Active Galactic Nuclei in Dusty Starbursts at z = 2: Feedback Still to Kick in

Rodighiero, G.; Enia, A.; Delvecchio, I.; Lapi, A.; Magdis, G.; Rujopakarn, W.; Mancini, C.; Rodríguez-Muñoz, L.; Carraro, R.; Iani, Edoardo; Negrello, M.; Franceschini, A.; Renzini, A.; Gruppioni, C.; Perna, M.; Baronchelli, Ivano; Puglisi, A.; Cassata, P.; Daddi, Emanuele; Morselli, L.; Silverman, John D.

doi:10.3847/2041-8213/ab222e

Cited by 13 publications

(15 citation statements)

References 54 publications

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“…starbursts) are even more efficient at triggering AGNs. Similar to our results, Rodighiero et al (2019) find higher BHARs in starbursts, with a factor of 3 enhancement compared to normal star-forming galaxies for a sample of 1.5<z<2.5 galaxies with a great diversity of star-forming properties. In their Figure 3, they present predictions of an enhancement of BHAR and BHAR/SFR during the merger phase based on the hydrodynamical models of Di and Hopkins et al (2012), which is in agreement with our findings (see Table 1).…”

Section: Discussionsupporting

confidence: 90%

Galaxy mergers up to z < 2.5 II: AGN incidence of merging galaxies at separations of 3-15 kpc

Silva,

Marchesini,

Silverman

et al. 2021

Preprint

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Section: Discussionsupporting

confidence: 90%

Galaxy mergers up to z < 2.5 II: AGN incidence of merging galaxies at separations of 3-15 kpc

Silva,

Marchesini,

Silverman

et al. 2021

Preprint

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“…Despite the large scatter of one order of magnitude or more among different studies, the H 2 mass density parameter Ω H 2 is observed to increase at z ≃ 0-3, assembling its mass with almost no observed environmental dependence (Darvish et al 2018;Tadaki et al 2019;Garratt et al 2021), and has been found to mimic the cosmological star formation rate (SFR) density at higher z (Decarli et al 2020;Riechers et al 2020a). These observations highlight the longstanding need to explore the origin of the large supply of H 2 gas required to sustain star formation at different z (Rodighiero et al 2019;Tacconi et al 2020;Hunt et al 2020) and question the ability to explain the large H 2 fractions (above 50%) detected in galaxies around z ∼ 4-6 (Dessauges-Zavadsky et al 2020;Boogaard et al 2021) in a primordial, presumably metal-poor gas. From a theoretical point of view, cold gas plays a key role in cooling and fragmentation.…”

Section: Introductionmentioning

confidence: 99%

Atomic and molecular gas from the epoch of reionisation down to redshift 2

Maio

Péroux

Ciardi

2022

A&A

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Context. Cosmic gas makes up about 90% of the baryonic matter in the Universe and H2 molecule is the most tightly linked to star formation. Aims. In this work we study cold neutral gas, its H2 component at different epochs, and corresponding depletion times. Methods. We perform state-of-the-art hydrodynamic simulations that include time-dependent atomic and molecular non-equilibrium chemistry coupled to star formation, feedback effects, different UV backgrounds presented in the recent literature and a number of additional processes occurring during structure formation (COLDSIM). We predict gas evolution and contrast the mass density parameters and gas depletion timescales. We also investigate their relation to cosmic expansion in light of the latest infrared and (sub)millimetre observations in the redshift range 2 ≲ z ≲ 7. Results. By performing updated non-equilibrium chemistry calculations we are able to broadly reproduce the latest HI and H2 observations. We find neutral-gas mass density parameters Ωneutral ≃ 10−3 and increasing from lower to higher redshift, in agreement with available HI data. Because of the typically low metallicities during the epoch of reionisation, time-dependent H2 formation is mainly led by the H− channel in self-shielded gas, while H2 grain catalysis becomes important in locally enriched sites at any redshift. Ultraviolet (UV) radiation provides free electrons and facilitates H2 build-up while heating cold metal-poor environments. Resulting H2 fractions can be as high as ∼50% of the cold gas mass at z ∼ 4–8, in line with the latest measurements from high-redshift galaxies. The H2 mass density parameter increases with time until a plateau of ΩH2 ≃ 10−4 is reached. Quantitatively, we find agreement between the derived ΩH2 values and the observations up to z ∼ 7 and both HI and H2 trends are better reproduced by our non-equilibrium H2-based star formation modelling. The predicted gas depletion timescales decrease at lower z in the whole time interval considered, with H2 depletion times remaining below the Hubble time and comparable to the dynamical time at all z. This implies that non-equilibrium molecular cooling is efficient at driving cold-gas collapse in a broad variety of environments and has done so since very early cosmic epochs. While the evolution of chemical species is clearly affected by the details of the UV background and gas self shielding, the assumptions on the adopted initial mass function, different parameterizations of H2 dust grain catalysis, photoelectric heating, and cosmic-ray heating can affect the results in a non-trivial way. In the Appendix, we show detailed analyses of individual processes, as well as simple numerical parameterizations and fits to account for them. Conclusions. Our findings suggest that, in addition to HI, non-equilibrium H2 observations are pivotal probes for assessing cold-gas cosmic abundances and the role of UV background radiation at different epochs.

