The peculiar cluster HS 327 in the Large Magellanic Cloud: can OH/IR stars and carbon stars be twins?

Details The peculiar cluster HS 327 in the Large Magellanic Cloud: can OH/IR stars and carbon stars be twins? The peculiar cluster HS 327 in the Large Magellanic Cloud: can OH/IR stars and carbon stars be twins?

2001-01-08

arxiv.org/abs/astro-ph/0101107v1

Astron.Astrophys.368:239-249,2001

Astronomy and Astrophysics

Astrophysics

11 pages (better quality Figs 1b & 9 on request from jacco@ast.cam.ac.uk). Accepted for publication in Astronomy and Astrophys

Scientific paper

10.1051/0004-6361:20000529

The obscured OH/IR star IRAS05298-6957 in the LMC was recently noticed to be member of the small double cluster HS 327 that also contains a carbon star (van Loon et al., 1998, A&A 329, 169). Hence they are coeval and have (nearly) the same progenitor mass, which can only be understood if Hot Bottom Burning (HBB) has prevented IRAS05298-6957 from being a carbon star. We present extensive visual and near-IR photometric data for >10^4 stars in and around HS 327, and spectroscopic data for some of the brightest AGB stars amongst these. Colour-magnitude diagrams are used to estimate the age for the cluster and its members, and luminosities are derived for the stars for which spectra have been obtained. The age for IRAS05298-6957 and the carbon star is estimated to be about 200 Myr. This corresponds to a Main-Sequence progenitor mass of about 4.0 M_sun --- the first direct measurement of the lower mass threshold for HBB. This agrees with stellar evolution models that, however, fail to reproduce the low luminosity of the carbon star.

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