Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared

Henry C. Woodruff; Maren Eberhardt; Thomas M. Driebe; Karl-Heinz Hofmann; Keiichi Ohnaka; Andrea Richichi; Dieter Schertl; Markus Schoeller; Michael Scholz; Gerd P. Weigelt; Markus Wittkowski; Peter R. Wood

doi:10.1117/12.551245

20 October 2004 Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared

Henry C. Woodruff, Maren Eberhardt, Thomas M. Driebe, Karl-Heinz Hofmann, Keiichi Ohnaka, Andrea Richichi, Dieter Schertl, Markus Schoeller, Michael Scholz, Gerd P. Weigelt, Markus Wittkowski, Peter R. Wood

Author Affiliations +

Proceedings Volume 5491, New Frontiers in Stellar Interferometry; (2004) https://doi.org/10.1117/12.551245
Event: SPIE Astronomical Telescopes + Instrumentation, 2004, Glasgow, United Kingdom

Abstract

We present K-band commissioning observations of the Mira star prototype o Cet obtained at the ESO Very Large Telescope Interferometer (VLTI) with the VINCI instrument and two siderostats. The observations were carried out between 2001 October and December, in 2002 January and December, and in 2003 January. Rosseland angular radii are derived from the measured visibilities by fitting theoretical visibility functions obtained from center-to-limb intensity variations (CLVs) of Mira star models. Using the derived Rosseland angular radii and the spectral energy distributions (SEDs) reconstructed from available photometric and spectrophotometric data, we find effective temperatures ranging from T_eff=3192 +/- 200 K at phase 0.13 to 2918 +/- 183 K at phase 0.26. Comparison of these Rosseland radii, effective temperatures, and the shape of the observed visibility functions with model predictions suggests that o Cet is a fundamental mode pulsator. Furthermore, we investigated the variation of visibility function and diameter with phase. The Rosseland angular diameter of o Cet increased from 28.9 +/- 0.3 mas (corresponding to a Rosseland radius of 332 +/- 38 R_sun for a distance of D=107 +/- 12 pc) at phase 0.13 to 34.9 +/- 0.4 mas (402 +/- 46 R_sun) at phase 0.4. The observational error of the Rosseland linear radius almost entirely results from the error of the parallax, since the error of the angular diameter is only approximately 1%.

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Henry C. Woodruff, Maren Eberhardt, Thomas M. Driebe, Karl-Heinz Hofmann, Keiichi Ohnaka, Andrea Richichi, Dieter Schertl, Markus Schoeller, Michael Scholz, Gerd P. Weigelt, Markus Wittkowski, and Peter R. Wood "Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared", Proc. SPIE 5491, New Frontiers in Stellar Interferometry, (20 October 2004); https://doi.org/10.1117/12.551245

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KEYWORDS

Visibility

Stars

Calibration

Interferometry

Atmospheric modeling

K band

Data modeling

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