We report on the first ALMA observation of the CO(3-2) and rest-frame ∼340 GHz continuum emission in PDS 456, which is the most luminous, radio-quiet QSO in the local Universe (z 0.18), with a bolometric luminosity LBol ∼ 1047 erg s-1. ALMA angular resolution allowed us to map scales as small as ∼700 pc. The molecular gas reservoir traced by the core of the very bright CO(3-2) emission line is distributed in a compact rotating disk, with a size of ∼1.3 kpc, seen close to face-on (i ∼ 25 deg). Fast CO(3-2) emission in the velocity range v [1000, 500] km s-1 is also present. Specifically, we detect several blue-shifted clumps out to ∼5 kpc from the nucleus, in addition to a compact (R 1.2 kpc), broad emission component. These components reveal a galaxy-wide molecular outflow, with a total mass Mmolout ∼2.5 × 108 M (for an αCO = 0.8 M (K km s-1 pc2)-1) and a mass outflow rate mol ∼290 M yr-1. The corresponding depletion time is τdep ∼ 8 Myr, shorter than the rate at which the molecular gas is converted into stars, indicating that the detected outflow is potentially able to quench star-formation in the host. The momentum flux of the molecular outflow normalised to the radiative momentum output (i.e. LBol/c) is 1, comparable to that of the X-ray ultra-fast outflow (UFO) detected in PDS 456. This is at odds with the expectations for an energy-conserving expansion suggested for most of the large-scale outflows detected in low-luminosity AGNs so far. We suggest three possible scenarios that may explain this observation: (i) in very luminous AGNs such as our target the molecular gas phase is tracing only a fraction of the total outflowing mass; (ii) a small coupling between the shocked gas by the UFO and the host-galaxy interstellar medium (ISM); and (iii) AGN radiation pressure may be playing an important role in driving the outflow.

The gentle monster PDS 456: Kiloparsec-scale molecular outflow and its implications for QSO feedback

Piconcelli E.;Feruglio C.;Carniani S.;Cicone C.;Bongiorno A.;Maiolino R.;Marconi A.;
2019

Abstract

We report on the first ALMA observation of the CO(3-2) and rest-frame ∼340 GHz continuum emission in PDS 456, which is the most luminous, radio-quiet QSO in the local Universe (z 0.18), with a bolometric luminosity LBol ∼ 1047 erg s-1. ALMA angular resolution allowed us to map scales as small as ∼700 pc. The molecular gas reservoir traced by the core of the very bright CO(3-2) emission line is distributed in a compact rotating disk, with a size of ∼1.3 kpc, seen close to face-on (i ∼ 25 deg). Fast CO(3-2) emission in the velocity range v [1000, 500] km s-1 is also present. Specifically, we detect several blue-shifted clumps out to ∼5 kpc from the nucleus, in addition to a compact (R 1.2 kpc), broad emission component. These components reveal a galaxy-wide molecular outflow, with a total mass Mmolout ∼2.5 × 108 M (for an αCO = 0.8 M (K km s-1 pc2)-1) and a mass outflow rate mol ∼290 M yr-1. The corresponding depletion time is τdep ∼ 8 Myr, shorter than the rate at which the molecular gas is converted into stars, indicating that the detected outflow is potentially able to quench star-formation in the host. The momentum flux of the molecular outflow normalised to the radiative momentum output (i.e. LBol/c) is 1, comparable to that of the X-ray ultra-fast outflow (UFO) detected in PDS 456. This is at odds with the expectations for an energy-conserving expansion suggested for most of the large-scale outflows detected in low-luminosity AGNs so far. We suggest three possible scenarios that may explain this observation: (i) in very luminous AGNs such as our target the molecular gas phase is tracing only a fraction of the total outflowing mass; (ii) a small coupling between the shocked gas by the UFO and the host-galaxy interstellar medium (ISM); and (iii) AGN radiation pressure may be playing an important role in driving the outflow.
2019
Settore FIS/05 - Astronomia e Astrofisica
Galaxies: active; Galaxies: evolution; Quasars: emission lines; Quasars: individual: PDS 456; Techniques: imaging spectroscopy; Techniques: interferometric
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11384/89786
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