  We present a spectral analysis of the Seyfert 1.8 ESO 113-G010 observed with
XMM-Newton for 4 ks. The spectrum shows a soft excess below 0.7 keV and more
interestingly a narrow emission Gaussian line at 5.4 keV (in its rest-frame),
most probably originating from a redshifted iron Kalpha line. No significant
line at or above 6.4 keV is found contrary to other objects showing redshifted
lines, ruling out a strong blue-wing to the line profile. The line is detected
at 99% confidence, from performing Monte Carlo simulations which fully account
for the range of energies where a narrow iron line is likely to occur. The
energy of the line could indicate emission from relativistic (0.17 - 0.23 c)
ejected matter moving away from the observer, as proposed for Mrk 766 by Turner
et al. (2004). Alternatively, the emission from a narrow annulus at the surface
of the accretion disk is unlikely due to the very small inclination angle (i.e.
less than 10 deg) required to explain the narrow, redshifted line in this
intermediate Seyfert galaxy. However emission from a small, localized hot-spot
on the disk, occurring within a fraction of a complete disk orbit, could also
explain the redshifted line. This scenario would be directly testable in a
longer observation, as one would see significant variations in the energy and
intensity of the line within an orbital timescale.

Astrophysics