SITELLE H{\alpha} Imaging Spectroscopy of z~0.25 Clusters: Emission Line Galaxy Detection and Ionized Gas Offset in Abell 2390 & Abell 2465

TL;DR

This study uses SITELLE imaging spectroscopy to analyze emission line galaxies in two galaxy clusters at z~0.25, revealing that ram pressure stripping during initial infall causes gas offsets and star formation quenching.

Contribution

It introduces a pipeline for identifying emission line galaxies and demonstrates the role of ram pressure stripping in galaxy evolution within clusters.

Findings

Offsets point away from cluster centers, indicating ram pressure effects.

High-velocity infalling galaxies show significant gas offsets.

Lower Hα flux in galaxies with large offsets supports ram pressure quenching.

Abstract

Environmental effects are crucial to the understanding of the evolution of galaxies in dense environments, such as galaxy clusters. Using the large field-of-view of SITELLE, the unique imaging fourier transform spectrograph at CFHT, we are able to obtain 2D spectral information for a large and complete sample of cluster galaxies out to the infall region. We describe a pipeline developed to identify emission line galaxies (ELGs) from the datacube using cross-correlation techniques. We present results based on the spatial offsets between the emission-line regions and stellar continua in ELGs from two z$\sim$0.25 galaxy clusters, Abell 2390 and Abell 2465. We find a preference in the offsets being pointed away from the cluster center. Combining the two clusters, there is a 3$\sigma$ excess for high-velocity galaxies within the virial radius having the offsets to be pointed away from the cluster center. Assuming the offset being a proxy for the velocity vector of a galaxy, as expected from ram pressure stripping, this excess indicates that ram pressure stripping occurs most effectively during the first passage of an infalling galaxy, leading to the quenching of its star formation. We also find that, outside the virial region, the continuum-normalized H$\alpha$ line flux for infalling galaxies with large offsets are on average lower than those with small or no measurable offset, further supporting ram pressure as a dominant quenching mechanism during the initial infall stages.