With known distances and metallicities and with a wide range of
 age, star clusters in the Magellanic Clouds (MCs) offer a unique
 opportunity for observational studies of stellar evolution.
 Particularly interesting are asymptotic giant branch (AGB) stars,
 i.e., low to intermediate mass stars in the late stage of their
 evolution in the star clusters.

 The recent studies revealed a large discrepancy between the
 prediction of the theory and the observation.  It was found that
 the AGBs in the intermediate age clusters do not extend to the
 expected luminosity from the theory.  This "luminous AGB stars
 deficiency" might be connected to another mystery of carbon stars
 whose bolometric magnitudes are found 1 or 2 mag. fainter than
 predicted.  Among amendments proposed to reconcile theory to
 observation, the modification of the evolutionary track by mass
 loss seems most promising.  Unfortunately, however, there are
 little direct evidence of mass loss from AGB stars in the Clouds.

 In order to clarify the mass loss phenomenon and its effect on
 stellar evolution, mid-infrared observations are obviously needed.
 We propose to observe spectrophotometrically AGB-rich clusters,
 NGC 1783 and NGC 419, in the MCs using ISOCAM CVF.  These clusters
 contain both M and C type AGBs which have been studied in the
 visual and near-infrared.  Our observations will show the spectral
 characteristics of both types of AGBs in the mid-infrared and
 enable us to estimate the mass loss rates of AGBs with known ages.
 Furthermore, we can establish a relationship between infrared
 colours to stellar types, which will help us to interpret the
 infrared photometric data which will be taken by our ISAS Time
 Proposal, TTANABE_REDSTAR3, or by others.