EFFECT OF GALAXY'S MOTION THROUGH THE UNIVERSE - The standard cosmological model has passed another test, performed using data from the NRAO VLA Sky Survey (NVSS). The dipole temperature anisotropy in the cosmic microwave background (CMB) has indicated the Milky Way is moving at about 370 km/s relative to the "rest frame" of the universe. If the standard model is correct, a similar dipole should be seen as an enhancement in the surface density of distant galaxies in the direction of motion. Using the NVSS data, investigators found just such an enhancement, in the same direction as the CMB's temperature dipole. Detecting this enhancement, at about the 1% level, required first subtracting nearby radio sources from the NVSS data, leaving only sources presumed to be at cosmological distances.

VLBA MEASURES NINE NEW PULSAR PARALLAXES-The VLBA has been used to measure nine new pulsar parallaxes, doubling the number of pulsars with accurate (errors of only 2%) distance measurements. Such results allow determination of the absolute luminosities and radiation efficiencies of pulsars, and, for thermally emitting neutron stars, promise the possibility of directly constraining the neutron star radius and thus the nuclear equation of state at high densities. Combined with measurements of proper motion, also completed in this study, this work helps constrain the pulsar velocity distribution and hence the symmetry of supernova explosions.

WATER MASERS ABOUT ACTIVE GALACTIC NUCLEI -22 GHz water masers have been observed toward the nuclei of 16 known sources in AGNs. These are the most sensitive data of this kind obtained to date. The high-quality GBT spectra make it possible to distinguish some features for the first time. By tracking the velocities of these features over several epochs, it will be possible to study the dynamics of molecular gas within a parsec of the central engine. New maser features are seen in most of the recent spectra, and in two galaxies (NGC 1386, NGC 5506), a weak, broad base of HjO emission is detected under previously identified narrow components. Some spectra cover more than 10,000 km/s of velocity space, though maser features are generally seen within a few hundred km/s of the systemic velocity of the host galaxy. This project marks the initial scientific application of the active surface of the GBT, and the wide-band (200 and 800 MHz) spectrometer modes.

YOUNG STAR PROBABLY EJECTED FROM TRIPLE SYSTEM - Analysis of nearly 20 years of VLA data leads researchers to conclude that a young, low-mass star passed within about 2 AU of a more massive, close binary system in the 1995-1998 time frame, causing a dramatic change in its orbit probably leading to its ultimate gravitational escape from the system. The result supports longstanding indications from computer simulations that such ejections occur in multiple-star systems. Ejections of low-mass protostars from their parent systems, and the resultant halt to accretion, could provide one explanation for the formation of brown dwarfs. Observing Hours Ob)ervin^ummary2002 3

40

-

30 1 1 1 1—ll—1 ■ ■ Hi■i o o HH est. est. est. 3 20 x i ft*vJ ■i - ■ i 1 3 O 1 X 1 10

1990 91 92 93 94 95 96 97 98 99 2000 01 02 03 04 05 Calendar Year

140 Foot □ GBT | | 12 Meter Fl VIA VLBA

Figure 1. This figure shows the hours for observing on each telescope during the last 16 years. It includes astronomical observing, testing, calibration, and commissioning. ■31 Distribution of Scheduled Observing Time rR&> 0bservinfiumrnanj2oo2

GBT VLA VLBA n hi

2001 02 1993 94 95 96 97 98 99 00 01 02 1993 94 95 96 97 98 99 00 01 02 Calendar Year Calendar Year Calendar Year

* pflS'li'Fl ** mmmm 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 NVO Observin;Jummanj2002

100 - - 80 "S - r V. 60 / *s - \ / & 40 ■ A - N/ V- 20 / / - f* +s -/

Calendar Year

Observing Testing, Maintenance & Calibration Lost Time

FigureS. 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 commissioning, maintenance, and calibration; and the percentage of time lost due to equipment failure, bad weather, and radio interference. ■51 Very Large Array Telescope Summary two Observing iummaru 2002 6

100

80

c 60 u £ 40

20

0 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 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 (8760 hours) that the telescope was scheduled for observing; for routine system testing, maintenance, and calibration; and the percentage of time lost due to equipment failure, bad weather, and radio interference. Very Long Baseline Array Telescope Summary Observin? Jummarij 2002 7

