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Excited OH Masers in Late-Type Stellar Objects

Published online by Cambridge University Press:  16 July 2018

A. Strack
Affiliation:
Physics Department, Western Illinois University, 1 University Circle, Macomb, IL 61455, USA.
E. D. Araya
Affiliation:
Physics Department, Western Illinois University, 1 University Circle, Macomb, IL 61455, USA.
M. E. Lebrón
Affiliation:
University of Puerto Rico at Rio Piedras, San Juan, PR 00931, USA.
R. F. Minchin
Affiliation:
Arecibo Observatory, NAIC, HC03 Box 53995, Arecibo, PR 00612, USA.
H. G. Arce
Affiliation:
Department of Astronomy, Yale University, New Haven, CT 06511, USA.
T. Ghosh
Affiliation:
Arecibo Observatory, NAIC, HC03 Box 53995, Arecibo, PR 00612, USA.
P. Hofner
Affiliation:
Physics Department, New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA. National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA.
S. Kurtz
Affiliation:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia 58090, Mexico.
L. Olmi
Affiliation:
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy.
Y. Pihlström
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA. The Department of Physics and Astronomy, The University of New Mexico, Albuquerque, NM 87131, USA.
C. J. Salter
Affiliation:
Arecibo Observatory, NAIC, HC03 Box 53995, Arecibo, PR 00612, USA.
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Abstract

The final stages of low-mass stellar evolution are characterized by significant mass loss due to stellar pulsations during the AGB phase, which lead to the development of planetary nebulae. Molecular masers of H2O, SiO, and ground state OH transitions are commonly detected in oxygen-rich late-type stars (OH/IR objects). In contrast, excited OH maser transitions are rare. We discuss our study of the carbon-rich pre-planetary nebula CRL618 (a prototypical post-AGB star). Observations conducted in May 2008 with the 305m Arecibo Telescope resulted in the first detection of a 4765MHz OH maser line in a late-type stellar object; the detection was confirmed a few months later also with Arecibo. Subsequent observations in 2015 and 2017 resulted in non-detection of the 4765MHz OH line. Our observations indicate that the 4765MHz OH maser in CRL 618 is highly variable, possibly tracing a short-lived phenomenon during the development of a pre-planetary nebula.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

References

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