We present an analysis of spectrum and variability of the bright reddened narrow line Seyfert 1 galaxy Was?61 using 90 ks archival XMM-Newton data. The X-ray spectrum in 0.2–10 keV can be characterized by an absorbed power-law plus soft excess and an Fe?Kα emission line. The power-law spectral index remains constant during the flux variation. The absorbing material is mildly ionized, with a column density of 3.2?×?1021 cm?2, and does not appear to vary during the period of the X-ray observation. If the same material causes the optical reddening (E(B–V)??0.6 mag), it must be located?outside the narrow line region with a dust-to-gas ratio similar to the average Galactic value. We detect significant variations of the Fe?Kα line during the observational period. A broad Fe?Kα line at with a width of ~0.6 keV is detected in the low flux segment of the first 40 ks exposure, and is absent in the spectra of other segments; a narrow Fe?Kα emission line ~6.4 keV with a width of ~0.1 keV is observed in the subsequent 20 ks segment, which has a count rate 35% higher and is in the next day. We believe this is due to the change in geometry and kinematics of the X-ray emitting corona. The temperature and flux of soft X-ray excess appear to correlate with the flux of the hard power-law component. Comptonization of disc photons by a warm and optically thick inner disk is preferred to interpret the soft excess, rather than the ionized reflection.
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