DOCSLIB.ORG

National Radio Astronomy Observatory Observing

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
National Radio Astronomy Observatory Observing NATIONAL RADIO ASTRONOMY OBSERVATORY OBSERVING SUMMARY-1989 STATISTICS February 1990 Cover The Radio Galaxy Fornax A The cover photograph is a superposition of the VLA radio emission (shown as red) from the radio galaxy Fornax A and the visible light in the vicinity of NGC 1316 (shown as blue-white). The two main radio emitting lobes are produced by relativistic electrons in magnetic fields which have been transported hundreds of thousands of light years outward from the elliptical galaxy NGC 1316 which lies between the two regions. The energy for the relativistic flow apparently was provided by the gravitational capture of small galaxies by NGC 1316. The shock waves and trails of the infallen galaxies produce the features in the radio lobes seen as filaments and rings. The small galaxy near NGC 1316 may soon be captured. Observation details: Observers: E. Fomalont (NRAO), R. Ekers (Australia Telescope), K. Ebneter and W. Van Breugel (U. California) Frequency of 1.384 GHz; five hours of D-configuration and five hours of C-configuration Resolution of 15"; field of view is 60' x 40' NATIONAL RADIO ASTRONOMY OBSERVATORY OBSERVING SUMMARY 1989 STATISTICS FEBRUARY 1990 SOME HIGHLIGHTS OF THE 1989 RESEARCH PROGRAM A second Einstein Ring has been identified from new A-configuration VLA observations of MG1652+138, the second candidate for an Einstein ring gravitational lens system to be selected from the MIT-Green Bank 5 GHz survey. Optical images and spectra established the redshift of a faint blue quasar between the two radio sources, while the VLA results have both detected the quasar core at its optical location and improved the ring image quality. The Einstein ring is thought to be the gravitationally lensed image of one of the quasar's radio lobes by an intervening galaxy. The VLA successfully observed a radar bounce from Saturn's largest satellite, Titan. The 8.6 GHz signals were transmitted from the 70-meter DSN Goldstone antenna and received 2.5 hours later at the VLA. The radar echo from Titan- is the weakest such echo ever measured. Differences in surface reflectivity from day to data indicate a highly variable surface on Titan, while the low reflectivity could indicate the presence of a deep ethane ocean. HI observations made with the Areclbo and 140-ft telescopes of the unique galaxy Mai in 1 have shown it to contain an enormous HI disk, of diameter greater than 240 kpc, and mass in excess of 1011 solar masses, making it the largest HI mass of any known galaxy. The low optical surface brightness indicates that Malin 1 has extremely inefficient star formation. It appears to be an unevolvlng disk galaxy whose surface mass density is so low that the chemical composition and mass fraction in gas change very slowly over Hubble times. Interstellar C^D has been detected at 17.6 GHz at the 140-ft, with signal strengths of only a few milli-kelvin, representing a considerable technical feat. Deuterated species are important diagnostics of interstellar ion-molecule chemistry. The observed C4D/C4H abundance ratio is consistent with model predictions, and confirms the expectation that the ratio decreases as the number of carbon atoms in the molecule increases. However, C4D/C4H is only about 5 percent of the C3HD/C3H2 ratio, indicating a problem in the current understanding of the ring