MeerKAT 1.3 GHz Observations of the Wide-angle Tail Radio Galaxy J1712–2435

Abstract We present full-polarization MeerKAT images of the wide-angle tail, giant radio galaxy J1712−2435 at 1.3 GHz with 7 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover> <mml:mrow> <mml:mo>.</mml:mo> </mml:mrow> <mml:mrow> <mml:mtext>″</mml:mtext> </mml:mrow> </mml:mover> </mml:math> 5 resolution and an rms sensitivity of 8 μ Jy beam −1 . Due to its angular proximity to the Galactic center ( l = 359 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover> <mml:mrow> <mml:mo>.</mml:mo> </mml:mrow> <mml:mrow> <mml:mtext>°</mml:mtext> </mml:mrow> </mml:mover> </mml:math> 6, b = +8 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover> <mml:mrow> <mml:mo>.</mml:mo> </mml:mrow> <mml:mrow> <mml:mtext>°</mml:mtext> </mml:mrow> </mml:mover> </mml:math> 5), the immediate environment is not well understood, but there are massive clusters nearby. Emission can be traced over an extent of 34 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover> <mml:mrow> <mml:mo>.</mml:mo> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">′</mml:mi> </mml:mrow> </mml:mover> </mml:math> 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 × 10 24 W Hz −1 , somewhat below the FRI/FRII divide. The total power emitted is estimated to be 5.6 × 10 41 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.