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The origin of spin of low-mass supermassive black hole (SMBH) is still apuzzle at present. We here report a study on the host galaxies of a sample ofradio-selected nearby ($z<0.05$) Seyfert 2 galaxies with a BH mass of $10^{6-7}M_\odot$. By modeling the SDSS $r$-band images of these galaxies through a2-dimensional bulge+disk decomposition, we identify a new dependence of SMBH'sradio power on host bulge surface brightness profile, in which more powerfulradio emission comes from a SMBH associated with a more disk-like bulge. Thisresult means low-mass and high-mass SMBHs are spun up by two entirely differentmodes that correspond to two different evolutionary paths. A low-mass SMBH isspun up by a gas accretion with significant disk-like rotational dynamics ofthe host galaxy in the secular evolution, while a high-mass one by a BH-BHmerger in the merger evolution.

Powerful Radio Emission From Low-mass Supermassive Black Holes Favors Disk-like Bulges