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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5933

Title: Comparative modelling of the spectra of cool giants
Authors: Lebzelter, T
Heiter, U
Abia, C
Eriksson, K
Ireland, M
Neilson, H
Nowotny, W
Maldonado, J
Merle, T
Peterson, R
Plez, B
Short, C. I
Wahlgren, G. M
Worley, C
Aringer, B
Bladh, S
de Laverny, P
Goswami, A
Mora, A
Norris, R. P
Recio-Blanco, A
Scholz, M
Thevenin, F
Tsuji, T
Kordopatis, G
Montesinos, B
Wing, R. F
Keywords: Stars
Atmospheres / stars
Late-type / stars
Abundances / stars
Fundamental parameters
Issue Date: Nov-2012
Publisher: EDP Sciences
Citation: Astronomy & Astrophysics, Vol. 547, A108
Abstract: Context. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. Various model codes and strategies for the analysis of stellar spectra are available today. Aims. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. The focus is set on high-resolution spectroscopy of cool giant stars. Methods. Spectra representing four cool giant stars were made available to various groups and individuals working in the area of spectral synthesis, asking them to derive stellar parameters from the data provided. The results were discussed at a workshop in Vienna in 2010. Most of the major codes currently used in the astronomical community for analyses of stellar spectra were included in this experiment. Results. We present the results from the different groups, as well as an additional experiment comparing the synthetic spectra produced by various codes for a given set of stellar parameters. Similarities and differences of the results are discussed. Conclusions. Several valid approaches to analyze a given spectrum of a star result in quite a wide range of solutions. The main causes for the differences in parameters derived by different groups seem to lie in the physical input data and in the details of the analysis method. This clearly shows how far from a definitive abundance analysis we still are.
URI: http://hdl.handle.net/2248/5933
ISSN: 1432-0746
Alternative Location: http://dx.doi.org/10.1051/0004-6361/201219142
http://arxiv.org/abs/1209.2656
Copyright: © ESO
Appears in Collections:IIAP Publications

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