Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum

R. Middei; S. Bianchi; M. Cappi; P.-O. Petrucci; F. Ursini; N. Arav; E. Behar; G. Branduardi-Raymont; E. Costantini; B. De Marco; L. Di Gesu; J. Ebrero; J. Kaastra; S. Kaspi; G. A. Kriss; J. Mao; M. Mehdipour; S. Paltani; U. Peretz; G. Ponti

doi:10.1051/0004-6361/201832726

Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum

R. Middei^*, S. Bianchi, M. Cappi, P.-O. Petrucci, F. Ursini, N. Arav, E. Behar, G. Branduardi-Raymont, E. Costantini, B. De Marco, L. Di Gesu, J. Ebrero, J. Kaastra, S. Kaspi, G. A. Kriss, J. Mao, M. Mehdipour, S. Paltani, U. Peretz, G. Ponti

^*Corresponding author for this work

Physics

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Abstract

We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off E_cut = 170⁺ ₋ ⁶⁰ ₄₀ keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45⁺ ₋ ¹⁵ ₁₂ keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3−0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.

Original language	English
Article number	A163
Number of pages	10
Journal	Astronomy and Astrophysics
Volume	615
Early online date	1 Aug 2018
DOIs	https://doi.org/10.1051/0004-6361/201832726
Publication status	E-pub ahead of print - 1 Aug 2018

Funding

Acknowledgements. We thank the referee for helping us improve the quality of this paper. This work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the nustardas jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work is also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). RM and SB acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. SB acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0. POP acknowledges financial support from the CNES french agency and the CNRS PNHE. GP acknowledges support by the Bundesministerium für Wirtschaft und Technologie/Deutsches Zentrum für Luftund Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research.BDM acknowledges support from the Polish National Science Center grant Polonez 2016/21/P/ST9/04025. The research at the Technion is supported by the I-CORE programme of the Planning and Budgeting Committee (grant number 1937/12). EB acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska–Curie grant agreement no. 655324. M.C. acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.O

Keywords

active
galaxies
quasars
X-rays
Seyfert galaxy

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10.1051/0004-6361/201832726

Middei-etal-AA-2018-Multi-wavelength-campaign-on-NCG-7469Accepted author manuscript, 0.98 MB

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Middei, R., Bianchi, S., Cappi, M., Petrucci, P.-O., Ursini, F., Arav, N., Behar, E., Branduardi-Raymont, G., Costantini, E., De Marco, B., Di Gesu, L., Ebrero, J., Kaastra, J., Kaspi, S., Kriss, G. A., Mao, J., Mehdipour, M., Paltani, S., Peretz, U., & Ponti, G. (2018). Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum. Astronomy and Astrophysics, 615, Article A163. Advance online publication. https://doi.org/10.1051/0004-6361/201832726

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title = "Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum",

abstract = "We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off Ecut = 170+ − 60 40 keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45+ − 15 12 keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3−0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.",

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author = "R. Middei and S. Bianchi and M. Cappi and P.-O. Petrucci and F. Ursini and N. Arav and E. Behar and G. Branduardi-Raymont and E. Costantini and {De Marco}, B. and {Di Gesu}, L. and J. Ebrero and J. Kaastra and S. Kaspi and Kriss, {G. A.} and J. Mao and M. Mehdipour and S. Paltani and U. Peretz and G. Ponti",

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Middei, R, Bianchi, S, Cappi, M, Petrucci, P-O, Ursini, F, Arav, N, Behar, E, Branduardi-Raymont, G, Costantini, E, De Marco, B, Di Gesu, L, Ebrero, J, Kaastra, J, Kaspi, S, Kriss, GA, Mao, J, Mehdipour, M, Paltani, S, Peretz, U & Ponti, G 2018, 'Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum', Astronomy and Astrophysics, vol. 615, A163. https://doi.org/10.1051/0004-6361/201832726

TY - JOUR

T1 - Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum

AU - Middei, R.

AU - Bianchi, S.

AU - Cappi, M.

AU - Petrucci, P.-O.

AU - Ursini, F.

AU - Arav, N.

AU - Behar, E.

AU - Branduardi-Raymont, G.

AU - Costantini, E.

AU - De Marco, B.

AU - Di Gesu, L.

AU - Ebrero, J.

AU - Kaastra, J.

AU - Kaspi, S.

AU - Kriss, G. A.

AU - Mao, J.

AU - Mehdipour, M.

AU - Paltani, S.

AU - Peretz, U.

AU - Ponti, G.

PY - 2018/8/1

Y1 - 2018/8/1

N2 - We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off Ecut = 170+ − 60 40 keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45+ − 15 12 keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3−0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.

AB - We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off Ecut = 170+ − 60 40 keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45+ − 15 12 keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3−0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.

KW - active

KW - galaxies

KW - quasars

KW - X-rays

KW - Seyfert galaxy

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UR - https://arxiv.org/abs/1803.07334

U2 - 10.1051/0004-6361/201832726

DO - 10.1051/0004-6361/201832726

M3 - Article

AN - SCOPUS:85056656537

SN - 0004-6361

VL - 615

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A163

ER -

Multi-wavelength campaign on NCG 7469 IV. The broad-band X-ray spectrum

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