1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 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 (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 0b5ervin^ummary2ooi 8

600 t,OL. tiDL. - 550 - 500 - 450

400 1 1 1 1 - M 350 -

| 300 - - - - - Z 250 - -

200 -

150

100

50

1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 Calendar Year Research and ,...... ,«■ VLBA i 1 GBT i ■ — ALMA EVLA Operations n 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 IRSD 0bservin?iummarij2002 9

est. 1050 Visitors and Students 1000 ^H Research Associates 950 I I NRAO Staff 900 1 Number of Institutions Bj 850 800 750 700 650 600

50 1331- mm 0 1988 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 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 rnfc Observin? Jummari) 2002 10

In Various Research Areas, by Percent

GBT VLA VLBA Overall

I. SOLAR SYSTEM- 5% 10% 0% 6% Sun, Planet, Satellites, and Comets

II. STELLAR - 22% 11% 17% 15% Pulsars, X-ray Sources, Planetary Nebulae, Circumstellar Shells, Supernova Remnants, Masers, Novae, Supemovae, and Stars

III. GALACTIC- 50% 14% 12% 19% Galactic Structure, Center, Molecular Clouds, HII Regions, Star Formation, Molecules, and Interstellar Medium

IV. EXTRAGALACTIC - 23% 65% 71% 60% Normal and Active Galaxies, Radio Galaxies, Clusters, Quasars, VLBA Studies, Extragalactic Molecules, and Cosmology Distribution of Telescope Time by Percent two Observing (ummary 2002 11

GBT VLA VLBA 2002 Summary

Visitors (U.S.) 9% 43% 25% 26% Visitors (Foreign) 7% 20% 21% 16% Students 1% 5% 1% 2% NRAO Staff 8% 6% 3% 6% Research Associates at NRAO 0.3% 1% 1% 0.7% Test and Calibration 45% 13% 14% 24% Maintenance and Installation 22% 11% 12% 15% Institutions Whose Visitors Used NRAO Telescopes in 2002 mib 0bservin?$ummar

VLA VLBA GB 1 Academia Sinica, IAA (Taiwan) X X 2 Adelaide University (Australia) X 3 Agnes Scott College (GA) X X X 4 Alabama at Huntsville, University of (AL) X X 5 American Astronomical Society (DC)

6 American Institute of Physics (MD) X 7 Amsterdam, University of- Astronomy Institute (Netherlands) X g Anglo-Australian Observatory (Australia) X 9 Arcetri Astrophyiscal Observatory (Italy) X X X \ o Arizona, University of (AZ) X

11 Arkansas, University of (AR) X 12 Astro Space Center (Russia) X 13 Astrofisica Andalucia, Institute de (Italy) X 14 Astrofisica, Optica Electronica, Institute Nacional de (Mexico) 15 Astronomia, Institute de, UNAM (Mexico) X X

16 Astronomical Institute, Academy of Sciences of the (Czech Republic) X 17 Astrophysikalisches Institut of Potsdam(Germany) X 1 g Australia Telescope National Facility, CSIRO (Australia) X X 19 Barcelona, University of (Spain) X 20 Beloit College (WI) X Institutions Whose Visitors Used NRAO Telescopes in 2002 mfc Observin? Jumman) 2002 13

VLA VLBA GBT 21 Bologna, Institute di Radioastronomia, CNR - Stazione VLBI di Note (Italy) X X 22 Bologna, Universitat degli Studi di (Italy) X X X 23 Bonn University (Germany) X 24 Bordeaux, Observatoire de (France) X X 25 Boston University (MA) X X

26 Brandeis University (MA) X X 27 Brera Astronomical Observatory (Italy) 28 Bristol-Cantock Close (UK) X 29 British Columbia, University of (Canada) X 30 Byurakan Astrophysical Observatory (Armenia) X

31 Cagliari, Universidad de (Italy) X 32 Calgary, University of (Canada) X X 33 California, University of, Berkeley (CA) X X X 34 California, University of, Los Angeles (CA) X 35 California, University of, San Diego (CA) X X

