X-ray Emission of the $\gamma$-ray Loud Young Radio Galaxy NGC 3894
  The radio source 1146+596 is hosted by an elliptical/S0 galaxy NGC\,3894,
with a low-luminosity active nucleus. The radio structure is compact,
suggesting a very young age of the jets in the system. Recently, the source has
been confirmed as a high-energy (HE, $>0.1$\,GeV) $\gamma$-ray emitter, in the
most recent accumulation of the {\it Fermi} Large Area Telescope (LAT) data.
Here we report on the analysis of the archival {\it Chandra} X-ray Observatory
data for the central part of the galaxy, consisting of a single 40\,ksec-long
exposure. We have found that the core spectrum is best fitted by a combination
of an ionized thermal plasma with the temperature of $\simeq 0.8$\,keV, and a
moderately absorbed power-law component (photon index $\Gamma = 1.4\pm 0.4$,
hydrogen column density $N_{\rm H}/10^{22}$\,cm$^{-2}$\,$= 2.4\pm 0.7$). We
have also detected the iron K$\alpha$ line at $6.5\pm 0.1$\,keV, with a large
equivalent width of EW\,$= 1.0_{-0.5}^{+0.9}$\,keV. Based on the simulations of
the {\it Chandra}'s Point Spread Function (PSF), we have concluded that, while
the soft thermal component is extended on the scale of the galaxy host, the
hard X-ray emission within the narrow photon energy range 6.0--7.0\,keV
originates within the unresolved core (effectively the central kpc radius). The
line is therefore indicative of the X-ray reflection from a cold neutral gas in
the central regions of NGC\,3894. We discuss the implications of our findings
in the context of the X-ray Baldwin effect. NGC\,3894 is the first young radio
galaxy detected in HE $\gamma$-rays with the iron K$\alpha$ line.
