Properties of cluster red-sequence spiral galaxies

We identify a sample of 324 red and 273 blue face-on spiral galaxies selected from 115 low-redshift (0.014 < z < 0.18) galaxy clusters imaged with CFHT+MegaCam in u- and r-band, KPNO 0.9-meter 2TKA and MOSAIC 8K camera in B and Rc, and images and catalogs extracted from the WINGS survey. Multi-wavelength photometry and spectroscopy were obtained by cross-matching sources with SDSS, GALEX, and WISE datasets. Primary findings indicate that up to 45% of optically red spiral galaxies exhibit significant dust content compared to blue spiral galaxies, as determined by infrared observations. This dust obscuration can conceal ongoing star formation, which may result in the misclassification of red spirals as passively evolving systems. Conversely, approximately half of the red spirals lack substantial dust abundance and appear optically red due to passive evolutionary processes. Support for the passive nature of these red spirals is provided by SDSS emission line data based on the Dn(4000) spectral index, EW(H-alpha), EW(H-delta), and [O III] 5007 A luminosity, and on a comparison of the star formation rate and the specific star formation rate with cluster blue spirals. Red spirals are an important link in the evolution of galaxies in the high-density cluster environment and play a key role in determining the physical mechanisms that are responsible for transforming blue star-forming galaxies into red spiral systems.