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 ($M_{\ast }>10^{10.5}{\mathrm{M}}_{\odot }$) 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$\acute{\mathrm{e}}$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/$⟨\mathrm{Fe}⟩$ and $V/\sigma$ radial profile. (2) By using MaNGA 2D spectra data, we separate the spatial regions into inner (R < 0.8$R_{\mathrm{e}}$) and outer (0.8$R_{\mathrm{e}}$ < R < 1.5$R_{\mathrm{e}}$) 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.

accepted for publication in MNRAS; 17 pages, 16 figures, 1 table

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