The Low-temperature Corona in ESO 511−G030 Revealed by NuSTAR and XMM-Newton

Author:

Zhang Zuobin,Jiang JiachenORCID,Liu Honghui,Bambi CosimoORCID,Reynolds Christopher S.ORCID,Fabian Andrew C.ORCID,Dauser ThomasORCID,Madsen KristinORCID,Young Andrew,Gallo Luigi,Yu Zhibo,Tomsick JohnORCID

Abstract

Abstract We present the results from a coordinated XMM-Newton + NuSTAR observation of the Seyfert 1 galaxy ESO 511−G030. With this joint monitoring program, we conduct a detailed variability and spectral analysis. The source remained in a low flux and very stable state throughout the observation period, although there are slight fluctuations of flux over long timescales. The broadband (0.3–78 keV) spectrum shows the presence of a power-law continuum with a soft excess below 2 keV, a relatively narrow iron Kα emission (∼6.4 keV), and an obvious cutoff at high energies. We find that the soft excess can be modeled by two different possible scenarios: a warm (kT e ∼ 0.19 keV) and optically thick (τ = 18–25) Comptonizing corona or a relativistic reflection from a high-density ( log [ n e / cm 3 ] = 17.1 18.5 ) inner disk. All models require a low temperature (kT e ∼ 13 keV) for the hot corona.

Funder

National Natural Science Foundation of China

Natural Science Foundation of Shanghai

Shanghai Municipal Education Commission

Fudan University

Publisher

American Astronomical Society

Subject

Space and Planetary Science,Astronomy and Astrophysics

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1. MRI turbulence in vertically stratified accretion discs at large magnetic Prandtl numbers;Monthly Notices of the Royal Astronomical Society;2024-04-03

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