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Previous X-ray spectral analysis has revealed an increasing number of AGNs with high accretion rates where an outflow with a mildly relativistic velocity originates from the inner accretion disk. Here we report the detection of a new ultra-fast outflow (UFO) with a velocity of $v_{rm out}=0.319^{+0.005}_{-0.008}c$ in addition to a relativistic disk reflection component in a poorly studied NLS1 WKK~4438, based on archival ustar and suzaku observations. The spectra of both suzaku and ustar observations show an Fe~textsc{xxvi} absorption feature and the suzaku data also show evidence for an Ar~textsc{xviii} with the same blueshift. A super-solar argon abundance ($Z^{prime}_{rm Ar}>6Z_{odot}$) and a slight iron over-abundance ($Z^{prime}_{rm Fe}=2.6^{+1.9}_{-2.0}Z_{odot}$) are found in our spectral modelling. Based on Monte-Carlo simulations, the detection of the UFO is estimated to be around at 3$sigma$ significance. The fast wind most likely arises from a radius of $geq20r_g$ away from the central black hole. The disk is accreting at a high Eddington ratio ($L_{rm bol}=0.4-0.7L_{rm Edd}$). The mass outflow rate of the UFO is comparable with the disk mass inflow rate ($dot M_{rm out}>30%dot M_{rm in}$), assuming a maximum covering factor. The kinetic power of the wind might not be high enough to have influence in AGN feedback ($dot E_{rm wind}/L_{rm bol}approx 3-5%$) due to a relatively small column density ($12^{+9}_{-4}times10^{22}$~cm$^{-2}$). However note that both the inferred velocity and the column density could be lower limits owing to the low viewing angle ($i=23^{+3}_{-2}$$^{circ}$).
Past X-ray observations of the nearby luminous quasar PDS 456 (at $z=0.184$) have revealed a wide angle accretion disk wind (Nardini et al. 2015), with an outflow velocity of $sim-0.25c$, as observed through observations of its blue-shifted iron K-sh
We present an improved model for excess variance spectra describing ultra-fast outflows and successfully apply it to the luminous (L ~ 10^47 erg/s) low-redshift (z = 0.184) quasar PDS 456. The model is able to account well for the broadening of the s
Gamma Cas and its dozen analogs comprise a small but distinct class of X-ray sources. They are early Be-type stars with an exceptionally hard thermal X-ray emission. The X-ray production mechanism has been under intense debate. Two competing ideas ar
We present the first broadband 0.3-25.0 kev X-ray observations of the bright ultraluminous X-ray source (ULX) Holmberg II X-1, performed by NuSTAR, XMM-Newton and Suzaku in September 2013. The NuSTAR data provide the first observations of Holmberg II
We present an analysis of the spectral shape and pulse profile of the accretion-powered pulsar 4U 1626-67 observed with Suzaku and NuSTAR during a spin-up state. The pulsar, which experienced a torque reversal to spin-up in 2008, has a spin period of