Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching

Suh, Hyewon; Civano, F.; Hasinger, G.; Lusso, Elisabeta; Lanzuisi, G.; Marchesi, S.; Trakhtenbrot, Benny; Allevato, V.; Cappelluti, N.; Capak, P.; Elvis, M.; Griffiths, R. E.; Laigle, C.; Lira, P.; Riguccini, L.; Rosario, D. J.; Salvato, M.; Schawinski, Kevin; Vignali, C.

doi:10.3847/1538-4357/aa725c

Cited by 42 publications

(65 citation statements)

References 112 publications

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“…It provides a sample of obscured AGNs which is complementary to a Compton-thick AGN sample selected purely by X-ray observations. Suh et al (2017) found that X-ray type-2 AGN hosts have similar SFRs compared to the normal star-forming galaxies. In this paper, we confirmed this result with our X-ray selected sample, and showed that IR-selected AGN hosts are not significant different from or slightly above the star-forming sequence.…”

Section: Visual Classificationmentioning

confidence: 95%

Infrared Selection of Obscured Active Galactic Nuclei in the COSMOS Field

Chang

Floc’h

Juneau

et al. 2017

ApJS

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We present a study of the connection between black hole accretion, star formation, and galaxy morphology at z ≤ 2.5. We focus on active galactic nuclei (AGNs) selected by their mid-IR power-law emission. By fitting optical to far-IR photometry with state-of-the-art spectral energy distribution (SED) techniques, we derive stellar masses, star formation rates, dust properties, and AGN contributions in galaxies over the whole COSMOS field. We find that obscured AGNs lie within or slightly above the star-forming sequence. We confirm our previous finding about compact host galaxies of obscured AGNs at z ∼ 1, and find that galaxies with 20-50% AGN contributions tend to have smaller sizes, by ∼25-50%, compared to galaxies without AGNs. Furthermore, we find that a high merger fraction of up to 0.5 is appropriate for the most luminous (log(L IR /L ) ∼ 12.5) AGN hosts and non-AGN galaxies, but not for the whole obscured AGN sample. Moreover, merger fraction depends on the total and star-forming infrared luminosity, rather than the decomposed AGN infrared luminosity. Our results suggest that major mergers are not the main driver of AGN activity, and therefore obscured AGNs might be triggered by internal mechanisms, such as secular processes, disk instabilities, and compaction in a particular evolutionary stage. We make the SED modeling results publicly available.

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Section: Visual Classificationmentioning

confidence: 95%

Infrared Selection of Obscured Active Galactic Nuclei in the COSMOS Field

Chang

Floc’h

Juneau

et al. 2017

ApJS

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“…The typical uncertainties for the stellar mass are +0.19 dex and −0.36 dex toward higher and lower masses, respectively. A full detailed description is presented in Suh et al (2017Suh et al ( , 2019.…”

Section: Host Stellar Massmentioning

confidence: 99%

No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

Suh

Civano

Trakhtenbrot

et al. 2020

ApJ

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We investigate the cosmic evolution of the ratio between black hole mass (M BH ) and host galaxy total stellar mass (M stellar ) out to z ∼ 2.5 for a sample of 100 X-ray-selected moderate-luminosity, broad-line active galactic nuclei (AGNs) in the Chandra-COSMOS Legacy Survey. By taking advantage of the deep multi-wavelength photometry and spectroscopy in the COSMOS field, we measure in a uniform way the galaxy total stellar mass using a SED decomposition technique and the black hole mass based on broad emission line measurements and single-epoch virial estimates. Our sample of AGN host galaxies has total stellar masses of 10 10−12 M ⊙ , and black hole masses of 10 7.0−9.5 M ⊙ . Combining our sample with the relatively bright AGN samples from the literature, we find no significant evolution of the M BH − M stellar relation with black hole-to-host total stellar mass ratio of M BH /M stellar ∼ 0.3% at all redshifts probed. We conclude that the average black hole-to-host stellar mass ratio appears to be consistent with the local value within the uncertainties, suggesting a lack of evolution of the M BH − M stellar relation up to z ∼ 2.5.

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“…more common in more massive galaxies (e.g. Silverman et al 2009;Aird et al 2013;Bongiorno et al 2012;Suh et al 2017;Georgakakis et al 2017;Yang et al 2018) 3 . However, amongst X-ray emitters in the CDFS (which we remind is the deepest of the two fields) we find a non negligible tail of low-mass, M * ∼ < 10 9 M , AGN whose relative contribution becomes more and more prominent as the mass of the host galaxy is lowered.…”

Section: % 75%mentioning

confidence: 99%

The role of galaxy mass on AGN emission: a view from the VANDELS survey

Magliocchetti

Pentericci

Cirasuolo

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a comparative analysis of the properties of AGN emitting at radio and X-ray wavelengths. The study is performed on 907 X-ray AGN and 100 radio AGN selected on the CDFS and UDS fields and makes use of new and ancillary data available to the VANDELS collaboration. Our results indicate that the mass of the host galaxy is a fundamental quantity which determines the level of AGN activity at the various wavelengths. Indeed large stellar masses are found to be connected with AGN radio emission, as virtually all radio-active AGN reside within galaxies of M * > 10 10 M . Large stellar masses also seem to favour AGN activity in the X-ray, even though X-ray AGN present a mass distribution which is more spread out and with a non-negligible tail at M * ∼ < 10 9 M . Stellar mass alone is also observed to play a fundamental role in simultaneous radio and X-ray emission: the percentage of AGN active at both wavelengths increases from around 1% of all X-ray AGN residing within hosts of M * < 10 11 M to ∼ 13% in more massive galaxies. In the case of radio-selected AGN, such a percentage moves from ∼ 15% to ∼ 45% (but up to ∼ 80% in the deepest fields). Neither cosmic epoch, nor radio luminosity, X-ray luminosity, Eddington ratio or starformation rate of the hosts are found to be connected to an enhanced probability for joint radio+X-ray emission of AGN origin. Furthermore, only a loose relation is observed between X-ray and radio luminosity in those AGN which are simultaneously active at both frequencies.

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Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching

Cited by 42 publications

References 112 publications

Infrared Selection of Obscured Active Galactic Nuclei in the COSMOS Field

Infrared Selection of Obscured Active Galactic Nuclei in the COSMOS Field

No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

The role of galaxy mass on AGN emission: a view from the VANDELS survey

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