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The enigmatic and intriguing phenomenon of the "soft excess" observed in the X-ray spectra of luminous quasars continues to be a subject of considerable interest and debate in the field of high-energy astrophysics. This study focuses on the quasar HE 1029-1401 (z=0. 086, (L₁₎₋/erg\, s^-1) = 46. 0 0. 2), with a particular emphasis on investigating the properties of the hot corona and the physical origin of the soft excess. In this study, we present the results of a joint XMM-Newton/NuSTAR monitoring campaign of this quasar conducted in May 2022. The source exhibits a cold and narrow Fe K emission line at 6. 4 keV, in addition to the detection of a broad component. Our findings suggest that the soft excess observed in HE 1029-1401 can be adequately explained by Comptonized emission originating from a warm corona. Specifically, fitting the spectra with two \, component we found that the warm corona is characterized by a photon index (^w) of 2. 750. 05 and by an electron temperature (kT₄^w) of 0. 39^+0. 06-₀. ₀₄ keV, while the optical depth (^w) is found to be 233. We also test more physical models for the warm corona, corresponding to two scenarios: pure Comptonization and Comptonization plus reflection. Both models provide a good fit to the data, and are in agreement with a radially extended warm corona having a size of a few tens of gravitational radii.
Vaia et al. (Mon,) studied this question.