Towards an Understanding of the Massive Red Spiral Galaxy Formation
  To understand the formation and quenching processes of local massive red
spiral galaxies with $M_{\ast} > 10^{10.5}M_{\odot}$, we perform a statistical
analysis of their spectroscopic and structural properties, and compare them
with elliptical and blue spiral galaxies of similar mass. The sample was
selected from the stellar mass catalog of galaxies in SDSS DR7, according to
their locations on the u-r color-stellar mass diagram. We find that red spirals
harbor compact cores with high stellar mass surface densities measured by
$\Sigma_1$ and they are bulge-dominated. Particularly, the red spirals,
especially their bulges follow the $\Sigma_1$-$M_{\ast}$ ridgeline for quenched
galaxies. Furthermore, the red spirals show similarly large central
D$_n(4000)$, high [Mg/Fe] and dark matter halo mass to ellipticals. These
results suggest that the bulges of red spirals formed within a short timescale
before redshift ~ 1-2 and were quenched via a fast mode, similar to
ellipticals. Careful examinations of the optical morphologies reveal that ~70%
of red spirals show strong bars, rings/shells and even merging features, which
suggests that interactions or mergers might have played an important role in
the formation of red spirals. In contrast, most of the massive blue spirals
have completely different spectral and structural properties from red spirals.
However, the blue spirals with high $\Sigma_1$ ($\Sigma_1 > 10^{9.5} M_\odot \,
{\rm kpc}^{-2}$) show similar structural and morphological properties, as well
as similar halo mass and HI mass to red spirals. We discuss rejuvenation from
red to blue as a possible explanation for these high $\Sigma_1$ blue spirals.
