Volume 644, December 2020
|Number of page(s)||18|
|Published online||24 November 2020|
Galaxy-scale ionised winds driven by ultra-fast outflows in two nearby quasars⋆
INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50127 Firenze, Italy
2 Dipartimento di Fisica e Astronomia, Università di Firenze, Via G. Sansone 1, 50019 Sesto Fiorentino, Firenze, Italy
3 Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Avda. Vicuña Mackenna 4860, 8970117 Macul, Santiago, Chile
4 Osservatorio Astronomico di Roma – INAF, Via Frascati 33, 00040 Monte Porzio Catone, Italy
5 INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, Italy
6 Dipartimento di Fisica, Univerisità di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy
7 Department of Astronomy, University of Maryland, College Park, MD 20742, USA
8 X-ray Astrophysics Laboratory, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
9 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
10 Centro de Astrobiología (CSIC-INTA), Departamento de Astrofísica, Cra. de Ajalvir Km 4, 28850 Torreón de Ardoz, Madrid, Spain
11 Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy
12 Dipartimento di Fisica e Astronomia, Alma Mater Studiorum Universitá di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy
Accepted: 21 September 2020
We used MUSE adaptive optics data in narrow field mode to study the properties of the ionised gas in MR 2251−178 and PG 1126−041, two nearby (z ≃ 0.06) bright quasars (QSOs) hosting sub-pc scale ultra-fast outflows (UFOs) detected in the X-ray band. We decomposed the optical emission from diffuse gas into a low- and a high-velocity components. The former is characterised by a clean, regular velocity field and a low (∼80 km s−1) velocity dispersion. It traces regularly rotating gas in PG 1126−041, while in MR 2251−178 it is possibly associated with tidal debris from a recent merger or flyby. The other component is found to be extended up to a few kpc from the nuclei, and shows a high (∼800 km s−1) velocity dispersion and a blue-shifted mean velocity, as is expected from outflows driven by active galactic nuclei (AGN). We estimate mass outflow rates up to a few M⊙ yr−1 and kinetic efficiencies LKIN/LBOL between 1−4 × 10−4, in line with those of galaxies hosting AGN of similar luminosities. The momentum rates of these ionised outflows are comparable to those measured for the UFOs at sub-pc scales, which is consistent with a momentum-driven wind propagation. Pure energy-driven winds are excluded unless about 100× additional momentum is locked in massive molecular winds. In comparing the outflow properties of our sources with those of a small sample of well-studied QSOs hosting UFOs from the literature, we find that winds seem to systematically lie either in a momentum-driven or an energy-driven regime, indicating that these two theoretical models bracket the physics of AGN-driven winds very well.
Key words: quasars: individual: MR 2251−178 / quasars: individual: PG 1126−041 / ISM: jets and outflows / techniques: imaging spectroscopy / galaxies: ISM
The reduced datacubes are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/644/A15
© ESO 2020
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