The pc-scale radio structure of MIR-observed radio galaxies
  We investigated the relationship between the accretion process and jet
properties by ultilizing the VLBA and mid-infrared (MIR) data for a sample of
45 3CRR radio galaxies selected with a flux density at 178 MHz $>16.4$ Jy, 5
GHz VLA core flux density $\geq$ 7 mJy, and MIR observations. The pc-scale
radio structure at 5 GHz are presented by using our VLBA observations for 21
sources in February, 2016, the analysis on the archival data for 16 objects,
and directly taking the measurements for 8 radio galaxies available in
literatures. The accretion mode is constrained from the Eddington ratio with a
dividing value of 0.01, which is estimated from the MIR-based bolometric
luminosity and the black hole masses. While most FRII radio galaxies have
higher Eddington ratio than FRIs, we found that there is indeed no single
correspondence between the FR morphology and accretion mode with eight FRIIs at
low accretion and two FRIs at high accretion rate. There is a significant
correlation between the VLBA core luminosity at 5 GHz and the Eddington ratio.
Various morphologies are found in our sample, including core only, single-sided
core-jet, and two-sided core-jet structures. We found that the higher accretion
rate may be more likely related with the core-jet structure, thus more extended
jet. These results imply that the higher accretion rates are likely able to
produce more powerful jets. There is a strong correlation between the MIR
luminosity at 15 $\mu$m and VLBA 5 GHz core luminosity, in favour of the tight
relation between the accretion disk and jets. In our sample, the core
brightness temperature ranges from $10^{9}$ to $10^{13.38}$ K with a median
value of $10^{11.09}$ K indicating that systematically the beaming effect may
not be significant....