36 California, University of, Santa Barbara CA) X X 37 California, University of, Santa Cruz (CA) X 38 California, University of,Davis (CA) X X 39 Caltech - OVRO, Palomar, Big Bear Solar (CA) X X 40 Calvin College (MI) X Institutions Whose Visitors Used NRAO Telescopes in 2002 ffiub Observin? Nummary 2002 n VLA VLBA GBT 41 Cambridge University - Cavendish, MRAO, loA (UK) X X 42 Cantabria Jnstituto de Fisica de, (Spain) X 43 Carleton University (Canada) X 44 Carnegie Institution of Washington (DC) X 45 Catania University (Italy) X

46 Catholic University of America (DC) X 47 Central Lancashire, University of (UK) X 48 Chicago, University of- Yerkes Obs. (IL) X 49 Chile, University of (Chile) X 50 Cologne, University of (Germany) X

51 Colorado, University of - JILA, CAS A, L ASP (CO) X X 52 Columbia University (NY) X X 53 Copenhagen University Observatory (Denmark) X 54 Cork, University of (Ireland) X X 55 Cornell University (NY) X X X

56 Cote d'Azur, Observatoire de la (France) X 57 Dartmouth College (NH) X 58 Delaware, University of (DE) X 59 Durham, University of (UK) X 60 ETH Zurich, Institute of Astronomy (Switzerland) X Institutions Whose Visitors Used NRAO Telescopes in 2002 mfc Observin? iummani 2002 15

VLA VLBA GBT 61 Etudes Spatiales, Centre National d' (France) X 62 European Southern Observatory (Chile) (Germany) X 63 European Space Agency - ESTEC, EXOSAT (Netherlands) X 64 Florida, University of (FL) X 65 FOMI Satellite Geodetic Observatory (Hungary)

66 George Mason University (VA) X 67 Granada (Spain) X 68 Groningen, University of- Kapteyn Institute (Netherlands) X X 69 Guadalajara, Universidad de (Mexico) X 70 Guanajuato, Universidad de (Mexico) X

71 Hamburg Institute (Germany) X 72 Harvard-Smithsonian Center for Astrophysics - SAO, Whipple (MA) X X X 73 Hawaii, University of- Institute for Astronomy (HI) X 74 Haystack Observatory - NEROC (MA) X X 75 Herfordshire University (UK) X

76 IAFE - Buenos Aires (Argentina) X 77 lAP-Paris (France) X 78 Ibaraki University (Japan) X 79 IBM Research Division (NY) X 80 lEEC-Barcelona X X Institutions Whose Visitors Used NRAO Telescopes in 2002 H Observin? iumman) 2002

81 Indian Institute of Astrophysics (India) 82 Indiana, University of (IN) 83 Inter-University Centre for Astronomy and Astrophysics (India) 84 Iowa, University of (IA) X 85 Jaen University (Spain) X

86 Jet Propulsion Laboratory (CA) X X X 84 John Moores University (UK) X X 88 Johns Hopkins University (MD) X X X 89 Kagoshima University (Japan) X 90 Keele, University of (UK)

91 Kennesaw State University (GA) X 92 Kentucky, University of (KY) X 93 Kyoto University (Japan) X 94 LAEFF- Madrid (Spain) X X 95 Lancashire, University of Central(UK) X

96 Lawrence Livermore National Laboratory (CA) X 97 Leeds, University of (UK) X 98 Leicester, University of (UK) X 99 Leiden University - Hyugens Labs (Netherlands) X X 100 Lisbon, University of (Portugal) X X Institutions Whose Visitors Used NRAO Telescopes in 2002 two 0b*emn?Jummanj2OO2 17

VLA VLBA GBT 101 London, University of (UK) X 102 Lowell Observatory (AZ) X 103 Madeira University (Portugal) X 104 Madrid, Universidad Complutense de (Spain) X 105 Manchester Institute of Science and Technology, Univ. of (UK)

106 Manchester, University of - Jodrell Bank, NRAL (UK) X X X 107 Maryland, University of (MD) X X 108 Massachusetts Institute of Technology - Lincoln Labs (MA) X 109 McDonald Observatory X 110 McGill University (Canada) X

111 McMaster University (Canada) X 112 Metsahovi Radio Observatory (Finland) X X 113 Michigan, University of (MI) X X 114 Milano, Universita degli Studi Di (Italy) X 115 Millimetric, Institut de Radioastronomie, (Spain)

