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We analyse the clump population of the spiral galaxy Sp 1149 at redshift 1.5.Located behind the galaxy cluster MACS J1149.5+2223, Sp 1149 has beensignificantly magnified allowing us to study the galaxy on physical scales downto ~100 pc. We have used the publicly available multi-band imaging dataset(CLASH) to reconstruct the spectral energy distributions (SEDs) of the clumpsin Sp 1149, and derive, by means of stellar evolutionary models, their physicalproperties. We found that 40% of the clumps observed in Sp 1149 are older than30 Myr and can be as old as 300 Myr. These are also the more massive (luminous)clumps in the galaxy. Among the complexes in the local reference sample, thestar-forming knots in luminous blue compact galaxies could be consideredprogenitor analogs of these long-lived clumps. The remaining 60% of clumps havecolors comparable to local cluster complexes, suggesting a similar young age.We observe that the Sp 1149 clumps follow the M ~ R^2 relation similar to localcluster complexes, suggesting similar formation mechanisms although they mayhave different initial conditions (e.g. higher gas surface densities). Wesuggest that the galaxy is experiencing a slow decline in star formation rateand a likely transitional phase toward a more quiescent star-formation mode.The older clumps have survived between 6 and 20 dynamical times and are alllocated at projected distances smaller than 4 kpc from the centre. Theircurrent location suggests migration toward the centre and the possibility to bethe building blocks of the bulge. On the other hand, the dynamical timescale ofthe younger clumps are significantly shorter, meaning that they are quite closeto their birthplace. We show that the clumps of Sp 1149 may account for theexpected metal-rich globular cluster population usually associated with thebulge and thick disk components of local spirals.

High resolution study of the cluster complexes in a lensed spiral at redshift ~1.5; constraints on the bulge formation and disk evolution