Volume 477, Number 1, January I 2008
|Page(s)||213 - 221|
|Section||Stellar structure and evolution|
|Published online||06 November 2007|
Institut d'Estudis Espacials de Catalunya, c/ Gran Capità 2–4, 08034 Barcelona, Spain e-mail: firstname.lastname@example.org
2 Institut de Ciències de l'Espai, CSIC, Facultat de Ciències, Campus UAB, 08193 Bellaterra, Spain
3 Departament de Física Aplicada, Escola Politècnica Superior de Castelldefels, Universitat Politècnica de Catalunya, Avda. del Canal Olímpic s/n, 08860 Castelldefels, Spain
4 McDonald Observatory and Department of Astronomy, University of Texas, Austin, TX 78712, USA
5 Vera Rubin Fellow, Department of Terrestrial Magnetism, Carnegie Institution of Washington, DC 20015, USA
Accepted: 1 October 2007
Context.The initial-final mass relationship of white dwarfs, which is poorly constrained, is of paramount importance for different aspects of modern astrophysics. From an observational perspective, most of the studies up to now have been done using white dwarfs in open clusters.
Aims.In order to improve the initial-final mass relationship, we explore the possibility of deriving a semi-empirical relation studying white dwarfs in common proper motion pairs. If these systems are comprised of a white dwarf and a FGK star, the total age and the metallicity of the progenitor of the white dwarf can be inferred from the detailed analysis of the companion.
Methods.We have performed an exhaustive search for common proper motion pairs containing a DA white dwarf and a FGK star using the available literature and crossing the SIMBAD database with the Villanova White Dwarf Catalog. We have acquired long-slit spectra of the white dwarf members of the selected common proper motion pairs, as well as high resolution spectra of their companions. From these observations, a full analysis of the two members of each common proper motion pair leads to the initial and final masses of the white dwarfs.
Results.These observations have allowed us to provide updated information for the white dwarfs, since some of them were misclassified. In the case of the DA white dwarfs, their atmospheric parameters, masses, and cooling times have been derived using appropriate white dwarf models and cooling sequences. From a detailed analysis of the FGK star spectra we have inferred the metallicity. Then, using either isochrones or X-ray luminosities we have obtained the main-sequence lifetime of the progenitors, and subsequently their initial masses.
Conclusions.This work is the first one using common proper motion pairs to improve the initial-final mass relationship, and has also allowed us to cover the poorly explored low-mass domain. As in the case of studies based on white dwarfs in open clusters, the distribution of the semi-empirical data presents a large scatter, which is higher than the expected uncertainties in the derived values. This suggests that the initial-final mass relationship may not be a single-valued function.
Key words: stars: evolution / stars: white dwarfs / open clusters and associations: individual: common proper motion pairs / binaries: visual
Based on observations obtained at: Calar Alto Observatory, Almería, Spain, el Roque de los Muchachos, Canary Islands, Spain, McDonald Observatory, Texas, USA, and Las Campanas Observatory, Chile.
© ESO, 2007
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