SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 327, 656-661 (1997)

Next Section Table of Contents

Oxygen-rich Mira variables: near-infrared luminosity calibrations *

Populations and period-luminosity relations

R. Alvarez 1, M-O. Mennessier 1, D. Barthès 1, X. Luri 2, 3 and J.A. Mattei 4

1 GRAAL, Université Montpellier II, UPRESA 5024/CNRS, F-34095 Montpellier Cedex 05, France
2 Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Avda. Diagonal 647, E-08028 Barcelona, Spain
3 DASGAL, Observatoire de Paris-Meudon, F-92195 Meudon Cedex, France
4 AAVSO, 25 Birch Street, Cambridge, Massachusetts 02138-1205, USA

Received 30 April 1997 / Accepted 10 July 1997

Abstract

HIPPARCOS astrometric and kinematical data of oxygen-rich Mira variables are used to calibrate absolute near-infrared magnitudes and kinematic parameters. Two sets of near-infrared magnitudes compiled from different authors are used: broad-band K and narrow-band photometric measurements at 1.04 [FORMULA] m (104 filter). Three distinct classes of stars with different kinematics and scale height have been identified. The two most significant groups present characteristics close to the ones usually assigned to extended/thick disk-halo population and old disk population respectively, and thus they might differ by their metallicity abundance. They exhibit different period distributions, as expected if these two groups actually correspond to populations of distinct initial masses, ages and metallicities. Two parallel period-luminosity relations are found in K as well as in 104, one for each significant population. The shift between these relations is interpreted as the consequence of the effects of metallicity abundance on the luminosity.

Key words: stars: distances – stars: fundamental parameters – stars: AGB, post-AGB – Galaxy: stellar content

* Based on data from the HIPPARCOS astrometry satellite

Send offprint requests to: alvarez@graal.univ-montp2.fr

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 1997

Online publication: April 6, 1998
helpdesk.link@springer.de