We present here the results from dual-frequency phase-referenced VLBI observations of the Seyfert galaxy KISSR 1494 , 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 \pm 0.5 ( S _ { \nu } \propto \nu ^ { \alpha } ) .
The high brightness temperature of the radio component ( \sim 1.4 \times 10 ^ { 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 \sim 1.4 \pm 1.0 \times 10 ^ { 8 } ~ { } M _ { \sun } ; it is accreting at an Eddington rate of \sim 0.02 .
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 KISSR 1494 .
From the kiloparsec-scale radio emission , the time-averaged kinetic power of this outflow is estimated to be Q \approx 1.5 \times 10 ^ { 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 .