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Distance and kinematics of IRAS 19134+2131 revealed by H2O maser observations

Published online by Cambridge University Press:  01 October 2007

H. Imai
Affiliation:
Department of Physics, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065, Japan, email: hiroimai@sci.kagoshima-u.ac.jp
R. Sahai
Affiliation:
Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA, email: raghvendra.sahai@jpl.nasa.gov
M. Morris
Affiliation:
Department of Physics and Astronomy, University of California, Los Angeles, CA 90095–1562, USA, email: morris@astro.ucla.edu
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Abstract

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Using the VLBA, we have observed H2O maser emission in the pre-planetary nebula, IRAS 19134+2131 (I1913), in which the H2O maser spectrum has two groups of emission features separated in radial velocity by ~100 km s−1. The morphology and 3-D kinematics indicate the existence of a fast collimated flow with a dynamical age of only ~40 years. Such a “water fountain” source is a signature of the recent operation of a stellar jet, that may be responsible for the final shape of the planetary nebula into which I1913 is expected to evolve. We have also estimated the distance to I1913 (~8 kpc) on the basis of an annual parallax and the kinematics of IRAS 19134+2131 in our Galaxy. I1913 may be a component in the “thick disk” or the Galactic “warp”, whose kinematics is different from that of the Galactic “thin” disk. These results are reported in Imai, Sahai & Morris (2007).

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Imai, H., Sahai, R., & Morris, M. 2007, ApJ 669, 424CrossRefGoogle Scholar