Interferometric Monitoring of Gamma-ray Bright AGNs: OJ 287
  We present the results of simultaneous multi-frequency imaging observations
at 22, 43, 86, and 129\,GHz of OJ\,287. We used the Korean VLBI Network as part
of the Interferometric MOnitoring of GAmma-ray Bright active galactic nuclei
(iMOGABA). The iMOGABA observations were performed during 31 epochs from 2013
January 16 to 2016 December 28. We also used 15\,GHz OVRO and 225\,GHz SMA flux
density data. We analyzed four flux enhancements in the light curves. The
estimated time scales of three flux enhancements were similar with time scales
of $\sim$50 days at two frequencies. A fourth flux enhancement had a
variability timescale approximately twice as long. We found that 225\,GHz
enhancements led the 15\,GHz enhancements by a range of 7 to 30 days in the
time delay analysis. We found the fractional variability did not change with
frequency between 43 and 86\,GHz. We could reliably measure the turnover
frequency, $\nu_{\rm c}$, of the core of the source in three epochs. This was
measured to be in a range from 27 to 50\,GHz and a flux density at the turnover
frequency, $S_{\rm m}$, ranging from 3-6\,Jy. The derived SSA magnetic fields,
$B_{\rm SSA}$, are in a range from $0.157\pm0.104$ to $0.255\pm0.146$ mG. We
estimated the equipartition magnetic field strengths to be in a range from
$0.95\pm0.15$ to $1.93\pm0.30$ mG. The equipartition magnetic field strengths
are up to a factor of 10 higher than the values of $B_{\rm SSA}$. We conclude
that the downstream jet may be more particle energy dominated.