species €3^. CO has been detected by the 12-meter telescope in the nearby Sc galaxy M33. Although HI has been long known in M33, previous studies suggested that the molecular gas content was low. A map of the CO emission reveals several large, unbound, molecular clouds, and a relative content of molecular to atomic gas comparable with that in our own galaxy. However, the total mass of M33 is considerably less than the Milky Way, which accounts for the weak CO emission and the difficulty of the long search. In 1989 September the VLA was used in support of the launch of the Normal Incidence X-ray Telescope (NIXT), which provides X-ray images of the sun's corona at one arcsecond resolution. The VLA discovered a powerful flare near the center of the sun's disk, with up to 100 percent circular polarization, and a maximum brightness temperature in excess of 1010 K. These properties are indicative of coherent emission processes (cyclotron maser or plasma radiation). The VLA has performed the first direct image of such a coherent microwave source. Together with the NIXT, Solar Maximum Mission satellite, and ground-based optical observations, the coherent emission mechanism may be identified with a high degree of confidence. Observing Hours 1977 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 Calendar Year 300-Foot MO-Foot iH 12Meter ("31 Interferometer I \VLA Fig. 1. This figure shows the hours scheduled for observing on each telescope during the last decade. Distribution of Scheduled Observing Time 12-Meter 140-Foot VLA o o o o3 1980 81 82 83 84 85 86 87 88 89 1980 81 82 83 84 85 86 87 88 89 1981 82 83 84 85 86 87 88 89 Calendar Year Calendar Year Calendar Year NRAO Staff | Visitors m Testing and Calibration Fig. 2. These graphs show the number of hours scheduled for calibration and for observing by the NRAO staff and by visitors on each telescope system during the last decade. 12-Meter Radio Telescope Summary 1980 I98l 1982 1983 I984 1985 1986 I987 I988 1989 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. During the last half of 1982 and most of 1983 the telescope was out of service for the replacement of the reflecting surface and its backup structure. 140-Foot Radio Telescope Summary 100 ■ I - /~ -s - ^\ /"■ ^ s^ ^ ^' y s^ \ ^N y /s •s LV A /"" / 80 > vN^ V i IV X> s V.- /* V V "^^ y f V / V • / N 60 •\ i vyV ' V - 40 A A - " / ! \ A 20 ^ ^7 \ r/s > \ y V V s - 5k- -< 4 ^ . ^ .-. 4 '•»••■ x^. ^-. s 0 \- '"1 -i —J ^1 -mm* 1980 1981 1982 1983 1984 1985 1986 1987 1988 1989 Calendar Year Observing Installation, Maintenance and Calibration Equipment Failure, Weather and Interference Fig. 4. This summary for each quarter of the calendar year shows the percentage of time the telescope was scheduled for observing; for routine 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: 1980 - installation of the Model IV autocorrelation receiver; 1982 - beam efficiency and pointing tests at 1.3 cm; 1983 - brake overhaul and installation of the second channel of the upconverter/maser receiver; 1987 - holographic surface tests and panel readjustments. Very Large Array Telescope Summary 100 - - 80 '**" 1 ^ \ ^S — — ^^ -^ — s ^ ^s ^ ^. - /^ »sX *- " - V /" ^ 60 / *s a> o r "^> f - 40 tr ^ st V A v. S r* ^ - v_ — — —■ ^ _ —^ ^- ^_ r N , / ^s X\ 20 , - ** s« _ * ^N "^ \ s 'x_ .-. >*^. .-. — v^ ^^« • —. •« . —- —- ..»- .-« ■ ._. .— ... .__. .— -> ._. .-• »^- '- —.. 