A&A 401, 1119-1129 (2003)
DOI: 10.1051/0004-6361:20030191

An analysis of the optical spectra of the post-asymptotic giant branch stars LSIV -12 111 and HD 341617

R. S. I. Ryans¹, P. L. Dufton¹, C. J. Mooney¹, W. R. J. Rolleston¹, F. P Keenan¹, I. Hubeny^{2, 3} and T. Lanz<sup>2, 4

1</sup>  The Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast BT7 1NN, Northern Ireland
²  Laboratory for Astronomy and Solar Physics, Code 681, Goddard Space Flight Centre, Greenbelt, MD 20771, USA
³  National Optical Astronomy Observatories, Tucson, AZ 85726, USA
⁴  Department of Astronomy, University of Maryland, College Park, MD 20742, USA

(Received 23 August 2002 / Accepted 4 February 2003)

Abstract
High spectral resolution and signal-to-noise observations of the absorption and emission line spectra in two post-asymptotic-giant-branch (PAGB) stellar candidates, LSIV -12 111 and HD 314617 are discussed. The absorption line spectra have been analysed using non-LTE model atmosphere techniques to determine stellar atmospheric parameters and chemical compositions, both in absolute terms and relative to a standard star, HD 13841. The atmospheric parameters differ from previous estimates based on LTE model atmospheres, probably due to non-LTE effects. In turn these imply stellar masses that are generally larger than have been previously estimated. Both PAGB candidates have relative uniform underabundances of metals with mean values of -0.35 dex for LSIV -12 111 and -0.50 dex for HD 314617.

Furthermore, their abundance patterns are remarkably similar to that observed for optically bright, F-type PAGBs. From the emission spectra, the plasma parameters and angular size of the circumstellar material are constrained, and these are consistent with previous estimates and with a PAGB evolutionary stage.

Key words: stars: abundances -- stars: supergiants -- stars: early-type -- stars: fundamental parameters

Offprint request: R. Ryans, R.Ryans@qub.ac.uk

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