The Role of Major Mergers and Nuclear Star Formation in Nearby Obscured Quasars

Zhao, Dongyao; Ho, Luis C.; Zhao, Yingnan; Shangguan, J.; Kim, Minjin

doi:10.3847/1538-4357/ab1921

Cited by 49 publications

(53 citation statements)

References 118 publications

(109 reference statements)

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“…A more detailed inspection shows that their model results in a more centrally peaked radial mass profile, with 2.5 times more mass in the inner 100 pc, reducing to a difference of ∼10 per cent at 500 pc and less than 1 per cent at distance larger than 1 kpc. In the case of Mrk 477, Zhao et al (2019) find a bulge mass 50 per cent larger than that of our two inner components, while our integrated mass is 2.5 times larger than theirs. The higher integrated mass can be attributed to our choice of mass-to-light ratio for the disc.…”

Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34contrasting

confidence: 73%

“…However, we find that their integrated mass distributions and radial mass profiles do not differ significantly from ours. In the case of Mrk 34, both galaxy models have the same mass, although Zhao et al (2019) find a bulge mass 2.5 times larger than ours. A more detailed inspection shows that their model results in a more centrally peaked radial mass profile, with 2.5 times more mass in the inner 100 pc, reducing to a difference of ∼10 per cent at 500 pc and less than 1 per cent at distance larger than 1 kpc.…”

Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34contrasting

confidence: 66%

“…It should be noted that a similar light profile decomposition done by Zhao et al (2019), on these same data, obtained structures with different parameters. Some of the differences between their results and ours are due to the fact that they adopt an exponential disc profile (Sérsic n = 1) and the use of a point spread function (PSF) model.…”

Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34mentioning

confidence: 57%

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Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Falcão

Kraemer

Fischer

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a dynamical study of the narrow-line regions in two nearby QSO2s. We construct dynamical models based on detailed photoionisation models of the emission-line gas, including the effects of internal dust, to apply to observations of large-scale outflows from these AGNs. We use Mrk 477 and Mrk 34 in order to test our models against recent HST STIS observations of [O III] emission-line kinematics, since these AGNs possess more energetic outflows than found in Seyfert galaxies. We find that the outflows within 500 pc are consistent with radiative acceleration of dusty gas, however the outflows in Mrk 34 are significantly more extended and may not be directly accelerated by radiation. We characterise the properties of X-ray winds found from the expansion of [O III]-emitting gas close to the black hole. We show that such winds possess the kinetic energy density to disturb [O III] gas at ∼ 1.8 kpc, and have sufficient energy to entrain the [O III] clouds at ∼ 1.2 kpc. Assuming that the X-ray wind possesses the same radial mass distribution as the [O III] gas, we find that the peak kinetic luminosity for this wind is 2 per cent of Mrk 34’s bolometric luminosity, which is in the 0.5 per cent - 5 per cent range required by some models for efficient feedback. Our work shows that, although the kinetic luminosity as measured from [O III]-emitting gas is frequently low, X-ray winds may provide more than one order of magnitude higher kinetic power.

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Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34contrasting

confidence: 73%

Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34contrasting

confidence: 66%

Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34mentioning

confidence: 57%

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Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Falcão

Kraemer

Fischer

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…15 This is not unexpected. AGNs in general and quasars in particular reside preferentially in bulge-dominated galaxies (Ho et al 1997;Ho 2008;Kim et al 2017;Zhao et al 2019), and bulgedominated systems tend to have higher molecular gas 13 For the purposes of this discussion, we exclude PG 1545+210, whose molecular gas mass and total gas mass are upper limits.…”

Section: Co-to-h 2 Conversion Factormentioning

confidence: 99%

An ALMA CO(2–1) Survey of Nearby Palomar–Green Quasars

Shangguan

Bauer

et al. 2020

ApJS

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The properties of the molecular gas can shed light on the physical conditions of quasar host galaxies and the effect of feedback from accreting supermassive black holes. We present a new CO(2-1) survey of 23 z < 0.1 Palomar-Green quasars conducted with the Atacama Large Millimeter/submillimeter Array. CO emission was successfully detected in 91% (21/23) of the objects, from which we derive CO luminosities, molecular gas masses, and velocity line widths. Together with CO(1-0) measurements in the literature for 32 quasars (detection rate 53%), there are 15 quasars with both CO(1-0) and CO(2-1) measurements and in total 40 sources with CO measurements. We find that the line ratio R 21 ≡ L CO(2-1) /L CO(1-0) is subthermal, broadly consistent with nearby galaxies and other quasars previously studied. No clear correlation is found between R 21 and the intensity of the interstellar radiation field or the luminosity of the active nucleus. As with the general galaxy population, quasar host galaxies exhibit a strong, tight, linear L IR -L CO(1-0) relation, with a normalization consistent with that of starburst systems. We investigate the molecular-to-total gas mass fraction with the aid of total gas masses inferred from dust masses previously derived from infrared observations. Although the scatter is considerable, the current data do not suggest that the CO-to-H 2 conversion factor of quasar host galaxies significantly differs from that of normal star-forming galaxies.

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“…BHs evidently do not require bulges to form (Ho 2008). Further, the mere existence of disk-dominated active galaxies (e.g., Cisternas et al 2011;Kim et al 2017;Zhao et al 2019) implies that BHs can grow by internal secular processes alone.…”

Section: Introductionmentioning

confidence: 99%

A New Channel of Bulge Formation via the Destruction of Short Bars

Guo

et al. 2020

ApJ

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Short (inner) bars of sub-kiloparsec radius have been hypothesized to be an important mechanism for driving gas inflows to small scales, thus feeding central black holes. Recent numerical simulations have shown that the growth of central black holes in galaxies can destroy short bars, when the black hole reaches a mass of ∼ 0.1% of the total stellar mass of the galaxy. We study N -body simulations of galaxies with single and double bars to track the long-term evolution of the central stellar mass distribution. We find that the destruction of the short bar contributes significantly to the growth of the bulge. The final bulge mass is roughly equal to the sum of the masses of the initial pseudo bulge and short bar. The initially boxy/peanut-shaped bulge of Sérsic index n 1 is transformed into a more massive, compact structure that bears many similarities to a classical bulge, in terms of its morphology (n ≈ 2), kinematics (dispersion-dominated, isotropic), and location on standard scaling relations (Kormendy relation, mass-size relation, and correlations between black hole mass and bulge stellar mass and velocity dispersion). Our proposed channel for forming classical bulges relies solely on the destruction of short bars without any reliance on mergers. We suggest that some of the less massive, less compact classical bulges were formed in this manner.

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The Role of Major Mergers and Nuclear Star Formation in Nearby Obscured Quasars

Cited by 49 publications

References 118 publications

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

An ALMA CO(2–1) Survey of Nearby Palomar–Green Quasars

A New Channel of Bulge Formation via the Destruction of Short Bars

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