0 V Calendar Year Construction Observing Testing, Maintenance and Calibration Downtime Fig. 5. This summary for each quarter of the calendar year shows the percentage of time 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. Time scheduled for completion of the construction was reduced to zero after the first quarter of 1981. Full-Time Permanent Employees 500 1976 1977 1978 1979 1980 1981 1982 1983 1984 1985 1986 1987 1988 1989 1990 1991 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 1000 I J 950 $8® Visitors and Students ~ - 900 V/A Research Associates - ■1 Permanent Staff 850 est. - - f^H Number of Institutiom t 1 - 800 i^< _, 1 M 750 H^ XW S^: em ^ 1 ^ 1 - 700 mi -m- — £$ — 1 ^ 1 650 I888E i m — M —-1- :•&# m ffl 1 : : : : $ S« : : : : : $S •ip ^ ■ 600 ili m M j^ ^ : ■x-x 1 m :W: m m ^ II . iW: 4fe$ i^ M w550 m m m m - m m 1 ^ X*5S £500 i i W i m ^ ii - m Z x-i'i* 81 450 ii 1 m 1 i m - M ■%•■•' m 1 M P •^•: ^ 400 : : : : _ ;:;.;•:•; •:W: « •x-x : : : : , •:•:?: m II M XWl*v. 350 X'X? m ^i -§- :•!•:•:•: e.:.;:si -I- S::§ S$s — : : : 1 1 — — m ■ .-•-.-.-. ■■ 1 "" ■" .••••*.•. "■ " !•'•■•'• ■'" I ■ ■ ■X'X* '" " 300 V.V.' • *•"•*. .••••••", "••••X I•:•»: m : : x " : :•;•£ ;•;•>>; x-x - ■ m :•:•?>: M $•& S$S ^ : jsS $8$. — m m —#$:—m m M :5¥: : 250 •:■:•;•■. Mi — M — M': : : m m m ; : : : ; sn -»- :?:•:: « ^ X'X' •Xv! :«•:■ ~w- vXv ::«• :¥:% ■x^x :?& ft?: :%¥ ': : :": && : : :: — 200 '.•'.''.•'.'_ """ 'X^v :-::xj ■ $•§■! """ - M ^ '.•'.''.•'.• M M~-m- — SS — -»- I^S pr •Xvl" Ii- 150 M ^ M. ^ ■* ivi'i*" M F %•;•! •.v.v !_PF 100 - ill •:•;•:■:' !? — iirSii: - 4 ^5" T~ 1 :| n n :?:§ * >ivi — !&&■.¥ .• — ^ ■ =? 50 ' — — — ■ ; ~M' : 5*^* "I". —;.:J.:J ■ _l|. _ 22. 7$ M tf i ' 0' i 1975 1976 1977 1978 1979 1980 1981 1982 1983 1984 1985 1986 1987 1988 1989 1990 Calendar Year Fig.
Load more

Recommended publications
  • Kinematics of Planetary Nebulae in M51's Tidal Debris
    Draft version December 17, 2018 A Preprint typeset using L TEX style emulateapj v. 14/09/00 KINEMATICS OF PLANETARY NEBULAE IN M51’S TIDAL DEBRIS Patrick R. Durrell [email protected] Department of Astronomy and Astrophysics, Penn State University, 525 Davey Lab, University Park, PA 16802 J. Christopher Mihos1, John J. Feldmeier [email protected], [email protected] Department of Astronomy, Case Western Reserve University, 10900 Euclid Ave, Cleveland, OH 44106 George H. Jacoby [email protected] WIYN Observatory2, P.O. Box 26732, Tucson AZ 85726 and Robin Ciardullo [email protected] Department of Astronomy and Astrophysics, Penn State University, 525 Davey Lab, University Park, PA 16802 accepted for publication in the Astrophysical Journal ABSTRACT We report the results of a radial velocity survey of planetary nebulae (PNe) located in the tidal features of the well-known interacting system NGC 5194/95 (M51). We find clear kinematic evidence that M51’s northwestern tidal debris consists of two discrete structures which overlap in projection – NGC 5195’s own tidal tail, and diffuse material stripped from NGC 5194. We compare these kinematic data to a new numerical simulation of the M51 system, and show that the data are consistent with the classic “single passage” model for the encounter, with a parabolic satellite trajectory and a 2:1 mass ratio. We also comment on the spectra of two unusual objects: a high-velocity PN which may be associated with NGC 5194’s halo, and a possible interloping high-redshift galaxy. Subject headings: galaxies: individual (M51) — galaxies: interactions — galaxies: kinematics and dynamics — planetary nebulae: general 1.