116 Minnesota, University of (MN) X X 117 Montreal, University of (Canada) X 118 Moscow State University - Sternberg State Astronomy Institution (Russia) X 119 MPIAP, Munich (Germany) X 120 MPIR, Bonn (Germany) Institutions Whose Visitors Used NRAO Telescopes in 2002 iftib Obiervin? Nummary 2002 18

VLA VLBA GBT 121 Mt. Stromlo Observatory (Australia) X 122 NASA Goddard Space Flight Center (MD) X X 123 NASA Marshall Space Flight Center (AL) 124 National Astronomical Observatory - Subaru Telescope (Japan) X X 125 National Center for Radio Astrophysics (India) X

126 National Center for Remote Sensing (Morocco) X 127 National Central Unversity, loA (Taiwan) X 128 National Optical Astronomy Observatory (AZ) X X 129 National Radio Astronomy Observatory (NM, VA, WV, AZ) X X X 130 Naval Research Lab (DC) X X X

131 New Jersey Institute of Technology (NJ) X 132 New Mexico Institute of Mining and Technology (NM) X 133 New Mexico State University (NM) X X X 134 New Mexico, University of (NM) X X X 135 New South Wales, University of (Australia) X

136 NFRA - JIVE, Dwingeloo, Zwiggelte, Westerbork (Netherlands) X X X 137 Northwestern University (IL) X X 138 Observatory Astronomico Nacional (Spain) X 139 Ohio State University (OH) X X 140 Oklahoma, University of (OK) X X Institutions Whose Visitors Used NRAO Telescopes in 2002 mfc Obwrvin? Jumman) 2002 19

LA VLBA GBT 141 Onsala Space Observatory (Sweden) X X X 142 Oxford University (UK) X 143 Padova, University of (Italy) 144 Paris, Observatoire de (Meudon) - DEMIRM (France) 145 Paris, Observatoire de (Paris) (France) X

146 Peking University (China) X 147 Pennsylvania State University (PA) X 148 Potsdam, University of (Germany) X 149 Princeton University (NJ) X X 150 Puerto Rico University (Puerto Rico) X

151 Purdue University (IN) X 152 Purple Mountain Observatory, Nanjing (China) X 153 Queens University (Canada) X 154 Radioastronomia, Institute de (Italy) 155 Radiometrics, Inc. (MD) X

156 Raman Research Institute (India) X X 157 Royal Observatory of Belgium (Belgium) X 15 8 Royal Observatory of Edinburgh (UK) X 159 Rutgers State University of New Jersey (NJ) X 160 SETI Institute (CA) X 51 Institutions Whose Visitors Used NRAO Telescopes in 2002 two■ Observin? Nummary 2002 20

VLA VLBA GBT 161 Sheffield, University of (UK) X 162 Southampton, University of (UK) X 163 Space and Astronautical Science, Institute of (Japan)) X 164 Space Telescope Science Institute (MD) X X X 165 St. Petersburg State University (Russia) X

166 Stanford University (CA) X 167 Sternberg Astronomical Institute of Russia X X 168 Stockhom Observatory (Sweden) X 169 Sweet Briar College (VA) X 170 Tata Institute Fundamental Research - GMRT, RAC (India) X

171 Texas, University of, Austin (TX) X 172 Tohoku University (Japan) X 173 Tokyo, University of- Tokyo Astronomy Observatory (Japan) X 174 Toronto, University of- David Dunlop Observatory - CITA(Canada) X X 175 Trieste, Osservatorio Astronomico (Italy) X X

176 Trinity College (TX) X 177 Union College (NY) 178 United States Naval Observatory (DC) X 179 University College London - MLSS (UK) X 180 Uppsala Astronomical Observatory (Sweden) X Institutions Whose Visitors Used NRAO Telescopes in 2002 mJEb Observin? fummanj 2002 21

VLA VLBA GBT 181 Valencia, Universidad de (Spain) X X X 182 Virginia, University of (VA) X X 183 Washington State University (WA) 184 Whittier College (CA) X 185 Wisconsin, University of (WI) X

186 Yale University (CT) X X X 187 York University (Canada) 188 Yunnan Observatory (China)

NUMBER OF INSTITUTIONS 148 82 55

NUMBER OF VISITORS (includes students) 693 311 126 NUMBER OF STUDENTS 79 47 12 NUMBER OF RESEARCH ASSOCIATES AT NRAO 07 05 02 NUMBER OF PERMANENT STAFF

