VLA observations of the OH and H2O masers in the young star cluster NGC 2071 IR

  • G. Sandell
  • L. A. Nyman
  • A. Haschick
  • A. Winnberg
Part V: Stellar Content of Nearby Molecular Clouds
Part of the Lecture Notes in Physics book series (LNP, volume 237)


We have mapped the maser emission in OH 205.1-14.1 (NGC 2071 IR), which is associated with a prominent bipolar outflow, at 1.6 and 22 GHz with the VLA in the A configuration. Our H2O data are only preliminary, since we have checked only four velocity channels, but at these velocities the H2O emission is resolved into at least three different point sources, each of which coincide with a compact HII region. At 1720 MHz we detected 100% polarized LC and RC maser emission from an unresolved point source. Since the LC and RC emission coincide in position, we interpret the line difference as due to Zeeman splitting, corresponding to a magnetic field of ~14mG. The 1720 MHz maser has no clear radio or IR counterpart, but in the 6cm VLA continuum map, we see some faint emission, which could be due to ionized gas within the molecular flow, probably driven by IRS1, the strongest radio and H2O source. The 6cm emission from IRSI is extended and may outline a disk perpendicular to the flow. The 1667 MHz LC OH line was too weak to be detected.


Zeeman Splitting Swedish Natural Science Research Council Strong Radio Faint Emission Haystack Observatory 
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Copyright information

© Springer-Verlag 1985

Authors and Affiliations

  • G. Sandell
    • 1
  • L. A. Nyman
    • 1
    • 2
  • A. Haschick
    • 1
    • 3
  • A. Winnberg
    • 1
  1. 1.Observatory and Astrophys. Lab.Univ. of HelsinkiHelsinkiFinland
  2. 2.Onsala Space ObservatoryOnsalaSweden
  3. 3.Haystack Observatory and Harward-Smithsonian Center for AstrophysicsUSA

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