2025ApJ...989..223C

We present full-polarization MeerKAT images of the wide-angle tail, giant radio galaxy J1712-2435 at 1.3 GHz with 7$\mathop{.}\limits^{\unicode{x02033}}$5 resolution and an rms sensitivity of 8 μJy beam^–1. Due to its angular proximity to the Galactic center (l = 359$\mathop{.}\limits^{\unicode{x000b0}}$6, b = +8$\mathop{.}\limits^{\unicode{x000b0}}$5), the immediate environment is not well understood, but there are massive clusters nearby. Emission can be traced over an extent of 34$\mathop{.}\limits^{{\rm{^{\prime} }}}$6, which at the redshift of 0.024330 corresponds to a projected length of 1.02 Mpc. The inner jets are quite straight, but then bend and completely decollimate into extended plumes nearly orthogonal to the initial jet directions at a projected distance of approximately 100 kpc. The near-unity brightness ratio of the inner jets suggest that they are orientated within a few degrees of the plane of the sky. The 1400 MHz power is 3.9 × 10²⁴ W Hz^–1, somewhat below the FRI/FRII divide. The total power emitted is estimated to be 5.6 × 10⁴¹ erg s^–1 over the range 10 MHz-100 GHz. The source dynamics are modeled with magnetohydrodynamics simulations; the result is a rough reproduction of the source's radio morphology/appearance. This study further highlights the merit of alternative scenarios, calling for future observational and numerical efforts.