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VLA observations of H2O and OH (1612 MHz) maser emission towards OH 231.8+4.2

Published online by Cambridge University Press:  03 August 2017

Yolanda Gómez  and
Luis F. Rodríguez
Yolanda Gómez
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán, México
Luis F. Rodríguez
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán, México

Abstract

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We present Very Large Array (VLA) observations of H2O and OH (1612 MHz) maser emission toward the protoplanetary nebula OH 231.8+4.2. The H2O observations show two features at VLSR of 23.1 and 44.5 km s−1, coinciding in position within error with the SiO (v=1; J=2−1) maser position from Sánchez Contreras et al. (2000). The H2O and SiO masers are most likely tracing the position of QX Pup, the Mira near the center of OH 231.8+4.2. This position is, however, clearly offset by ∼1 from the axis of the bipolar outflow traced by the OH maser emission. These results suggest the presence of a binary system: one invisible star powering the bipolar outflow and the other, the Mira star QX Pup, associated with the H2O and SiO masers. This scenario requires that the two stars have evolved at very similar rates.

Type
Part 3. Protoplanetary Nebulae
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 348 - 351
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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