| dc.description.abstract | We investigate the properties of 16 star-forming early-type galaxies (SFETGs) with
the integral field spectroscopy (IFS) from SDSS MaNGA. The ETGs are selected from
the morphological parameters provided by Galaxy Zoo 2 and then classified into SFETGs and Non-SFETGs (NSFETGs) through the BPT maps. The differences of the galaxy properties between the SFETGs and NSFETGs are that the SFETGs are less massive, showing bluer color, and, of course, more star-forming, while the NSFETGs are massive, red, and passive. The origins of the gas fueling the star formation may be external because of the existence of the kinematically misaligned gas and stars in some SFETGs. We further classify the SFETGs into round, shifted, double-peaked, and multiple-peaked using the morphology derived from the maps of the equivalent width (EW) of the Hα emission line. To express the specific angular momentum of the gas of the galaxies, we employ the λ_R parameter. These four types of morphology correspond to different levels of λ_R of gas; the round and the shifted SFETGs are at the lower levels, whereas the double- and multiple-peaked ones are at the higher ones. Based on the relation between λ_R and local Hα EW, the loss of the angular momentum of gas may enhance the star formation. To verify the well-known sSFR-Dn4000 relation on the local scale, we adopt the Hα EW to be the local sSFR. We find that the anti-correlation works on the local scale as well. The gradients of the stellar age profiles of the round, shifted, double-peaked, and multiple-peaked SFETGs are positive, mixed, negative-positive, and negative, respectively, which reflect the distribution of gas while forming stars. | en_US |