The host galaxies of X-ray selected active galactic nuclei to<i>z</i>= 2.5: Structure, star formation, and their relationships from CANDELS and<i>Herschel</i>/PACS

Rosario, D. J.; McIntosh, Daniel H.; Wel, Arjen van der; Kartaltepe, Jeyhan S.; Lang, P.; Santini, P.; Wuyts, Stijn; Lutz, D.; Rafelski, Marc; Villforth, C.; Alexander, D. M.; Bauer, F. E.; Bell, Eric F.; Berta, S.; Brandt, W. N.; Conselice, Christopher J.; Dekel, Avishai; Faber, S. M.; Ferguson, Henry C.; Genzel, R.; Grogin, Norman A.; Kocevski, Dale D.; Koekemoer, Anton M.; Koo, David C.; Lotz, Jennifer M.; Magnelli, B.; Maiolino, R.; Mozena, Mark; Mullaney, James; Papovich, Casey; Popesso, P.; Tacconi, L. J.; Trump, Jonathan R.; Avadhuta, S.; Bassett, Robert; Bell, A. R.; Bernyk, Maksym; Bournaud, F.; Cassata, P.; Cheung, Edmond; Croton, Darren J.; Donley, J. L.; DeGroot, Laura; Guedes, Javiera; Hathi, N. P.; Herrington, Jessica; Hilton, Matthew; Lai, Kamson; Lani, Caterina; Martig, Marie; McGrath, Elizabeth J.; Mutch, Simon J.; Mortlock, Alice; McPartland, Conor; O’Leary, Erin; Peth, Michael; Pillepich, Annalisa; Poole, Gregory B.; Snyder, D.; Straughn, Amber N.; Telford, O. Grace; Tonini, Chiara; Wandro, P.

doi:10.1051/0004-6361/201423782

Cited by 67 publications

(54 citation statements)

References 129 publications

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“…They find galaxies in the current state of a merger are ≈ 2-7 times more likely to contain a luminous AGN than their non-interacting counterparts. This quantitatively agrees with previous studies, who also find a noticeable enhancement in the fraction of AGN that reside in either close pairs or morphologically disturbed hosts above a control sample (e.g, Cotini et al 2013;Ellison et al 2011Ellison et al , 2013Ellison et al , 2015Koss et al 2010;Satyapal et al 2014;Rosario et al 2015;Koss et al 2018). Yet, again, many low-redshift studies also fail to find a distinction between the AGN fraction of interacting and non-interacting galaxies (e.g, Cisternas et al 2011;Villforth et al 2014;Hewlett et al 2017;Villforth et al 2017).…”

Section: Agn Luminositysupporting

confidence: 92%

Galaxy mergers in eagle do not induce a significant amount of black hole growth yet do increase the rate of luminous AGN

McAlpine

Harrison

Rosario

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We investigate the connection between galaxy-galaxy mergers and enhanced black hole (BH) growth using the cosmological hydrodynamical eagle simulation. We do this via three methods of analysis, investigating: the merger fraction of AGN, the AGN fraction of merging systems and the AGN fraction of galaxies with close companions. In each case, we find an increased abundance of AGN within merging systems relative to control samples of inactive or isolated galaxies (by up to a factor of ≈ 4 depending on the analysis method used), confirming that mergers are enhancing BH accretion rates for at least a subset of the galaxy population. The greatest excess of AGN triggered via a merger are found in lower mass (M * ∼ 10 10 M ) gas rich ( f gas > 0.1) central galaxies with lower mass BHs (M BH ∼ 10 7 M ) at lower redshifts (z < 1). We find no enhancement of AGN triggered via mergers in more massive galaxies (M * 10 11 M ). The enhancement of AGN is not uniform throughout the phases of a merger, and instead peaks within the early remnants of merging systems (typically lagging ≈ 300 Myr post-coalescence of the two galaxies at z = 0.5). We argue that neither major (4 ) are statistically relevant for enhancing BH masses globally. Whilst at all redshifts the galaxies experiencing a merger have accretion rates that are on average 2-3 times that of isolated galaxies, the majority of mass that is accreted onto BHs occurs outside the periods of a merger. We compute that on average no more than 15% of a BHs final day mass comes from the enhanced accretion rates triggered via a merger.

