AGN in Dusty Starbursts at Z=2: Feedback Still To Kick In. (arXiv:1905.06955v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rodighiero_G/0/1/0/all/0/1">G. Rodighiero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Enia_A/0/1/0/all/0/1">A. Enia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delvecchio_I/0/1/0/all/0/1">I. Delvecchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lapi_A/0/1/0/all/0/1">A. Lapi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magdis_G/0/1/0/all/0/1">G. E. Magdis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rujopakarn_W/0/1/0/all/0/1">W. Rujopakarn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mancini_C/0/1/0/all/0/1">C. Mancini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Munoz_L/0/1/0/all/0/1">L. Rodriguez-Munoz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carraro_R/0/1/0/all/0/1">R. Carraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iani_E/0/1/0/all/0/1">E. Iani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Negrello_M/0/1/0/all/0/1">M. Negrello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franceschini_A/0/1/0/all/0/1">A. Franceschini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Renzini_A/0/1/0/all/0/1">A. Renzini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruppioni_C/0/1/0/all/0/1">C. Gruppioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perna_M/0/1/0/all/0/1">M. Perna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baronchelli_I/0/1/0/all/0/1">I. Baronchelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puglisi_A/0/1/0/all/0/1">A. Puglisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassata_P/0/1/0/all/0/1">P. Cassata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daddi_E/0/1/0/all/0/1">E. Daddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morselli_L/0/1/0/all/0/1">L. Morselli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverman_J/0/1/0/all/0/1">J. Silverman</a>

We investigate a sample of 152 dusty sources at 1:5 < z < 2:5 to understand the connection of enhanced Star-Formation-Rate (SFR) and Black-Hole-Accretion-Rate (BHAR). The sources are Herschel-selected, having stellar masses M*>10^10Msun and SFR (100-1000Msun/yr) elevated(>4?) above the
star-forming “main sequence”, classifying them as Starbursts (SB). Through a
multiwavelength fitting approach (including a dusty torus component), we
divided the sample into active SBs (dominated by an AGN emission, SBs-AGN, ?
23% of the sample) and purely star-forming SBs (SBs-SFR). We visually inspected
their HST/UV-restframe maps: SBs-SFR are generally irregular and composite
systems; ? 50% of SBs-AGN are instead dominated by regular compact
morphologies. We then found archival ALMA continuum counterparts for 33
galaxies (12 SBs-AGN and 21 SBs-SFR). For these sources we computed dust
masses, and, with standard assumptions, we also guessed total molecular
gas-masses. SBs turn to be gas rich systems (fgas = Mgas=Mgas/(Mgas+M*) sim
20%-70%), and the gas fractions of the two SB classes are very similar (fgas =
43 +/-4% and fgas = 42+/- 2%). Our results show that SBs are consistent with a
mixture of: 1) highly star-forming merging systems (dominating the SBs-SFR),
and 2) primordial galaxies, rapidly growing their M* together with their Black
Hole (mainly the more compact SBs-AGN). Anyway, feedback effects have not
reduced their fgas yet. Indeed, SBs at z = 2, with relatively low bolometric
AGN luminosities in the range 10^44 < Lbol(AGN) < 10^46 erg/s (compared to bright optical and X-ray quasars), are still relatively far from the epoch when the AGN feedback will quench the SFR in the host and will substantially depress the gas fractions.

We investigate a sample of 152 dusty sources at 1:5 < z < 2:5 to understand
the connection of enhanced Star-Formation-Rate (SFR) and
Black-Hole-Accretion-Rate (BHAR). The sources are Herschel-selected, having
stellar masses M*>10^10Msun and SFR (100-1000Msun/yr) elevated(>4?) above the
star-forming “main sequence”, classifying them as Starbursts (SB). Through a
multiwavelength fitting approach (including a dusty torus component), we
divided the sample into active SBs (dominated by an AGN emission, SBs-AGN, ?
23% of the sample) and purely star-forming SBs (SBs-SFR). We visually inspected
their HST/UV-restframe maps: SBs-SFR are generally irregular and composite
systems; ? 50% of SBs-AGN are instead dominated by regular compact
morphologies. We then found archival ALMA continuum counterparts for 33
galaxies (12 SBs-AGN and 21 SBs-SFR). For these sources we computed dust
masses, and, with standard assumptions, we also guessed total molecular
gas-masses. SBs turn to be gas rich systems (fgas = Mgas=Mgas/(Mgas+M*) sim
20%-70%), and the gas fractions of the two SB classes are very similar (fgas =
43 +/-4% and fgas = 42+/- 2%). Our results show that SBs are consistent with a
mixture of: 1) highly star-forming merging systems (dominating the SBs-SFR),
and 2) primordial galaxies, rapidly growing their M* together with their Black
Hole (mainly the more compact SBs-AGN). Anyway, feedback effects have not
reduced their fgas yet. Indeed, SBs at z = 2, with relatively low bolometric
AGN luminosities in the range 10^44 < Lbol(AGN) < 10^46 erg/s (compared to
bright optical and X-ray quasars), are still relatively far from the epoch when
the AGN feedback will quench the SFR in the host and will substantially depress
the gas fractions.

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