Astron. Astrophys. Suppl. Ser.
Volume 140, Number 1, November II 1999
|Page(s)||55 - 67|
|Published online||15 November 1999|
I. Luminosity calibrations
Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Avda. Diagonal 647, E–08028 Barcelona, Spain
2 Institut d'Astrophysique, CP 226, Université Libre de Bruxelles, Bd. du Triomphe, B–1050 Bruxelles, Belgium
3 GRAAL (UPRES-A 5024 CNRS), Université Montpellier II, F–34095 Montpellier Cedex 05, France
Accepted: 6 September 1999
The absolute K magnitudes and kinematic parameters of about 350 oxygen–rich Long–Period Variable stars are calibrated, by means of an up–to–date maxi mum–likelihood method, using Hipparcos parallaxes and proper motions together with radial velocities and, as additional data, periods and colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period–lumi nosity–colour relations and their two–dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower–order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so–called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal–deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period–luminosity relation from one galaxy to the other.
Key words: stars: variables: long period variables / AGB / fundamental parameters / kinematics / evolution
Appendix B is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsweb.u-strasbg.fr/Abstract.html
© European Southern Observatory (ESO), 1999