EDP Sciences
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Volume 372, Number 1, June II 2001
Page(s) 85 - 94
Section Stellar clusters and associations
DOI http://dx.doi.org/10.1051/0004-6361:20010361

A&A 372, 85-94 (2001)
DOI: 10.1051/0004-6361:20010361

Evolution of the dust mass loss with luminosity along the giant branch of the globular cluster 47 Tucanae

A. Ramdani1, 2 and A. Jorissen2

1  Département de Physique, Université d'Oujda, Maroc
2  Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, 1050 Bruxelles, Belgium

(Received 4 December 2000 / Accepted 7 March 2001 )

The present paper investigates the properties of the dust mass loss in stars populating the giant branch of the globular cluster 47 Tuc, by combining ISOCAM and DENIS data. Raster maps of 5 fields covering areas ranging from $4\times4$ to $15\times15$ arcmin2 at different distances from the center of the cluster have been obtained with ISOCAM at 11.5 $\mu$m (LW10 filter). The covered fields include most of the red variables known in this cluster. A detection threshold of about 0.2 mJy is achieved, allowing us to detect giant stars at 11.5 $\mu$m all the way down to the horizontal branch. No dust-enshrouded asymptotic giant branch stars have been found in the observed fields, contrary to the situation encountered in LMC/SMC globular clusters with larger turnoff masses. The color index [12]-[2] (based on the ISO 11.5 $\mu$m flux and on the DENIS $K_{\rm s}$ magnitude) is used as a diagnostic of dust emission (and hence dust mass loss). Its evolution with luminosity along the giant branch reveals that dust mass loss is only present in V3 (the only cluster Mira variable observed in the present study) and in V18, a star presenting intermittent variability. This conclusion confirms the importance of stellar pulsations in the dust formation and ensuing mass loss.

Key words: globular clusters: 47 Tuc -- stars: AGB and post-AGB -- circumstellar matter -- stars: mass loss -- infrared: stars

Offprint request: A. Jorissen, ajorisse@astro.ulb.ac.be

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