High-energy monitoring of NGC 4593 II. Broadband spectral analysis: testing the two-corona model. (arXiv:1812.03180v1 [astro-ph.HE])

High-energy monitoring of NGC 4593 II. Broadband spectral analysis: testing the two-corona model. (arXiv:1812.03180v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Middei_R/0/1/0/all/0/1">R. Middei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchi_S/0/1/0/all/0/1">S. Bianchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petrucci_P/0/1/0/all/0/1">P.-O. Petrucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ursini_F/0/1/0/all/0/1">F. Ursini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cappi_M/0/1/0/all/0/1">M. Cappi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marco_B/0/1/0/all/0/1">B. De Marco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosa_A/0/1/0/all/0/1">A. De Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malzac_J/0/1/0/all/0/1">J. Malzac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marinucci_A/0/1/0/all/0/1">A. Marinucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matt_G/0/1/0/all/0/1">G. Matt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ponti_G/0/1/0/all/0/1">G. Ponti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tortosa_A/0/1/0/all/0/1">A. Tortosa</a>

It is widely believed that the primary X-ray emission of AGN is due to the
Comptonisation of optical-UV photons from a hot electron corona, while the
origin of the ‘soft-excess’ is still uncertain and matter of debate. A second
Comptonisation component, called warm corona, was therefore proposed to account
for the soft-excess, and found in agreement with the optical-UV to X-ray
emission of a sample of Seyfert galaxies. In this context, we exploit the
broadband XMM-Newton and NuSTAR simultaneous observations of the Seyfert galaxy
NGC 4593 to further test the so called “two corona model”. The NGC 4593 spectra
are well reproduced by the model, from the optical/UV to the hard X-rays.
Moreover, the data reveal a significant correlation between the hot and the
warm corona parameters during our monitoring campaign.

It is widely believed that the primary X-ray emission of AGN is due to the
Comptonisation of optical-UV photons from a hot electron corona, while the
origin of the ‘soft-excess’ is still uncertain and matter of debate. A second
Comptonisation component, called warm corona, was therefore proposed to account
for the soft-excess, and found in agreement with the optical-UV to X-ray
emission of a sample of Seyfert galaxies. In this context, we exploit the
broadband XMM-Newton and NuSTAR simultaneous observations of the Seyfert galaxy
NGC 4593 to further test the so called “two corona model”. The NGC 4593 spectra
are well reproduced by the model, from the optical/UV to the hard X-rays.
Moreover, the data reveal a significant correlation between the hot and the
warm corona parameters during our monitoring campaign.

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