We present high resolution radio continuum observations with the Karl G. Jansky Very Large Array at 6 , 8.5 , 11.5 and 15 GHz of the double-peaked emission-line galaxy 2MASXJ12032061+1319316 .
The radio emission has a prominent S-shaped morphology with highly symmetric radio jets that extend over a distance of \sim 1.5 ^ { \prime \prime } ( 1.74 kpc ) on either side of the core of size \sim 0.1 ^ { \prime \prime } ( 116 pc ) .
The radio jets have a helical structure resembling the precessing jets in the galaxy NGC 326 which has confirmed dual active galactic nuclei ( AGN ) .
The nuclear bulge velocity dispersion gives an upper limit of ( 1.56 \pm 0.26 ) \times 10 ^ { 8 } M _ { \odot } for the total mass of nuclear black hole ( s ) .
We present a simple model of precessing jets in 2MASXJ1203 and find that the precession timescale is around 10 ^ { 5 } years : this matches the source lifetime estimate via spectral aging .
We find that the expected super massive black hole ( SMBH ) separation corresponding to this timescale is 0.02 pc .
We used the double peaked emission lines in 2MASXJ1203 to determine an orbital speed for a dual AGN system and the associated jet precession timescale , which turns out to be more than the Hubble time , making it unfeasible .
We conclude that the S-shaped radio jets are due to jet precession caused either by a binary/dual SMBH system , a single SMBH with a tilted accretion disk or a dual AGN system where a close pass of the secondary SMBH in the past has given rise to jet precession .