Unveiling the shape: a multi-wavelength analysis of the galaxy clusters Abell 76 and Abell 1307

Abstract

We analyse the dynamical state of the galaxy clusters Abell 76 and Abell 1307 from the optical point of view, presenting a coherent scenario that responds to the X-ray emissions observed in these structures. Our study is based on 231 and 164 spectroscopic redshifts, for the clusters A76 and A1307, respectively. We find that A76 and A1307 are two galaxy clusters at $z=0.0390$ and 0.0815, respectively, with velocity dispersions of $650\pm 56$ km s${}^{-1}$ and $863\pm 85$ km s${}^{-1}$, and showing velocity distributions following, in practice, Gaussian profiles. From our dynamical analysis, X-ray studies and SZ-Planck emission, we obtain a mean total mass M${}_{500}=1.7\pm 0.6\cdot 10^{14}$ M${}_{\odot }$ and $3.5\pm 1.3\cdot 10^{14}$ M${}_{\odot }$ for A76 and A1307, respectively. We find that the spatial distribution of likely cluster members in the case of A76 is very anisotropic, while A1307 shows a compact distribution of galaxies, but double peaked and elongated in the south-north direction. we compare the XMM-Newton surface brightness maps with galaxy distributions and see that both distributions are correlated. We reconstruct the total mass profile and velocity anisotropy of both clusters by analysing the full projected phase space, through the MG-MAMPOSSt code. Our study reveals a slight indication of radial orbits for A76, while A1307 seems to prefer more isotropic orbits in the whole cluster range. Summarizing, A76 represent a typical young cluster, in an early stage of formation, with a very low X-ray surface brightness but high temperature showing a very anisotropic galaxy distribution. A1307 is however more consolidated and massive showing in-homogeneous galaxy distribution and an asymmetric X-ray emission, which suggest a scenario characterised by recent minor mergers.

14 pages and 12 figures. Tables 1 and 2 are included as electronic form at the CDS

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• CHEX-MATE: exploring the kinematical properties of Planck galaxy clusters