The unrelaxed dynamical structure of the galaxy cluster Abell 85

• Published in: arXiv.org
• Main Authors: Yu, Heng, Diaferio, Antonaldo, Agulli, Irene, Jose Alfonso Lopez Aguerri, Tozzi, Paolo
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 08.09.2016
• Subjects: Galactic clusters; Galactic evolution; Galaxies; Line of sight; Physics - Astrophysics of Galaxies; Physics - Cosmology and Nongalactic Astrophysics; Red shift; Spectroscopy; Spectrum analysis; Substructures
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1609.02237

For the first time, we explore the dynamics of the central region of a galaxy cluster within \(r_{500}\sim 600h^{-1}\)~kpc from its center by combining optical and X-ray spectroscopy. We use (1) the caustic technique that identifies the cluster substructures and their galaxy members with optical spectroscopic data, and (2) the X-ray redshift fitting procedure that estimates the redshift distribution of the intracluster medium (ICM). We use the spatial and redshift distributions of the galaxies and of the X-ray emitting gas to associate the optical substructures to the X-ray regions. When we apply this approach to Abell 85 (A85), a complex dynamical structure of A85 emerges from our analysis: a galaxy group, with redshift \(z=0.0509 \pm 0.0021\) is passing through the cluster center along the line of sight dragging part of the ICM present in the cluster core; two additional groups, at redshift \(z=0.0547 \pm 0.0022\) and \(z=0.0570 \pm 0.0020\), are going through the cluster in opposite directions, almost perpendicularly to the line of sight, and have substantially perturbed the dynamics of the ICM. An additional group in the outskirts of A85, at redshift \(z=0.0561 \pm 0.0023\), is associated to a secondary peak of the X-ray emission, at redshift \(z=0.0583^{+0.0039}_{-0.0047}\). Although our analysis and results on A85 need to be confirmed by high-resolution spectroscopy, they demonstrate how our new approach can be a powerful tool to constrain the formation history of galaxy clusters by unveiling their central and surrounding structures.