Unified properties of supermassive black hole winds in radio-quiet and radio-loud AGN

Author:

Mestici S12,Tombesi F134,Gaspari M5ORCID,Piconcelli E3,Panessa F6ORCID

Affiliation:

1. Physics Department, Tor Vergata University of Rome , Via della Ricerca Scientifica 1, 00133 Rome , Italy

2. Physics Department, Sapienza University of Rome, Piazzale Aldo Moro , 00185 Rome , Italy

3. INAF – Astronomical Observatory of Rome , Via Frascati 33, 00040 Monte Porzio Catone , Italy

4. INFN – Rome Tor Vergata , Via della Ricerca Scientifica 1, 00133 Rome , Italy

5. Department of Physics, Informatics and Mathematics, University of Modena and Reggio Emilia , 41125 Modena , Italy

6. INAF – Istituto di Astrofisica e Planetologia Spaziali , via Fosso del Cavaliere 100, I-00133 Roma , Italy

Abstract

ABSTRACT Powerful supermassive black hole (SMBH) winds in the form of ultra-fast outflows (UFOs) are detected in the X-ray spectra of several active galactic nuclei (AGNs) seemingly independently of their radio classification between radio quiet (RQ) and radio loud (RL). In this work, we explore the physical parameters of SMBH winds through a uniform analysis of a sample of X-ray bright RQ and RL AGN. We explored several correlations between different wind parameters and with respect to the AGN bolometric and Eddington luminosities. Our analysis shows that SMBH winds are not only a common trait of both AGN classes but also that they are most likely produced by the same physical mechanism. Consequently, we find that SMBH winds do not follow the radio-loudness dichotomy seen in jets. On average, a comparable amount of material accreted by the SMBH is ejected through such winds. The average wind power corresponds to about 3 per cent of the Eddington luminosity, confirming that they can drive AGN feedback. Moreover, the most energetic outflows are found in the most luminous sources. We find a possible positive correlation of the wind energetics, renormalized to the Eddington limit, with respect to $\lambda _{\mathrm{ Edd}}$, consistent with the correlation found with bolometric luminosity. We also observe a possible positive correlation between the energetics of the outflow and the X-ray radio-loudness parameter. In general, these results suggest an underlying relation between the acceleration mechanisms of accretion disc winds and jets.

Funder

European Union

ERC

Publisher

Oxford University Press (OUP)

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