We analyze the dynamical state of Abell 1914 , a merging cluster hosting a radio halo , quite unusual for its structure .
Our study considers spectroscopic data for 119 galaxies obtained with the Italian Telescopio Nazionale Galileo .
We select 89 cluster members from spatial and velocity distributions .
We also use photometry Canada-France-Hawaii Telescope archives .
We compute the mean cluster redshift , \left < z \right > = 0.168 , and the velocity dispersion which shows a high value , \sigma _ { V } = 1210 _ { -110 } ^ { +125 } km s ^ { -1 } .
From the 2D analysis we find that Abell 1914 has a NE-SW elongated structure with two galaxy clumps , that mostly merge in the plane of the sky .
Our best , but very uncertain estimate of the velocity dispersion of the main system is \sigma _ { V,main } \sim 1000 km s ^ { -1 } .
We estimate a virial mass M _ { sys } = 1.4 –2.6 \times 10 ^ { 15 } h _ { 70 } ^ { -1 } M _ { \odot } for the whole system .
We study the merger through a simple two-body model and find that data are consistent with a bound , outgoing substructure observed just after the core crossing .
By studying the 2D distribution of the red galaxies , photometrically selected , we show that Abell 1914 is contained in a rich large scale structure , with two close companion galaxy systems , known to be at z \sim 0.17 .
The system at SW supports the idea that the cluster is accreting groups from a filament aligned in the NE-SW direction , while that at NW suggests a second direction of the accretion ( NW-SE ) .
We conclude that Abell 1914 well fits among typical clusters with radio halos .
We argue that the unusual radio emission is connected to the complex cluster accretion and suggest that Abell 1914 resembles the well-known nearby merging cluster Abell 754 for its particular observed phenomenology .