On the slow quenching of M* galaxies: feeding the heart on the way to taming the beast. (arXiv:1812.05216v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Moutard_T/0/1/0/all/0/1">Thibaud Moutard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malavasi_N/0/1/0/all/0/1">Nicola Malavasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sawicki_M/0/1/0/all/0/1">Marcin Sawicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnouts_S/0/1/0/all/0/1">Stéphane Arnouts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tripathi_S/0/1/0/all/0/1">Shruti Tripathi</a>
We investigate the connection between X-ray and radio-loud optically-obscured
AGNs and the physical properties of their evolved and massive host galaxies,
focussing on the mass-related quenching channel followed by $mathcal{M}^star
(simeq 10^{10.6} M_odot)$ galaxies in the rest-frame NUVrK colour diagram.
While our results confirm (1) radio-loud AGNs to be mostly hosted by
already-quenched and massive ($M_*>10^{11}M_odot$) galaxies, ruling out their
feedback as primary driver of $mathcal{M}^star$ galaxy quenching, we found
(2) heavily-obscured X-ray AGNs to be mostly hosted by $mathcal{M}^star$
galaxies in the process of quenching. This argues for a quenching scenario that
enables mergers of (gas-poor) $mathcal{M}^star$ galaxies $after$ they have
left the star formation main sequence, i.e., after the onset of quenching
process. In that respect, we discuss how our results support a scenario where
the slow quenching of $mathcal{M}^star$ galaxies happens along cosmic
filaments.
We investigate the connection between X-ray and radio-loud optically-obscured
AGNs and the physical properties of their evolved and massive host galaxies,
focussing on the mass-related quenching channel followed by $mathcal{M}^star
(simeq 10^{10.6} M_odot)$ galaxies in the rest-frame NUVrK colour diagram.
While our results confirm (1) radio-loud AGNs to be mostly hosted by
already-quenched and massive ($M_*>10^{11}M_odot$) galaxies, ruling out their
feedback as primary driver of $mathcal{M}^star$ galaxy quenching, we found
(2) heavily-obscured X-ray AGNs to be mostly hosted by $mathcal{M}^star$
galaxies in the process of quenching. This argues for a quenching scenario that
enables mergers of (gas-poor) $mathcal{M}^star$ galaxies $after$ they have
left the star formation main sequence, i.e., after the onset of quenching
process. In that respect, we discuss how our results support a scenario where
the slow quenching of $mathcal{M}^star$ galaxies happens along cosmic
filaments.
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