Massive Red Spiral Galaxies in SDSS-IV MaNGA Survey

Abstract

Massive red spiral galaxies (MRSGs) are supposed to be the possible progenitors of lenticular galaxies (S0s). We select a large sample of MRSGs ($M_*>10^{10.5}\rm M_{\odot}$) from MaNGA DR17 using the $g-r$ color vs. stellar mass diagram, along with control samples of blue spirals and S0s. Our main results are as follows: (1) After comparing the S$\rm \acute{e}$rsic index, concentration parameter, asymmetry parameter distribution, size-mass relation and $\Sigma_1$ (stellar mass surface density within the central 1 kpc)-mass relation, we find MRSGs are similar to S0s and have more compact and symmetric structures than blue spirals. MRSGs also resemble S0s in Dn4000, metallicity, Mgb/$\rm \left \langle Fe \right \rangle$ and $V/\sigma$ radial profile. (2) By using MaNGA 2D spectra data, we separate the spatial regions into inner (R < 0.8$R_{\rm e}$) and outer (0.8$R_{\rm e}$ < R < 1.5$R_{\rm e}$) regions, and detect residual star formation in the outer regions of MRSGs. (3) When we select a sub-sample of MRSGs with NUV$-r$ > 5, we find that they are completely star-formation quenched in both inner and outer regions. Compared to optically selected MRSGs, NUV$-r$ selected MRSGs appear to be more concentrated and have more massive dark matter halos. The similarities between S0s and MRSGs suggest the possible evolutionary trend between MRSGs and S0s.