TOTAL OBSERVERS 731 342 148

All told, 1003 visitors, including 107 students, from 188 institutions. 5! NRAO Student Program ■two Observin? iummari) 2002 22

220 - himmer Undergraduah 200 1 1 Summer Graduate - - \ . ] Ph n 180 - - -3 i —"1 160 1 - est lEg 140 - 1 1

——A S3 120 ~ ■ 6 Z 100 - - 80 -

60 -

40

20

1988 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 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. J3I NRAO Front-End Status - Very Long Baseline Array mSb Obtervin?Jummanj2002 23

(MARCH 2003 SYSTEM 3db PERSON(S) FREQUENCY AMPLIFIER CAUBRATION SWITCHMC TEMPERATURE BANDWIDTH FEED TYPE POLARIZATION REMARKS IN (MHi) TYPE VALUE SYSTEM (KELVIN) ("Hz) CHARGE DUAL NOISE INJECTION UNCOOL£D 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 FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION CCKXED 2150-2350 35 128 CASSEGRA1N 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 6000-8800 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 Front-End Status - Very Large Array two

Observin? Nummary 2002 ih

MARCH 2003 SYSTEM 3db PERSONS) FREQUENCY AMPLIFIER CAUBRATION SWITCHING (MHz) TYPE TEMPERATURE BANDVNDTH FEED TYPE POLARIZATION VALUE SYSTEM REMARKS M (KELVM) (MHz) CHARGE DUAL NOISE INJECTION UNCOOLED PRIME 74 -1200 0.8 ORTHOGONAL 120 9.6 Hz TYPICALLY INSTAI1 FT) DURING A-ARRAY MERTELY FET FOCUS CIRCULAR 50 PERCENT CYCLE 3 MHz DUAL NOISE INJECTION UNCOOLED PRIME 308-343 160 (LIMITED BY ORTHOGONAL 10 9.6 Hz MbRIELY FET FOCUS INTERFERENCE) CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOiFD 35 55 CASSEGRAIN ORTHOGONAL 4 9.6 Hz MERTELY 1340-1730 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 35 55 CASSEGRAIN ORTHOGONAL 4 9.6 Hz MERTELY 8000-8800 FET CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION COOLED 14400-15400 CASSEGRAIN ORTHOGONAL 7 9.6 Hz FET 140 55 MERTELY CIRCULAR 50 PERCENT CYCLE DUAL NOISE INJECTION 50K Tsy* EXCEPT ON ANTENNAS 12.13, 22000-24000 COOLED 130/50 55 CASSEGRAIN ORTHOGONAL 10M 9.6 Hz MERTELY FET 14,22 & 27. CIRCULAR 50 PERCENTCYCLE NRAO Front-End Status - Green Bank Telescope two Ob$ervin?Jummanj2002 25

MARCH 2003 SYSTEM TEMP MAXIMUM CALIBRATION PERSONS) RECEIVER FREQUENCY AMPUFER swrrcHMQ KELVIN BANDWIDTH FEED TYPE POLARIZATION VALUE REMARKS M NAME (GHi) TYPE SYSTEM (ESTMATED) (MHz) (APPROXIMATE) CHARGE PRIME PFI COOLED ANDERSON 290-395 MHz 70 80 SHORT LIN/CIRC 2/40K FREQUENCY DUAL POLARIZATION 340 MHz HFET BAUSERMAN BACKFIRE PRIME PFI COOLED ANDERSON 385-520 MHz 57 80 SHORT LINKJIRC 2M0K FREQUENCY DUAL POLARIZATION 450 MHz HFET BAUSERMAN BACKFIRE PRIME PFI COOLED ANDERSON 46 80 SHORT LIN/CIRC 2/40K FREQUENCY DUAL POLARIZATION 600 MHz 510-690 MHz HFbl BAUSERMAN BACKFIRE PFI COOLED PRIME ANDERSON 680-920 MHz 25 240 UN/CIRC 2/40K FREQUENCY DUAL POLARIZATION 800 MHz HFET CONICAL BAUSERMAN