    [Show full text]
  • Arxiv:1903.02002V1 [Astro-Ph.GA] 5 Mar 2019
    Draft version March 7, 2019 Typeset using LATEX twocolumn style in AASTeX62 RELICS: Reionization Lensing Cluster Survey Dan Coe,1 Brett Salmon,1 Maruˇsa Bradacˇ,2 Larry D. Bradley,1 Keren Sharon,3 Adi Zitrin,4 Ana Acebron,4 Catherine Cerny,5 Nathalia´ Cibirka,4 Victoria Strait,2 Rachel Paterno-Mahler,3 Guillaume Mahler,3 Roberto J. Avila,1 Sara Ogaz,1 Kuang-Han Huang,2 Debora Pelliccia,2, 6 Daniel P. Stark,7 Ramesh Mainali,7 Pascal A. Oesch,8 Michele Trenti,9, 10 Daniela Carrasco,9 William A. Dawson,11 Steven A. Rodney,12 Louis-Gregory Strolger,1 Adam G. Riess,1 Christine Jones,13 Brenda L. Frye,7 Nicole G. Czakon,14 Keiichi Umetsu,14 Benedetta Vulcani,15 Or Graur,13, 16, 17 Saurabh W. Jha,18 Melissa L. Graham,19 Alberto Molino,20, 21 Mario Nonino,22 Jens Hjorth,23 Jonatan Selsing,24, 25 Lise Christensen,23 Shotaro Kikuchihara,26, 27 Masami Ouchi,26, 28 Masamune Oguri,29, 30, 28 Brian Welch,31 Brian C. Lemaux,2 Felipe Andrade-Santos,13 Austin T. Hoag,2 Traci L. Johnson,32 Avery Peterson,32 Matthew Past,32 Carter Fox,3 Irene Agulli,4 Rachael Livermore,9, 10 Russell E. Ryan,1 Daniel Lam,33 Irene Sendra-Server,34 Sune Toft,24, 25 Lorenzo Lovisari,13 and Yuanyuan Su13 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2Department of Physics, University of California, Davis, CA 95616, USA 3Department of Astronomy, University of Michigan, 1085 South University Ave, Ann Arbor, MI 48109, USA 4Physics Department, Ben-Gurion University of the Negev, P.O.
    [Show full text]
  • Messier Objects
    Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun.
    [Show full text]
  • Radio Observations of the Merging Galaxy Cluster Abell 520 D
    A&A 622, A20 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833900 & c ESO 2019 Astrophysics LOFAR Surveys: a new window on the Universe Special issue Radio observations of the merging galaxy cluster Abell 520 D. N. Hoang1, T. W. Shimwell2,1, R. J. van Weeren1, G. Brunetti3, H. J. A. Röttgering1, F. Andrade-Santos4, A. Botteon3,5, M. Brüggen6, R. Cassano3, A. Drabent7, F. de Gasperin6, M. Hoeft7, H. T. Intema1, D. A. Rafferty6, A. Shweta8, and A. Stroe9 1 Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, The Netherlands e-mail: [email protected] 2 Netherlands Institute for Radio Astronomy (ASTRON), PO Box 2, 7990 AA Dwingeloo, The Netherlands 3 INAF-Istituto di Radioastronomia, via P. Gobetti 101, 40129 Bologna, Italy 4 Harvard-Smithsonian for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 5 Dipartimento di Fisica e Astronomia, Università di Bologna, via P. Gobetti 93/2, 40129 Bologna, Italy 6 Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 7 Thüringer Landessternwarte, Sternwarte 5, 07778 Tautenburg, Germany 8 Indian Institute of Science Education and Research (IISER), Pune, India 9 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany Received 18 July 2018 / Accepted 10 September 2018 ABSTRACT Context. Extended synchrotron radio sources are often observed in merging galaxy clusters. Studies of the extended emission help us to understand the mechanisms in which the radio emitting particles gain their relativistic energies. Aims. We examine the possible acceleration mechanisms of the relativistic particles that are responsible for the extended radio emis- sion in the merging galaxy cluster Abell 520.
    [Show full text]
  • INVESTIGATING ACTIVE GALACTIC NUCLEI with LOW FREQUENCY RADIO OBSERVATIONS By
    INVESTIGATING ACTIVE GALACTIC NUCLEI WITH LOW FREQUENCY RADIO OBSERVATIONS by MATTHEW LAZELL A thesis submitted to The University of Birmingham for the degree of DOCTOR OF PHILOSOPHY School of Physics & Astronomy College of Engineering and Physical Sciences The University of Birmingham March 2015 University of Birmingham Research Archive e-theses repository This unpublished thesis/dissertation is copyright of the author and/or third parties. The intellectual property rights of the author or third parties in respect of this work are as defined by The Copyright Designs and Patents Act 1988 or as modified by any successor legislation. Any use made of information contained in this thesis/dissertation must be in accordance with that legislation and must be properly acknowledged. Further distribution or reproduction in any format is prohibited without the permission of the copyright holder. Abstract Low frequency radio astronomy allows us to look at some of the fainter and older synchrotron emission from the relativistic plasma associated with active galactic nuclei in galaxies and clusters. In this thesis, we use the Giant Metrewave Radio Telescope to explore the impact that active galactic nuclei have on their surroundings. We present deep, high quality, 150–610 MHz radio observations for a sample of fifteen predominantly cool-core galaxy clusters. We in- vestigate a selection of these in detail, uncovering interesting radio features and using our multi-frequency data to derive various radio properties. For well-known clusters such as MS0735, our low noise images enable us to see in improved detail the radio lobes working against the intracluster medium, whilst deriving the energies and timescales of this event.
