SUPER V. ALMA continuum observations of z~2 AGN and the elusive evidence of outflows influencing star formation

Abstract

We study the impact of active galactic nuclei (AGN) ionised outflows on star formation in high-redshift AGN host galaxies, by combining near-infrared integral field spectroscopic (IFS) observations, mapping the Hα emission and [O iii]λ5007 outflows, with matched-resolution observations of the rest-frame far-infrared (FIR) emission. We present high-resolution ALMA Band 7 observations of eight X-ray selected AGN (L 2−10 keV = 10 43.8 − 10 45.2 erg s −1 ) at z ∼ 2 from the SUPER (SINFONI Survey for Unveiling the Physics and Effect of Radiative feedback) sample, targeting the observed-frame 870 µm (rest-frame ∼ 260 µm) continuum at ∼ 2 kpc (0.2") spatial resolution. The targets were selected among the SUPER AGN with an [O iii] detection in the IFS maps and with a detection in the FIR photometry. We detected six out of eight targets with signal-to-noise ratio S/N 10 in the ALMA maps, from which we measured continuum flux densities in the range 0.27 − 2.58 mJy and FIR half-light radii (R e ) in the range 0.8 − 2.1 kpc. The other two targets were detected with S/N of 3.6 and 5.9, which are insufficient for spatially resolved analysis. The FIR R e of our sample are comparable to other AGN and star-forming galaxies at a similar redshift from the literature. However, combining our sample with the literature samples, we find that the mean FIR size in X-ray AGN (R e = 1.16 ± 0.11 kpc) is slightly smaller than in non-AGN (R e = 1.69 ± 0.13 kpc). From spectral energy distribution (SED) fitting, we find that the main contribution to the 260 µm flux density is dust heated by star formation, with ≤ 4% contribution from AGN-heated dust and ≤ 1% from synchrotron emission. The majority of our sample show different morphologies for the FIR (mostly due to reprocessed stellar emission) and the ionised gas emission (Hα and [O iii], mostly due to AGN emission). This could be due to the different locations of dust and ionised gas, the different sources of the emission (stars and AGN), or the effect of dust obscuration. We are unable to identify any residual Hα emission, above that dominated by AGN, that could be attributed to star formation. Under the assumption that the FIR emission is a reliable tracer of obscured star formation, we find that the obscured star formation activity in these AGN host galaxies is not clearly affected by the ionised outflows. However, we cannot rule out that star formation suppression is happening on smaller spatial scales than the ones we probe with our observations (< 2 kpc) or on different timescales.

Evidence of extended cold molecular gas and dust haloes around z ~ 2.3 extremely red quasars with ALMA

“…The CO(7-6), [C ] and H 2 O sizes are consistent with CO sizes measured by Chen et al (2017); Calistro Rivera et al (2018) and [C ] sizes measured by ALPINE survey (Fujimoto et al 2020) and Hot Dust Obscured Galaxies (Hot DOGs; Scholtz et al in prep). The median FIR sizes of our sample agree with those found in AGN host galaxies (Harrison et al 2016;Scholtz et al 2020;Lamperti et al 2021;Scholtz et al 2021), Hot DOGs (Scholtz et al, in prep) and sub-mm and star-forming galaxies (e.g. Ikarashi et al 2015;Simpson et al 2015;Hodge et al 2016;Spilker et al 2016;Tadaki et al 2017;Fujimoto et al 2018;Lang et al 2019;Chen et al 2020), however, the range of the values is a factor of ∼1.5 higher than those found in submm and AGN host galaxies.…”