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Section: Agn Luminositysupporting

confidence: 92%

Galaxy mergers in eagle do not induce a significant amount of black hole growth yet do increase the rate of luminous AGN

McAlpine

Harrison

Rosario

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…In general, the fraction of the coeval galaxy population with major merger signatures is comparable to that found for the (majority of) distant AGNs, when the galaxy sample is matched in mass to the AGN sample; however, see Rosario et al (2014) for tentative evidence of a factor ≈ 2 decrease in the fraction of z = 0.5-1.0 galaxies with major-merger signatures when compared to the coeval AGN population. More significant differences are found by the present day, with a ≈ 5 times lower fraction of the galaxy population hosted in major mergers when compared to Swift-BAT selected AGNs (≈ 4% vs. ≈ 20%; Cotini et al 2013).…”

Section: Host-galaxy Morphologiessupporting

confidence: 50%

Cosmic X-ray surveys of distant active galaxies

Brandt

Alexander

2015

Astron Astrophys Rev

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314

227

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We review results from cosmic X-ray surveys of active galactic nuclei (AGNs) over the past ≈ 15 yr that have dramatically improved our understanding of growing supermassive black holes in the distant universe. First, we discuss the utility of such surveys for AGN investigations and the capabilities of the missions making these surveys, emphasizing Chandra, XMM-Newton, and NuSTAR. Second, we briefly describe the main cosmic X-ray surveys, the essential roles of complementary multiwavelength data, and how AGNs are selected from these surveys. We then review key results from these surveys on the AGN population and its evolution ("demographics"), the physical processes operating in AGNs ("physics"), and the interactions between AGNs and their environments ("ecology"). We conclude by describing some significant unresolved questions and prospects for advancing the field.

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“…The lack of evidence for merger-driven AGN growth in typical Seyfert-luminosity, X-ray selected AGNs (Sánchez et al 2004;Grogin et al 2005;Pierce et al 2007;Gabor et al 2009;Cisternas et al 2011b;Schawinski et al 2011;Kocevski et al 2012;Simmons et al 2012;Villforth et al 2014;Rosario et al 2015;Bruce et al 2016) can therefore be attributed to looking for mergers among the wrong population of AGNs/ hosts. By targeting luminous and heavily obscured AGNs using IR selection, we have selected exactly the sample of AGNs most likely to be merger driven, and indeed find evidence that the vast majority are heavily disturbed.…”

Section: Discussionmentioning

confidence: 99%

“…Studies of AGN hosts in the GEMS, GOODS, AEGIS, and COSMOS fields have predominantly targeted X-ray selected AGNs at z 0.2 1.3 < < (Sánchez et al 2004;Grogin et al 2005;Pierce et al 2007;Gabor et al 2009;Cisternas et al 2011b;Simmons et al 2012;Villforth et al 2014;Rosario et al 2015;Bruce et al 2016). While a small fraction of these AGN hosts show strong distortions, the rate of morphological disturbances is similar to that of inactive galaxy control samples, suggesting that mergers do not play a dominant role in AGN fueling, at least out to z 1 .…”

Section: Introductionmentioning

confidence: 99%

Evidence for Merger-driven Growth in Luminous, High-z, Obscured AGNs in the CANDELS/COSMOS Field

Donley

Kartaltepe

Kocevski

et al. 2018

ApJ

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWhile major mergers have long been proposed as a driver of both active galactic nucleus (AGN) activity and the M BH bulge s -relation, studies of moderate to high-redshift Seyfert-luminosity AGN hosts have found little evidence for enhanced rates of interactions. However, both theory and observation suggest that while these AGNs may be fueled by stochastic accretion and secular processes, high-luminosity, high-redshift, and heavily obscured AGNs are the AGNs most likely to be merger-driven. To better sample this population of AGNs, we turn to infrared selection in the CANDELS/COSMOS field. Compared to their lower-luminosity and less obscured X-ray-only counterparts, IR-only AGNs (luminous, heavily obscured AGNs) are more likely to be classified as either irregular (50 % ) to be classified either as interacting or merging in a way that significantly disturbs the host galaxy or as disturbed, though not clearly interacting or merging, which potentially represents the late stages of a major merger. This suggests that while major mergers may not contribute significantly to the fueling of Seyfertluminosity AGNs, interactions appear to play a more dominant role in the triggering and fueling of high-luminosity heavily obscured AGNs.

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The host galaxies of X-ray selected active galactic nuclei toz= 2.5: Structure, star formation, and their relationships from CANDELS andHerschel/PACS

Cited by 67 publications

References 129 publications

Galaxy mergers in eagle do not induce a significant amount of black hole growth yet do increase the rate of luminous AGN

Galaxy mergers in eagle do not induce a significant amount of black hole growth yet do increase the rate of luminous AGN

Cosmic X-ray surveys of distant active galaxies

Evidence for Merger-driven Growth in Luminous, High-z, Obscured AGNs in the CANDELS/COSMOS Field

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