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  • 1.
    Bartel, N.
    et al.
    Department of Earth and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA & Harvard-Smithsonian Astrophysical Observatory, Cambridge, MA, USA.
    Shapiro, I.I.
    Department of Earth and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA & Harvard-Smithsonian Astrophysical Observatory, Cambridge, MA, USA.
    Corey, B.E.
    NEROC, Haystack Observatory, Westford, MA, USA.
    Marcaide, J.M.
    Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA & Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Rogers, A.E.E.
    NEROC, Haystack Observatory, Westford, MA, USA.
    Whitney, A.R.
    NEROC, Haystack Observatory, Westford, MA, USA.
    Cappallo, R.J.
    NEROC, Haystack Observatory, Westford, MA, USA.
    Kühr, H.
    Steward Observatory, Tucson, AZ, USA.
    Graham, D.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Bååth, L.B.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    The Compact Radio Source 2021+614: Simultaneous 2.3 and 8.3 GHz Mark III VLBI Observations1984In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 279, no 1, p. 116-121Article in journal (Refereed)
    Abstract [en]

    Second-epoch VLBI observations of the flat-spectrum radio source 2021+614 made simultaneously at 2.3 and 8.3 GHz with the Mark III system are reported. The maps derived from these observations reveal a complex, frequency-dependent radio structure on the milliarcsecond scale. The object has four nearly collinear components oriented at a position angle of about 35 degrees and embedded in an extended region. Two of these are optically thin, one has a flat spectrum, and the other appears to be synchrotron self-absorbed in the frequency range 2.3-8.3 GHz. No significant structural variation is found at either frequency between epochs separated by about three years. The formal estimate of the transverse velocity between two components, one with a flat and the other with an inverted spectrum, is v/c = 0.7 + or - 2.3. Remarkable similarities between 2021+614 and the unusual source 0316+413 are discussed.

  • 2.
    Bååth, L.B.
    et al.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    Rönnäng, B.O.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    Pauliny-Toth, I.I.K.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Kellermann, K.I.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Preuss, E.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Witzel, A.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Matveenko, L.I.
    Space Research Institute, Moscow, USSR.
    Kogan, L.R.
    Space Research Institute, Moscow, USSR.
    Kostenko, V.I.
    Space Research Institute, Moscow, USSR.
    Moiseev, I.G.
    Crimean Astrophysical Observatory, USSR Academy of Sciences, P/O Nauchny, Crimea, USSR.
    Shaffer, D.B.
    National Radio Astronomy Observatory, Goddard Space Flight Center, Greenbelt, MD, USA.
    High Resolution Observations of the QSO 3C 345 at 1.3 centimeters1981In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 243, p. L123-L126Article in journal (Refereed)
    Abstract [en]

    High-resolution VLBI observations made at a frequency of 22.235 GHz of the quasar 3C 345 are discussed. Antennas located at the Crimean Astrophysical Observatory, USSR; Onsala, Sweden; Effelsberg, West Germany; and the Haystack Observatory, Massachusetts were employed at 4-min integration times to provide baselines ranging up to 5.5 x 10 to the 8th wavelengths. About 40% of the total flux density of 7.85 Jy, observed in November 1977, and 8.05 Jy, observed in October 1978, is found to originate in an unresolved component of the quasar core in a region less than 0.1 milliarcsec in diameter. The elongated jet-like component of the quasar is observed to contain several peaks of emission extending up to 6 milliarsec from the core which decreased in extent between the two observations.

  • 3.
    Cotton, W. D.
    et al.
    National Radio Astronomy Observatory, Socorro, NM, USA.
    Owen, F. N.
    National Radio Astronomy Observatory, Socorro, NM, USA.
    Geldzahler, B. J.
    E. O. Hulburt Center for Space Research, Washington, DC, USA.
    Johnston, K.
    E. O. Hulburt Center for Space Research, Washington, DC, USA.
    Bååth, L.B.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    Romney, J.
    Max-Planck Institut für Radioastronomie, Bonn, Germany.
    High Resolution Observations of the Steep Spectrum Source 2147+1451984In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 277, p. L41-L44Article in journal (Refereed)
    Abstract [en]

    The results of an eight station, 18-cm intercontinental very long baseline interferometry for which the synthesized beam obtained was 0.008 x 0.003 arcsec are presented for the steep spectrum compact radio source 2147+145. These observations reveal a structure similar to flat spectrum compact sources and, if the source radiates due to the synchrotron process, a very weak magnetic field. The source consists of a line of knots 0.022 arcsec long along position angle of 38 deg dominated on one side by a component of size 0.0032 arcsec measured along a position angle of 38 deg. It is suggested that 2147+145 and, perhaps, related steep spectrum objects are similar to flat spectrum, optically active sources except that the magnetic field is much weaker.

