VLBI Imaging of the Double Peaked Emission Line Seyfert KISSR1494
  We present here the results from dual-frequency phase-referenced VLBI
observations of the Seyfert galaxy KISSR1494, which exhibits double peaked
emission lines in its SDSS spectrum. We detect a single radio component at 1.6
GHz, but not at 5 GHz implying a spectral index steeper than $-1.5\pm0.5$
($S_\nu\propto\nu^\alpha$). The high brightness temperature of the radio
component ($\sim1.4\times10^7$ K) and the steep radio spectrum support a
non-thermal synchrotron origin. A crude estimate of the black hole mass derived
from the $M_{BH}-\sigma_{\star}$ relation is $\sim1.4\pm1.0\times10^8$ Msun; it
is accreting at an Eddington rate of $\sim0.02$. The radio data are consistent
with either the radio emission coming from the parsec-scale base of a
synchrotron wind originating in the magnetised corona above the accretion disk,
or from the inner ionised edge of the accretion disk or torus. In the former
case, the narrow line region (NLR) clouds may form a part of the broad outflow,
while in the latter, the NLR clouds may form a part of an extended disk beyond
the torus. The radio and NLR emission may also be decoupled so that the radio
emission originates in an outflow while the NLR is in a disk, and vice versa.
While with the present data, it is not possible to clearly distinguish between
these scenarios, there appears to be greater circumstantial evidence supporting
the coronal wind picture in KISSR1494. From the kiloparsec-scale radio
emission, the time-averaged kinetic power of this outflow is estimated to be
$Q\approx1.5\times10^{42}$ erg s$^{-1}$, which is typical of radio outflows in
low-luminosity AGN. This supports the idea that radio "jets" and outflowing
coronal winds are indistinguishable in Seyfert galaxies.
