AGB stars as tracers of metallicity and mean age across M 33^*

¹ Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
² SUPA, School of Physics, University of Edinburgh, IfA, Blackford Hill, Edinburgh EH9 3HJ, UK e-mail: M.Cioni@herts.ac.uk
³ Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
⁴ Deptartment of Physics & Astronomy, University of Victoria, PO Box 3055, STN CSC, Victoria, BC, V8W 3P6, Canada
⁵ European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
⁶ Department of Physics, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK
⁷ Observatoire de Strasbourg, 11 rue de l'Université, 67000 Strasbourg, France
⁸ Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia
⁹ Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK

Received: 8 January 2008
Accepted: 5 May 2008

Abstract

Context. Wide-field near-infrared observations covering an area of centred on M 33 were obtained using WFCAM at UKIRT. These data show a large population of intermediate-age asymptotic giant branch (AGB) stars.

Aims. We have used both C-type and M-type AGB stars to determine spatial variations in metallicity and mean age across the galaxy.

Methods. We distinguished between C-type and M-type AGB stars from their location in the colour-magnitude diagram (, K_s). The distribution of these stars is supported by a cross-identification between our sample and a catalogue of optically confirmed, long-period variable stars, as well as with the list of sources detected by Spitzer in the mid-infrared. We calculated the C/M ratio and the orientation of the galaxy in the sky, and compared the K_s magnitude distribution with theoretical distributions spanning a range of metallicities and star formation rates (SFRs).

Results. The C/M ratio surface map confirms a metallicity gradient in the galaxy corresponding to a spread in  dex with substructures in the inner and outer galaxy. Magnitude and colour variations suggest orientation and extinction effects on the galaxy disc. Maps showing the distribution of mean age and metallicity obtained from the K_s method suggest that: the outer galaxy disc/halo is metal poorer than the nuclear region and metal-rich clumps in the inner galaxy change location with time. The average outer ring and nuclear stellar population is ~6 Gyr old while central regions are a few Gyr younger.