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Near-IR spectroscopy of OHIR stars in the Galactic Centre
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Astronomy Astrophysics manuscript no. SOFI c? ESO 2008
February 5, 2008
Near-IR Spectroscopy of OH/IR stars in the Galactic Centre
E. Vanhollebeke
1
, J.A.D.L. Blommaert
1
, M. Schultheis
2
, B. Aringer
3
, and A. Lanc?on
4
1
Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200B, B–3001 Leuven, Belgium
2
CNRS UMR6091, Observatoire de Besanc?on, BP1615, F-25010 Besanc?on, France
3
Institut fu?r Astronomie, Tu?rkenschanzstrasse 17, A–1180 Wien, Austria
4
Observatoire Astronomique, Rue de L’Universite 11, F–67000 Strasbourg, France
Received / Accepted
ABSTRACT
Context. Galactic Centre (GC) OH/IR stars can be, based on the expansion velocities of their circumstellar shells, divided into two groups
which are kinematically different and therefore are believed to have evolved from different stellar populations.
Aims. To study the metallicity distribution of the OH/IR stars population in the GC on basis of a theoretical relation between EW(Na), EW(Ca)
and EW(CO) and the metallicity.
Methods. For 70 OH/IR stars in the GC, we obtained near-IR spectra. The equivalent line widths of Na ?, Ca ?, 12CO(2,0) and the curvature of
the spectrum around 1.6 μm due to water absorption are determined.
Results. The near-IR spectrum of OH/IR stars is influenced by several physical processes. OH/IR stars are variable stars suffering high
mass-loss rates. The dust that is formed around the stars strongly influences the near-IR spectra and reduces the equivalent line widths of Na ?,
Ca ?. A similar effect is caused by the water content in the outer atmosphere of the OH/IR star. Because of these effects, it is not possible with
our low resolution near-infrared spectroscopy to determine the metallicities of these stars.
Key words. Stars: AGB and post-AGB – Stars: late-type – Stars: mass-loss – Galaxy: bulge – Galaxy: center – Infrared: stars
1. Introduction
The inner region of our Galaxy has been extensively searched
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