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We present a spectral analysis of the Seyfert 1.8 ESO 113-G010 observed withXMM-Newton for 4 ks. The spectrum shows a soft excess below 0.7 keV and moreinterestingly a narrow emission Gaussian line at 5.4 keV (in its rest-frame),most probably originating from a redshifted iron Kalpha line. No significantline at or above 6.4 keV is found contrary to other objects showing redshiftedlines, ruling out a strong blue-wing to the line profile. The line is detectedat 99% confidence, from performing Monte Carlo simulations which fully accountfor the range of energies where a narrow iron line is likely to occur. Theenergy 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 Turneret al. (2004). Alternatively, the emission from a narrow annulus at the surfaceof 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 thisintermediate Seyfert galaxy. However emission from a small, localized hot-spoton the disk, occurring within a fraction of a complete disk orbit, could alsoexplain the redshifted line. This scenario would be directly testable in alonger observation, as one would see significant variations in the energy andintensity of the line within an orbital timescale.Comment: A&A, accepted (5 pages, 5 figures), (The html abstract was truncated  by error in the first submission, the .ps and .pdf files are strictly  identical between the first and the second submissions

XMM-Newton observation of the Seyfert 1.8 ESO 113-G010: Discovery of a highly redshifted iron line at 5.4 keV