There is strong evidence of interstellar matter in the central regions
 of Galactic globular clusters (GGCs) due to mass loss processes of
 Population II stars during the post MS stages of the stellar evolution.
 Dust should be present in the most massive and concentrated clusters:
 IR excesses around luminous giants and long period variables and
 scattered polarized light have been detected in their central regions.
 Recent 10 mum ground based imaging obtained by the proposers in a
 central field of Omega Centauri shows the presence of both compact and
 extended emission. Besides, some clusters have an IRAS source in their
 core and the 12-25 mum color temperature (100<= T <=300) indicates the
 possible presence of a warm dust.
 ISO offers a unique opportunity to investigate the physical and
 chemical properties of this intracluster matter. Its photometric and
 polarimetric capabilities, with relatively large spatial resolution
 and field coverage and with very low thermal background in the 10 and
 20 mum windows, allow one to make a deep survey of the distribution
 and chemical composition of the dust in the central region of GGCs.
 The resulting database would be valuable for ground-based observations
 with 8m class telescopes at higher spatial resolution but lower
 sensitivity. It would have at least 2 fundamental astrophysical
 implications:
 1) studying the physics of mass loss in Pop II stellar systems of
 well known age and metallicity.
 This part of the program would be complementary to that one on field
 AGB stars for which ISO guaranteed time has already been scheduled;
 2) studying the circumstellar medium inside a closed stellar system,
 its chemical evolution and dynamical interaction with the Galaxy.