  • 4.
    Jones, D. L.
    et al.
    Owens Valley Radio Observatory, California Institute of Technology, Pasadena, California, USA.
    Unwin, S. C.
    Owens Valley Radio Observatory, California Institute of Technology, Pasadena, California, USA.
    Readhead, A. C. S.
    Owens Valley Radio Observatory, California Institute of Technology, Pasadena, California, USA.
    Sargent, W. L. W.
    Owens Valley Radio Observatory, California Institute of Technology, Pasadena, California, USA.
    Seielstad, G. A.
    Owens Valley Radio Observatory, California Institute of Technology, Pasadena, California, USA.
    Simon, R. S.
    Naval Research Laboratory, Washington, USA.
    Walker, R. C.
    National Radio Astronomy Observatory, Socorro, New Mexico, USA.
    Benson, J. M.
    National Radio Astronomy Observatory, Socorro, New Mexico, USA.
    Perley, R. A.
    National Radio Astronomy Observatory, Socorro, New Mexico, USA.
    Bridle, A. H.
    National Radio Astronomy Observatory, Socorro, New Mexico, USA.
    Pauliny-Toth, I. I. K.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Romney, J.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Witzel, A.
    Max-Planck-Institut für Radioastronomie, Bonn, Germany.
    Wilkinson, P. N.
    Jodrell Bank, The University of Manchester, Macclesfield, United Kingdom.
    Bååth, L.B.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    Booth, R. S.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    Fort, D. N.
    Algonquin Radio Observatory, Lake Traverse, Ontario, Canada.
    Galt, J. A.
    Dominion Radio Astrophysical Observatory, Penticton, Canada.
    Mutel, R. L.
    University of Iowa, Iowa City, USA.
    Linfield, R. P.
    Hat Creek Radio Observatory, Redding, California, USA.
    High dynamic range VLBI observations of NGC 62511986In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 305, no 2, p. 684-697Article in journal (Refereed)
  • 5.
    Mundy, Lee G.
    et al.
    Owens Valley Radio Observatory, Californa Institute of Technology, Pasadena, CA, USA.
    Cornwell, T. J.
    National Radio Astronomy Observatory, Socorro, NM, USA.
    Masson, Colin R.
    Owens Valley Radio Observatory, Californa Institute of Technology, Pasadena, CA, USA.
    Scoville, Nicholas Z.
    Owens Valley Radio Observatory, Californa Institute of Technology, Pasadena, CA, USA.
    Bååth, L.B.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    Johansson, Lars E. B.
    Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden.
    High-resolution images of the Orion molecular ridge in the CS J = 2-1 transition1988In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 325, no 1, p. 382-388Article in journal (Refereed)
    Abstract [en]

    The authors have constructed 7arcsec.5 resolution images of the CS J = 2-1 emission from a 3arcmin.5 section of the Orion molecular ridge using a maximum entropy algorithm to combine Owens Valley Millimeter-Wave Interferometer and Onsala Space Observatory 20 m data. The resulting images include all of the flux and have positional accuracy of 1arcsec-2arcsec on the small-scale features. The observed section of the ridge includes four condensations. The condensations have dimensions from 0.03 to 0.11 pc and virial massses from 30 to 80 M_sun;. Approximately 70% of the total mass within the 3arcmin region is contained in these condensations.

  • 6.
    Mundy, Lee G.
    et al.
    California Institute of Technology, Pasadena, CA, USA.
    Scoville, Nicholas Z.
    California Institute of Technology, Pasadena, CA, USA.
    Bååth, Lars B.
    Onsala Space Observatory, Onsala, Sweden.
    Masson, Colin R.
    California Institute of Technology, Pasadena, CA, USA.
    Woody, David P.
    Owens Valley Radio Observatory, Big Pine, CA, USA.
    Protostellar Condensations within the Orion Ridge1986In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 304, no 2, p. L51-L55Article in journal (Refereed)
    Abstract [en]

    Aperture synthesis observations of the CS J = 2 to 1 line and 95 GHz continuum emission from a 2 arcmin x 3 arcmin region around IRc2 in the OMC-1 molecular cloud have been obtained at 7.5 arcsec resolution with the Owens Valley Radio Observatory millimeter interferometer. These observations reveal four distinct condensations with the OMC-1 molecular ridge. The condensations lie along the edge of the bright central part of the H II region, M 42, suggesting that they may have been formed as a result of shock compression driven by the H II region. Their masses and densities, M about 50 solar masses and n about 10 to the 6th - 10 to the 7th/cu cm, suggest that the condensations will undergo further massive star formation on a short time scale (about 20,000 yr).

1 - 6 of 6
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