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ALMA spectrum of the extreme OH/IR star OH 26.5+0.6

Published online by Cambridge University Press:  30 December 2019

K. Justtanont
Affiliation:
Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden
S. Muller
Affiliation:
Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden
M. J. Barlow
Affiliation:
Univ. College London, Dept. of Physics & Astronomy, Gower Street, London, UK
D. Engels
Affiliation:
Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany
D. A. García-Hernández
Affiliation:
Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain Departamento de Astrofísica, Univ. de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain
M. A. T. Groenewegen
Affiliation:
Koninklijke Sterrenwacht van België, Ringlaan 3, 1180 Brussels, Belgium
M. Matsuura
Affiliation:
School of Physics & Astronomy, Cardiff University, The Parade, Cardiff, UK
H. Olofsson
Affiliation:
Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden
D. Teyssier
Affiliation:
Telespazio Vega UK Ltd for ESA/ESAC, Camino bajo del Castillo, s/n, Urbanizacion Villafranca del Castillo, Villanueva de la Cañada, E-28692 Madrid, Spain
I. Marti-Vidal
Affiliation:
Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden
T. Khouri
Affiliation:
Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden
M. Van de Sande
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
W. Homan
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
T. Danilovich
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
A. de Koter
Affiliation:
Sterrenkundig Instituut “Anton Pannekoek”, Science Park 904, 1098 XH Amsterdam, The Netherlands
L. Decin
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
L. B. F. M. Waters
Affiliation:
Sterrenkundig Instituut “Anton Pannekoek”, Science Park 904, 1098 XH Amsterdam, The Netherlands SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
R. Stancliffe
Affiliation:
Argelander-Inst. für Astronomie, Univ. of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
W. Vlemmings
Affiliation:
Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden
P. Royer
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
F. Kerschbaum
Affiliation:
University of Vienna, Dept. of Astrophysics, Türkenschanzstrasse 17, 1180 Wien, Austria
C. Paladini
Affiliation:
European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
J. Blommaert
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
R. de Nutte
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium

Abstract

We present ALMA band 7 data of the extreme OH/IR star, OH 26.5+0.6. In addition to lines of CO and its isotopologues, the circumstellar envelope also exhibits a number of emission lines due to metal-containing molecules, e.g., NaCl and KCl. A lack of C18O is expected, but a non-detection of C17O is puzzling given the strengths of H217O in Herschel spectra of the star. However, a line associated with Si17O is detected. We also report a tentative detection of a gas-phase emission line of MgS. The ALMA spectrum of this object reveals intriguing features which may be used to investigate chemical processes and dust formation during a high mass-loss phase.

Type
Contributed Papers
Copyright
© International Astronomical Union 2019 

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References

Garca-Hernández, D. A., Zamora, O., Yagüe, A., et al. 2013, A&A, 555, L3 Google Scholar
Justtanont, K., Muller, S., Barlow, M. J., et al. 2018, A&A, submittedGoogle Scholar
Justtanont, K., Teyssier, D., Barlow, M. J., et al. 2013, A&A, 556, A101 Google Scholar
Karakas, A. I. & Lattanzio, J. C. 2014, PASA, 31, 30 CrossRefGoogle Scholar

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ALMA spectrum of the extreme OH/IR star OH 26.5+0.6
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