High-Resolution Near-Infrared Speckle Interferometry and Radiative Transfer Modeling of the OH/IR Star OH 26.5+0.6

Details High-Resolution Near-Infrared Speckle Interferometry and Radiative Transfer Modeling of the OH/IR Star OH 26.5+0.6 High-Resolution Near-Infrared Speckle Interferometry and Radiative Transfer Modeling of the OH/IR Star OH 26.5+0.6

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..378..289d&link_type=abstract

Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes. ASP Conference Series, Vol. 378, proceedings of the co

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present near-infrared speckle interferometry of the OH/IR star OH 26.5+0.6 in the K' band obtained with the 6-m telescope of the Special Astrophysical Observatory (SAO) in October 2003. At λ = 2.12 μm the diffraction-limited resolution of 74 mas was attained. The reconstructed visibility function shows that the stellar contribution to the total flux at λ = 2.12 μm is less than 50%, indicating a rather large optical depth of the circumstellar dust shell (CDS) surrounding this highly reddened object, in accordance with the strong silicate absorption feature seen in the spectral energy distribution (SED). Our phase-dependent modeling approach follows a strategy similar to the one recently applied successfully to interpret observations of the OH/IR star OH 104.9+2.4 (Riechers et al. 2005). From our analysis, we derived several physical parameters of the central star and the CDS as a function of pulsation phase.

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