Internal dynamics of Abell 2294: a massive, likely merging cluster

Context. The mechanisms giving rise to diffuse radio emission in galaxy clusters, and in particular their connection with cluster mergers, are still debated. Aims. We seek to explore the internal dynamics of the cluster Abell 2294, which has been shown to host a radio halo. Methods. Our analysis is mainly based on redshift data for 88 galaxies acquired at the Telescopio Nazionale Galileo. We combine galaxy velocities and positions to select 78 cluster galaxies and analyze its internal dynamics. We also use both photometric data acquired at the Isaac Newton Telescope and X-ray data from the Chandra archive. Results. We re-estimate the redshift of the large, brightest cluster galaxy (BCG) obtaining < z > = 0.1690, which closely agrees with the mean cluster redshift. We estimate a quite large line-of-sight (LOS) velocity dispersion sigma(V) similar to 1400 km s(-1) and X-ray temperature T-X similar to 10 keV. Our optical and X-ray analyses detect substructure. Our results imply that the cluster is composed of two massive subclusters separated by a LOS rest frame velocity difference V-rf similar to 2000 km s-1, very closely projected in the plane of sky along the SE-NW direction. This observational picture, interpreted in terms of the analytical two-body model, suggests that Abell 2294 is a cluster merger elongated mainly in the LOS direction and captured during the bound outgoing phase, a few fractions of Gyr after the core crossing. We find that Abell 2294 is a very massive cluster with a range of M = 2-4 x 10(15) h(70)(-1) M-circle dot, depending on the adopted model. In contrast to previous findings, we find no evidence of Ha emission in the spectrum of the BCG galaxy. Conclusions. The emerging picture of Abell 2294 is that of a massive, quite normal merging cluster, like many clusters hosting diffuse radio sources. However, perhaps because of its particular geometry, more data are needed for reach a definitive, more quantitative conclusion.