Properties of barred galaxies with the environment

Context. Bars are elongated structures developed by a large fraction of disk galaxies in their central few kiloparsecs. However, the bar formation process is still not fully understood, particularly the role played by the galaxy environment in the formation and evolution of these structures. Aims. The aim of this work is to establish how the galaxy environment affects the evolution of bars by analyzing the bar structural parameters in a sample of galaxies located in three different galaxy environments: in the Virgo cluster, in filaments in the Cosmic Web around it, and in the field. Methods. We performed structural analysis using optical imaging from the DESI Legacy survey, measuring bar radii and disk scale lengths through Fourier analysis and surface brightness fitting techniques. Results. After defining a homogeneous sample of barred galaxies across the three different galaxy environments in terms of color and magnitude, the median bar radii were found to be 2.54 ± 0.34 kpc, 3.29 ± 0.38 kpc, and 4.44 ± 0.81 kpc in the cluster, filaments, and field environments, respectively. In addition, the median bar radii scaled by the disk scale lengths were found to be 1.26 ± 0.09, 1.72 ± 0.11, and 2.57 ± 0.21 in the cluster, filaments, and field environments, respectively. These results indicate that the galaxy environment has a significant influence on the structural parameters of bars, with bars in high-density environments being shorter and less prominent than those in the field. Conclusions. Our findings can be interpreted in terms of a slowing of the secular evolution of bars in dense galaxy environments. Barred galaxies located in clusters could experience a reduced rate of bar secular evolution due to various physical processes that occur in high-density environments, such as gas stripping, strangulation, or tidal interactions.