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“…This picture might suggest that just like the majority of galaxies follow a main-sequence in the SFR-M * plane, a similar relation between the black hole accretion rate (BHAR) and the M * might exist: the more massive the galaxy, the higher the availability of inflowing gas for star formation and black hole accretion, which would mean that they both should correlate with stellar mass. In addition, galaxies offset from the mainsequence (starbursts and quiescents), might have a BHAR that varies accordingly with the gas that is typically available in that phase (Rodighiero et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

Carraro

Rodighiero

Cassata

et al. 2020

A&A

Self Cite

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Aims. We study the coevolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different phases of galaxy life: main-sequence star-forming galaxies, quiescent galaxies, and starburst galaxies at different cosmic epochs. Methods. We exploited the unique combination of depth and area in the COSMOS field and took advantage of the X-ray data from the Chandra COSMOS-Legacy survey and the extensive multiwavelength ancillary data presented in the COSMOS2015 catalog, including in particular the UVista Ultra-deep observations. These large datasets allowed us to perform an X-ray stacking analysis and combine it with detected sources in a broad redshift interval (0.1 < z < 3.5) with unprecedented statistics for normal star-forming, quiescent, and starburst galaxies. The X-ray luminosity was used to predict the black holeAR, and a similar stacking analysis on far-infrared Herschel maps was used to measure the corresponding obscured SFR for statistical samples of sources in different redshifts and stellar mass bins. Results. We focus on the evolution of the average SFR-stellar mass (M*) relation and compare it with the BHAR-M* relation. This extends previous works that pointed toward the existence of almost linear correlations in both cases. We find that the ratio between BHAR and SFR does not evolve with redshift, although it depends on stellar mass. For the star-forming populations, this dependence on M* has a logarithmic slope of ∼0.6 and for the starburst sample, the slope is ∼0.4. These slopes are both at odds with quiescent sources, where the dependence remains constant (log(BHAR/SFR) ∼ −3.4). By studying the specific BHAR and specific SFR, we find signs of downsizing for M* and black hole mass (MBH) in galaxies in all evolutionary phases. The increase in black hole mass-doubling timescale was particularly fast for quiescents, whose super-massive black holes grew at very early times, while accretion in star-forming and starburst galaxies continued until more recent times. Conclusions. Our results support the idea that the same physical processes feed and sustain star formation and black hole accretion in star-forming galaxies while the starburst phase plays a lesser role in driving the growth of the supermassive black holes, especially at high redshift. Our integrated estimates of the M* − MBH relation at all redshifts are consistent with independent determinations of the local M* − MBH relation for samples of active galactic nuclei. This adds key evidence that the evolution in the BHAR/SFR is weak and its normalization is relatively lower than that of local dynamical M* − MBH relations.

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Active Galactic Nuclei in Dusty Starbursts at z = 2: Feedback Still to Kick in

Cited by 13 publications

References 54 publications

Galaxy mergers up to z < 2.5 II: AGN incidence of merging galaxies at separations of 3-15 kpc

Galaxy mergers up to z < 2.5 II: AGN incidence of merging galaxies at separations of 3-15 kpc

Atomic and molecular gas from the epoch of reionisation down to redshift 2

Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

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