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We present for the first time the timing and spectral analyses for anarrow-line Seyfert 1 galaxy, SBS 1353+564, using \it{XMM-Newton} and\it{Swift} multi-band observations from 2007 to 2019. Our main results are asfollows: 1) The temporal variability of SBS 1353+564 is random, while thehardness ratio is relatively constant over a time span of 13 years; 2) We finda prominent soft X-ray excess feature below 2 keV, which cannot be welldescribed by a simple blackbody component; 3) After comparing the two mostprevailing models for interpreting the origin of the soft X-ray excess, we findthat the relativistically smeared reflection model is unable to fit the dataabove 5 keV well and the X-ray spectra do not show any reflection features,such as the Fe K\alpha emission line. However, the warm corona model can obtaina good fitting result. For the warm corona model, we try to use three differentsets of spin values to fit the data and derive different best-fitting parametersets; 4) We compare the UV/optical spectral data with the extrapolated valuesof the warm corona model to determine which spin value is more appropriate forthis source, and we find that the warm corona model with non-spin cansufficiently account for the soft X-ray excess in SBS 1353+564.

The origin of the soft X-ray excess in the narrow-line Seyfert 1 galaxy SBS 1353+564