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Bulges in spiral galaxies have been supposed to be classified into two types:classical bulges or pseudobulges. Classical bulges are thought to form bygalactic merger with bursty star formation, whereas pseudobulges are suggestedto form by secular evolution. Noguchi (1998, 1999) suggested another bulgeformation scenario, `clump-origin bulge'. He demonstrated using a numericalsimulation that a galactic disc forms clumpy structures in the early stage ofdisc formation, then the clumps merge into a single bulge at the centre. Iperform a high-resolution N-body/SPH simulation for the formation of theclump-origin bulge in an isolated galaxy model. I find that the clump-originbulge resembles pseudobulges in dynamical properties, but this bulge consistsof old and metal-rich stars. These natures, old metal-rich population butpseudobulge-like structures, mean that the clump-origin bulge can not be simplyclassified into classical bulges nor pseudobulges. From these results, Idiscuss similarities of the clump-origin bulge to the Milky Way bulge.

Natures of clump-origin bulges: similarities to the Milky Way bulge