Bulge Formation from Super Star Clusters in a Responding Cuspy Dark Matter Halo

We simulate the bulge formation in very late-type dwarf galaxies fromcircumnuclear super star clusters (SSCs) moving in a responding cuspy darkmatter halo (DMH). The simulations show that (1) the response of DMH to sinkingof SSCs is detectable only in the region interior to about 200 pc. The meanlogarithmic slope of the responding DM density profile over that area displaystwo different phases: the very early descent followed by ascent tillapproaching to 1.2 at the age of 2 Gyrs. (2) the detectable feedbacks of theDMH response on the bulge formation turned out to be very small, in the sensethat the formed bulges and their paired nuclear cusps in the fixed and theresponding DMH are basically the same, both are consistent with $HST$observations. (3) the yielded mass correlation of bulges to their nuclear(stellar) cusps and the time evolution of cusps' mass are accordance withrecent findings on relevant relations. In combination with the consistenteffective radii of nuclear cusps with observed quantities of nuclear clusters,we believe that the bulge formation scenario that we proposed could be a verypromising mechanism to form nuclear clusters.Comment: 27 pages, 11 figures, accepted for publication in Ap