High-energy monitoring of NGC 4593 with XMM-Newton and NuSTAR. X-ray spectral analysis

Creators: Ursini, F.; Petrucci, P.-O.; Matt, G.; Bianchi, S.; Cappi, M.; De Marco, B.; De Rosa, A.; Malzac, J.; Marinucci, A.; Ponti, G.; Tortosa, A.

Abstract

We present results from a joint XMM–Newton/NuSTAR monitoring of the Seyfert 1 NGC 4593, consisting of 5 × 20 ks simultaneous observations spaced by 2 d, performed in 2015 January. The source is variable, both in flux and spectral shape, on time-scales down to a few ks and with a clear softer-when-brighter behaviour. In agreement with past observations, we find the presence of a warm absorber well described by a two-phase ionized outflow. The source exhibits a cold, narrow and constant Fe Kα line at 6.4 keV, and a broad component is also detected. The broad-band (0.3–79 keV) spectrum is well described by a primary power law with Γ ≃ 1.6–1.8 and an exponential cut-off varying from 90^(+40_+(−20) to >700 keV, two distinct reflection components, and a variable soft excess correlated with the primary power law. This campaign shows that probing the variability of Seyfert 1 galaxies on different time-scales is of prime importance to investigate the high-energy emission of active galactic nuclei.

Additional Information

© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 August 9. Received 2016 August 9; in original form 2016 July 4. Published: 12 August 2016. We thank the anonymous referee for helpful comments and suggestions that improved the paper. This work is based on observations obtained with: the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA; XMM–Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of data, software and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. FU, P-OP, GM, SB, MC, ADR and JM acknowledge support from the French–Italian International Project of Scientific Collaboration: PICS-INAF project number 181542. FU and P-OP acknowledge support from CNES. FU acknowledges support from Université Franco-Italienne (Vinci PhD fellowship). FU and GM acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. P-OP acknowledges financial support from the Programme National Hautes Energies. SB, MC and ADR acknowledge financial support from the Italian Space Agency under grant ASI-INAF I/037/12/P1. GP acknowledges support by the Bundesministerium für Wirtschaft und Technologie/Deutsches Zentrum für Luft und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society.

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