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Context: Clumpy disk galaxies in the distant universe, at redshift of z>1,have been observed to host several giant clumps in their disks. They arethought to correspond to early formative stages of disk galaxies. On the otherhand, halo objects, such as old globular clusters and halo stars, are likely toconsist of the oldest stars in a galaxy (age>10 Gyr), therefore the clumpy diskformation can be presumed to take place in a pre-existing halo system. Aims:Giant clumps are orbiting in the same direction in a premature disk and somassive that they may be expected to interact gravitationally with halo objectsand exercise influence on kinematic state of the halo. Accordingly, Iscrutinize the possibility that the clumps leave a kinematic imprint of theclumpy disk formation on a halo system. Methods: I perform a restricted N-bodycalculation with a toy-model to study the kinematic influence on a halo byorbital motions of clumps, examine dependence of the results on masses(mass-loss), number and orbital radii of the clumps. Results: I will show thathalo objects can catch clump motions and acquire disky rotation in a dynamicalfriction time-scale of the clumps, ~0.5 Gyr. The influence of clumps is limitedwithin a region around the disk, the halo system shows vertical gradients ofnet rotation velocity and orbital eccentricity. The significance of thekinematic influence strongly depends on the clump masses, the lower limit ofpostulated clump mass would be 5x10^8 solar masses. The result depends also onwhether the clumps are subjected to rapid mass-loss or not, which is an openquestion under debate in recent studies. The existence of such massive clumpsis not unrealistic, I therefore suggest that there could remain the imprints ofpast clumpy disk formation in current galactic halos.

Kinematic imprint of clumpy disk formation on halo objects