COOLED PRIME ANDERSON PF2 0.910-1.23 22 240 LM/CIRC 2/40K FREQUENCY UNDER CONSTRUCTION HFET CONICAL BAUSERMAN

COOLED STENNES L-BAND 1.15-1.73 18 580 GREGORIAN LIN/CIRC 2/20K FREQUENCY DUAL POLARIZATION HFET GUTHRIE

COOLED STENNES S-BAND 1.73-2.60 20 870 GREGORIAN LWCIRC 2/20K FREQUENCY DUAL POLARIZATION HFET GUTHRIE

COOLED C-BAND 3.95-5.85 25 2000 GREGORIAN LIN/CIRC 3/30K FREQUENCY DUAL POLARIZATION SIMON HFET

COOLED STENNES X-BAND 8-10.1 25 2100 GREGORIAN CIRC 2.&25K FREQUENCY DUAL POLARIZATION HFET GUTHRIE

COOLED FREQUENCY. 2 BEAMS, SEPARATED BY 5 AMIN STENNES Ku-BAND 12 -15.4 30 3500 GREGORIAN CIRC 3»0K WET BEAM DUAL POLARIZATION GUTHRIE

COOLED FREQUENCY, 2 BEAMS, SEPARATED BY 4 AMIN STENNES K-BAND 18-26.5 40 4000 GREGORIAN CIRC AMOK HFET BEAM DUAL POLARIZATION GUTHRIE NRAO - Staff and Visitor Publications 2002 two Observin? Jummanj 2002 26

AGUDO, I.; GOMEZ, J.L.; GABUZDA, D.C.; ALBERDI, A.; MARSCHER, A.P.; JORSTAD, S.G. "Multi-frequency VLBI Observations of the BL Lac Object 0735+178." European VLBI Network Symp. 6:115-118,2002.

AHMAD, F.; SASLAW, W.C.; BHAT, N.I. "Statistical Mechanics of the Cosmological Many-Body Problem." ApJ 571:576-584,2002.

ALLER, H.D.; ALLER, M.F.; HUGHES, P.A. "Oblique Polarization Structures in AGN and QSO Radio Jets." European VLBI Network Symp. 6: 111-114,2002.

ANGLADA, G.; RODRIGUEZ, L.F. "VLA Detection of the Exciting Sources of the Molecular Outflows Associated with L1448IRS2, IRAS 05327+3404, L43, IRAS 22142+5206, L1211, and IRAS 23545+6508." Rev. Mex. A&A 38:13-21, 2002.

APPLETON, P.N.; CHARMANDARIS, V.; GAO, Y.; COMBES, F.; GHIGO, F.; HORELLOU, C; MIRABEL, I.F. "Mid-Infrared and CO Observations of the Infrared/X-ray Luminous Seyfert I Galaxy NGC 985: The Making or Breaking of a ULIRG?" ApJ 566: 682-698,2002.

ARCE, H.G.; GOODMAN, A.A. "The Great PV Cephei Outflow: A Case Study in Outflow-Cloud Interaction." ApJ 575:911-927, 2002.

ASADA, K.; INOUE, M.; UCHIDA, Y.; KAMENO, S.; FUJISAWA, K.; IGUCHI, S.; MUTOH, M. "A Helical Magnetic Field in the Jet of 3C 273." PASJ 54:L39-L43,2002.

AUFDENBERG, J.P.; HAUSCHILDT, P.H.; BARON, E.; NORDGREN, T.E.; BURNLEY, A.W.; HOWARTH, I.D.; GORDON, K.D.; STANSBERRY, J.A. "The Spectral Energy Distribution and Mass-Loss Rate of the A-type Supergiant Deneb." ApJ 570: 344-368,2002.

BACH, U.; KRICHBAUM, T.P.; ALEF, W.; WITZEL, A.; ZENSUS, J.A. "Proper Motion in Cyg A." European VLBI Network Symp. 6:155-158,2002.

BAKKER, E.J.; MILEY, G.; WATERS, R.; LE POOLE, R.; JAFFE, W.; ROTTGERING, H.; PERCHERON, I.; MEISNER, J.; DE JONG, J.; HARTMANN, D.; COTTON, B.; HEIJLIGERS, B.; VAN BOEKEL, R.; GLINDEMANN, A.; D'ARCIO, L.; BOLAND, W. "NEVEC: The NOVA ESO VLTI Expertise Centre." In: Scientific Drivers for ESO Future VLT/VLTI Instrumentation (Springer, ed. Bergeron & Monnet): 347-349,2002.

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