    [Show full text]
  • Provisional Scientific Programme
    Galaxy Clusters as Giant Cosmic Laboratories – Programme Monday, 21 May 2012 09:00 Registration 09:50 Schartel: Opening Remarks Session I Dynamical and Thermal Structure of Galaxy Clusters and their ICM Chair: Birzan 10:00 Sanders: The thermal and dynamical state of cluster cores 10:30 Ohashi: X-ray study of clusters at the outer edge and beyond 10:45 Eckert: The gas distribution in galaxy cluster outer regions 11:00 Molendi: Extending measures of the ICM to the outskirts: facts, myths and puzzles 11:15 Sato: Temperature, entropy, and mass profiles to the virial radius of galaxy clusters with Suzaku 11:30- Coffee Break & Poster Viewing 12:00 Session II Dynamical and Thermal Structure of Galaxy Clusters and their ICM Chair: Altieri Cluster Mass Determination 12:00 Ettori: Cluster mass profiles from X-ray observations: present constraints and limitations 12:30 Russell: Shock fronts, electron-ion equilibration and ICM transport processes in the merging cluster Abell 2146 12:45 ZuHone: Probing the Microphysics of the Intracluster Medium with Cold Fronts in the ICM 13:00 Rossetti: Challenging the merging/sloshing cold front paradigm with a new XMM observation of A2142 13:15 Nevalainen: Bulk motion measurements in clusters of galaxies using XMM-Newton and ATHENA 13:30- Lunch 15:00 Session III Dynamical and Thermal Structure of Galaxy Clusters and their ICM Chair: de Grandi Cluster Mass Determination 15:00 Mahdavi: Multiwavelength Constraints on Scaling Relations and Substructure in a Sample of 50 Clusters of Galaxies 15:30 Pratt: Galaxy cluster
    [Show full text]
  • Do Normal Galaxies Host a Black Hole? the High Energy Perspective
    DO NORMAL GALAXIES HOST A BLACK HOLE? THE HIGH ENERGY PERSPECTIVE 1 Y. Terashima2 Nagoya University ABSTRACT We review ASCA results on a search for low luminosity active nuclei at the center of nearby normal galaxies. More than a dozen low-luminosity AGN have been discovered with 2–10 keV − − luminosity in the range 1040 41 ergs s 1. Their X-ray properties are in some respects similar to those of luminous Seyfert galaxies, but differ in other respects. We also present estimated black hole masses in low luminosity AGNs and a drastic activity decline in the nucleus of the radio galaxy Fornax A. These results altogether suggest that relics of the past luminous AGNs lurk in nearby normal galaxies. KEYWORDS: Galaxies; Low luminosity AGNs; LINERs; Black holes 1. Introduction The number density of quasars is peaked at a redshift of z ∼ 2 and rapidly de- creases toward smaller redshifts. In the local universe, there is no AGN emitting at huge luminosity like quasars. These facts infer that quasars evolve to supermassive black holes in nearby apparently normal galaxies (e.g. Rees 1990). The growing evidence for supermassive black holes in nearby galaxies are ob- tained from recent optical and radio observations of gas/stellar kinematics around the center of galaxies (e.g. Ho 1998a; Magorrian et al. 1998; Kormendy & Rich- stone 1995). If fueling to the supermassive black hole takes place with a small arXiv:astro-ph/9905218v1 17 May 1999 mass accretion rate, they are expected to be observed as very low luminosity AGNs compared to quasars. Recent optical spectroscopic surveys have shown that low level activity is fairly common in nearby galaxies.
