  Over recent years there has been mounting evidence that accreting
supermassive black holes in active galactic nuclei (AGN) and stellar mass black
holes have similar observational signatures: thermal emission from the
accretion disk, X-ray corona, and relativisitic jets. Further, there have been
investigations into whether or not AGN have spectral states similar to that of
X-ray binaries (XRBs) and what parallels can be drawn between the two using a
hardness-intensity diagram (HID). To address whether AGN jets might be related
to accretion states as in XRBs, we explore whether populations of radio-AGN
classified according to their radio jet morphology (Fanaroff-Riley classes I
and II; FR I and II), excitation class (HERG and LERG), and radio jet linear
extent (compact to giant) occupy different and distinct regions of the AGN
hardness-intensity diagram (total luminosity vs. hardness). We do this by cross
correlating 15 catalogs of radio galaxies with the desired characteristics from
the literature with XMM Newton and Swift X-ray and ultraviolet (UV) source
catalogs. We calculate the luminosity and hardness from the X-ray and UV
photometry, place the sources on the AGN hardness-intensity diagram, and search
for separation of populations and analogies with the XRB spectral state HID. We
find that (a) FR Is and IIs, (b) HERGs and LERGs, (c) FR I-LERGs and FR
II-HERGs occupy distinct areas of the HID at a statistically significant level
(p-value < 0.05) and no clear evidence for population distinction between the
different radio jet linear extents. The separation between FR I-LERG and FR
II-HERG populations is the strongest in this work. Our results indicate that
radio-loud AGN occupy distinct areas of the HID depending on the morphology and
excitation class, showing strong similarities to XRBs.
