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Issue A&A Volume 438, Number 2, August I 2005 Page(s) 521 - 532 Section Extragalactic astronomy DOI 10.1051/0004-6361:20041904

A&A 438, 521-532 (2005)
DOI: 10.1051/0004-6361:20041904

Pulsation properties of C stars in the Small Magellanic Cloud

G. Raimondo^{1, 2}, M.-R. L. Cioni¹, M. Rejkuba¹ and D. R. Silva<sup>1

1</sup>  European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
    e-mail: [graimond;mcioni;mrejkuba;dsilva]@eso.org
²  INAF - Osservatorio Astronomico di Teramo, via M. Maggini, 64100 Teramo, Italy
    e-mail: raimondo@te.astro.it

(Received 26 August 2004 / Accepted 18 March 2005 )

Abstract
A sample of carbon-rich stars (C-stars) in the Small Magellanic Cloud (SMC) was selected from the combined 2MASS and DENIS catalogues on the basis of their  colour. This sample was extended to include confirmed C-stars from the Rebeirot et al. (1993) spectroscopic atlas. In this combined sample (N = 1149), a smaller number (N = 1079) were found to have MACHO observations. For this sub-sample, light curves were determined and 919 stars were found to have high quality light-curves with amplitudes of at least 0.05 mag. Of these stars, only 4% have a well-defined single period - most of these have multiple well-defined periods, while 15% have highly irregular light-curves. The distribution of the logarithm of the period versus magnitude, colour, period ratio (if applicable), and amplitude was analyzed and compared with previous works. Variable C-stars are distributed in three sequences: B, C, and D from Wood et al. (1999), and do not populate sequences with periods shorter than . Stellar ages and masses were estimated using stellar evolutionary models.

Key words: stars: AGB and post-AGB -- stars: variables: general -- Magellanic Clouds

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