    [Show full text]
  • What's in This Issue?
    A JPL Image of surface of Mars, and JPL Ingenuity Helicioptor illustration. July 11th at 4:00 PM, a family barbeque at HRPO!!! This is in lieu of our regular monthly meeting.) (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory) This is a pot-luck. Club will provide briskett and beverages, others will contribute as the spirit moves. What's In This Issue? President’s Message Member Meeting Minutes Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night SubReddit and Discord BRAS Member Astrophotos ARTICLE: Astrophotography with your Smart Phone Observing Notes: Canes Venatici – The Hunting Dogs Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society BRAS YouTube Channel Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 23 July 2021 President’s Message Hey everybody, happy fourth of July. I hope ya’ll’ve remembered your favorite coping mechanism for dealing with the long hot summers we have down here in the bayou state, or, at the very least, are making peace with the short nights that keep us from enjoying both a good night’s sleep and a productive observing/imaging session (as if we ever could get a long enough break from the rain for that to happen anyway). At any rate, we figured now would be as good a time as any to get the gang back together for a good old fashioned potluck style barbecue: to that end, we’ve moved the July meeting to the Sunday, 11 July at 4PM at HRPO.
    [Show full text]
  • Radio Astronom1y G
    £t,: ,/ NATIONAL RADIO ASTRONOMY OBSERVATORY QUARTERLY REPORT October 1 - December 31, 1989 RADIO ASTRONOM1Y G.. '8 tO- C~oe'' n,'evI! I E. Vi. t-Li 1 2 1990 TABLE OF CONTENTS A. TELESCOPE USAGE ... .... ...... ............ 1 B. 140-FOOT OBSERVING PROGRAMS . .... .......... ... 1 C. 12-METER TELESCOPE ....... ..... ., .... ........ 5 D. VERY LARGE ARRAY ....... 1...................8 E. SCIENTIFIC HIGHLIGHTS .... ........ 19 F. PUBLICATIONS ............. G. CENTRAL DEVELOPMENT LABORATORY ........ 20 H. GREEN BANK ELECTRONICS . .. .a.. ...... 21 I. 12-METER ELECTRONICS ...... .. 0. I. 22 J. VLA ELECTRONICS ...... 0..... ..... .... a. 24 K. AIPS .... .............. ...... ............. 26 L. VLA COMPUTER ............. .. .0. .0. ... 27 M. VERY LONG BASELINE ARRAY . .. .0 .0 .0 .0 .0 . .0 .. 27 N. PERSONNEL .. ...... .... .0.0 . .0. .0. .. e. 30 APPENDIX A: List of NRAO Preprints A. TELESCOPE USAGE The NRAO telescopes have been scheduled for research and maintenance in the following manner during the fourth quarter of 1989. 140-ft 12-m VLA Scheduled observing (hrs) 1901.75 1583.50 1565.2 Scheduled maintenance and equipment changes 132.00 107.75 259.8 Scheduled tests and calibrations 20.75 425.75 327.1 Time lost 139.25 208.25 107.0 Actual observing 1762.50 1375.25 1458.2 B. 140-FOOT OBSERVING PROGRAMS The following line programs were conducted during this quarter. No. Observer(s) Program A-95 Avery, L (Herzberg) Observations at 18.2, 18.6, and Bell, M. (Herzberg) 23.7 GHz of cyanopolyynes in carbon Feldman, P. (Herzberg) stars part II. MacLeod, J. (Herzberg) Matthews, H. (Herzberg) B-493 Bania, T. (Boston) Measurements at 8.666 GHz of 3He + Rood, R. (Virginia) emission in HII regions and planetary Wilson, T.
