Contents of: VI/111/./abstract/JBLOMMAE_AGB_SMC.abs

The following document lists the file abstract/JBLOMMAE_AGB_SMC.abs from catalogue VI/111.
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We propose to study the final stages of stellar evolution of Asymptotic
Giant Branch (AGB) stars in the Small Magellanic Cloud.
Based on the IRAS Faint Source Catalog we have selected 29 objects with
IRAS 12 and 25 micron colors indicative of red AGB stars. Ground-based
near-infrared (NIR) JHK images were obtained of these fields. In SOC/PS
guaranteed time (JBLOMMAE, SMC_AGB) CAM LW2 (6.75 micron) and LW10 (11.4
micron) raster-images were made for 16 of these objects. This allowed a
direct connection between our NIR work and the IRAS 12 micron data.
In every of the 16 fields a red source (F12 > F6.8) was seen in the middle
of the CAM images with a 12 micron flux comparable to the IRAS flux,
corresponding to the NIR position and therefore confirming the accuracy of
these coordinates. Here we propose a  follow-up study to obtain the spectral
energy distribution (SED) between 3.6 and 60 microns of all 29 AGB stars
detected by IRAS. The SEDs will be analyzed using a radiative transfer model
which will provide accurate determinations of the luminosities and mass loss
rates of the objects. The results will be compared to the luminosities and
mass loss rates of AGB stars in the Large Magellanic Cloud, which are observed
in several programs in the guaranteed and open time involving most of the
investigators on this proposal.
Combining the data on the SMC, LMC and existing data on the Galaxy will
answer the open question of the metallicity dependence of mass loss in
late-type stars. This in turn is important in the ejection of matter by
AGB stars to the interstellar medium over the age of the Galaxy.
ISO observations are essential to this project as the proposed observations
include observations at 25 and 60 micron which cannot be performed from
the ground. As the stars are expected to be Mira variables it is essential
to have simultaneous observations over the broad range in wavelengths.
Only ISO is giving this possibility and also the sensitivity that is needed.



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