    [Show full text]
  • An Optical Spectroscopic Survey of the 3CR
    A&A 560, A81 (2013) Astronomy DOI: 10.1051/0004-6361/201322842 & c ESO 2013 Astrophysics An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3 V. Implications for the unified model for FR IIs Ranieri D. Baldi1, Alessandro Capetti2, Sara Buttiglione3, Marco Chiaberge4,5,6, and Annalisa Celotti1,7,8 1 SISSA-ISAS, via Bonomea 265, 34136 Trieste, Italy e-mail: [email protected] 2 INAF − Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy 3 INAF − Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 INAF − Istituto di Radio Astronomia, via P. Gobetti 101, 40129 Bologna, Italy 6 Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles Street Baltimore, MD 21218, USA 7 INAF − Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate, Italy 8 INFN − Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy Received 14 October 2013 / Accepted 30 October 2013 ABSTRACT We explore the implications of our optical spectroscopic survey of 3CR radio sources with z < 0.3 for the unified model (UM) for radio-loud AGN, focusing on objects with a “edge-brightened” (FR II) radio morphology. The sample contains 33 high ionization galaxies (HIGs) and 18 broad line objects (BLOs). According to the UM, HIGs, the narrow line sources, are the nuclearly obscured counterparts of BLOs. The fraction of HIGs indicates a covering factor of the circumnuclear matter of 65% that corresponds, adopting a torus geometry, to an opening angle of 50◦ ± 5.
    [Show full text]
  • Overview on Spectral Line Source Finding and Visualisation
    CSIRO PUBLISHING Publications of the Astronomical Society of Australia, 2012, 29, 359–370 http://dx.doi.org/10.1071/AS12030 Overview on Spectral Line Source Finding and Visualisation B. S. Koribalski CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia Email: [email protected] Abstract: Here I will outline successes and challenges for finding spectral line sources in large data cubes that are dominated by noise. This is a 3D challenge as the sources we wish to catalog are spread over several spatial pixels and spectral channels. While 2D searches can be applied, e.g. channel by channel, optimal searches take into account the 3-dimensional nature of the sources. In this overview I will focus on HI 21-cm spectral line source detection in extragalactic surveys, in particular HIPASS, the HI Parkes All-Sky Survey and WALLABY, the ASKAP HI All-Sky Survey. I use the original HIPASS data to highlight the diversity of spectral signatures of galaxies and gaseous clouds, both in emission and absorption. Among others, I report the À1 discovery of a 680 km s wide HI absorption trough in the megamaser galaxy NGC 5793. Issues such as source confusion and baseline ripples, typically encountered in single-dish HI surveys, are much reduced in interferometric HI surveys. Several large HI emission and absorption surveys are planned for the Australian Square Kilometre Array Pathfinder (ASKAP): here we focus on WALLABY, the 21-cm survey of the sky (d , þ308; z , 0.26) which will take about one year of observing time with ASKAP.
    [Show full text]
  • The Jets in Radio Galaxies
    The jets in radio galaxies Martin John Hardcastle Churchill College September 1996 A dissertation submitted in candidature for the degree of Doctor of Philosophy in the University of Cambridge i `Glaucon: ª...But how did you mean the study of astronomy to be reformed, so as to serve our pur- poses?º Socrates: ªIn this way. These intricate traceries on the sky are, no doubt, the loveliest and most perfect of material things, but still part of the visibleworld, and therefore they fall far short of the true realities Ð the real relativevelocities,in theworld of purenumber and all geometrical ®gures, of the movements which carry round the bodies involved in them. These, you will agree, can be conceived by reason and thought, not by the eye.º Glaucon: ªExactly.º Socrates: ªAccordingly, we must use the embroidered heaven as a model to illustrateour study of these realities, just as one might use diagrams exquisitely drawn by some consummate artist like Daedalus. An expert in geometry, meeting with such designs, would admire their ®nished workmanship, but he wouldthink it absurd to studythem in all earnest with the expectation of ®nding in their proportionsthe exact ratio of any one number to another...º ' Ð Plato (429±347 BC), The Republic, trans. F.M. Cornford. ii Contents 1 Introduction 1 1.1 Thisthesis...................................... ... 1 1.2 Abriefhistory................................... .... 2 1.3 Synchrotronphysics........ ........... ........... ...... 4 1.4 Currentobservationalknowledgeintheradio . ............. 5 1.4.1 Jets ........................................ 6 1.4.2 Coresornuclei ................................. 6 1.4.3 Hotspots ..................................... 7 1.4.4 Largescalestructure . .... 7 1.4.5 Theradiosourcemenagerie . .... 8 1.4.6 Observationaltrends .
    [Show full text]