Secular Evolution in Disk Galaxies

Kormendy, John

doi:10.48550/arxiv.1311.2609

Cited by 6 publications

(11 citation statements)

References 210 publications

(296 reference statements)

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“…Sellwood 2013; Kormendy 2013, for up to date reviews). After the initial instability responsible for the bar formation, the bar itself generally undergoes a thickening that can be either caused by a second "buckling" instability or by a vertical resonance (Sellwood 2013), possibly responsible for the pseudobulge formation (Kormendy 2013). In this scenario, the gas could accrete with a more disk like dynamics until the bar thickens, and fall toward the MBH with a higher velocity dispersion after the pseudobulge forms if the buckling instability and/or any vertical resonances significantly affect the gas motion.…”

Section: Discussionmentioning

confidence: 99%

“…The former are the result of major galactic mergers, which cause bursts of star formation (Daddi et al 2010;Genzel et al 2010), while the latter result from bar instabilities in galactic disks and undergo a slower, disk-like star formation (see, e.g. Kormendy 2013). In B12, both bar instabilities and major mergers were modeled, but star formation in the bulge component was the same irrespective of the bulge's formation mechanism.…”

Section: The Star Formation Modelmentioning

confidence: 99%

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Linking the Spin Evolution of Massive Black Holes to Galaxy Kinematics

Sesana

Barausse

Dotti

et al. 2014

ApJ

206

248

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We present the results of a semianalytical model that evolves the masses and spins of massive black holes together with the properties of their host galaxies along the cosmic history. As a consistency check, our model broadly reproduces a number of observations, e.g. the cosmic star formation history, the black hole mass and luminosity function and the galaxy mass function at low redshift, the black hole to bulge mass relation, and the morphological distribution at low redshift. For the first time in a semianalytical investigation, we relax the simplifying assumptions of perfect coherency or perfect isotropy of the gas fueling the black holes. The dynamics of gas is instead linked to the morphological properties of the host galaxies, resulting in different spin distributions for black holes hosted in different galaxy types. We compare our results with the observed sample of spin measurements obtained through broad Kα iron line fitting. The observational data disfavor both accretion along a fixed direction and isotropic fueling. Conversely, when the properties of the accretion flow are anchored to the kinematics of the host galaxy, we obtain a good match between theoretical expectations and observations. A mixture of coherent accretion and phases of activity in which the gas dynamics is similar to that of the stars in bulges (i.e., with a significant velocity dispersion superimposed to a net rotation) best describes the data, adding further evidence in support to the coevolution of massive black holes and their hosts.

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Section: Discussionmentioning

confidence: 99%

Section: The Star Formation Modelmentioning

confidence: 99%

Linking the Spin Evolution of Massive Black Holes to Galaxy Kinematics

Sesana

Barausse

Dotti

et al. 2014

ApJ

206

248

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“…Bars are also thought to be responsible for the build-up of the pseudo/disky bulges, whose nearly exponential profiles hints to a disk origin (e.g. Kormendy 2013, for a review). These structures are the most common type of bulges among galaxies in the stellar-mass range 10 9.5 M⊙ < M * < 10 10.5 M⊙, while classical bulges dominate among more massive systems (e.g.…”

mentioning

confidence: 99%

“…On longer timescales, the removal of the gas forced towards nuclear regions affects the star formation processes within the bar extent (Cheung et al 2013;Fanali et al 2015), contributing to the lowering of the specific star formation rate in the most massive spiral galaxies at low redshift (Cheung et al 2013;Gavazzi et al 2015a). In addition to the effect of the bar onto the inter stellar medium (ISM), the dynamical evolution of the bar itself is advocated to be responsible for the boxy/peanut-shaped stellar bulges (B/P bulges hereafter) (see Kormendy 2013;Sellwood 2014, for a review), observed in ∼ > 40% of edge on disk galaxies (e.g. Lütticke, Dettman & Pohlan 2000).…”

mentioning

confidence: 99%

“…Athanassoula 1992;Berentzen et al 1998;Regan & Teuben 2004;Berentzen et al 2007;Villa-Vargas, Shlosman & Heller 2010;Kim, Seo & Kim 2012;Cole et al 2014). Although these kind of simulations are extremely informing about the dynamical effect of bars, cosmological simulations are needed to follow bar formation within the hierarchical growth of galaxies (as discussed in, e.g., Kormendy 2013). Furthermore, most of the simulation literature on bar formation and evolution is based on collisionless simulations.…”

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confidence: 99%

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Bar-driven evolution and quenching of spiral galaxies in cosmological simulations

Spinoso

Bonoli

Dotti

et al. 2016

Mon. Not. R. Astron. Soc.

109

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We analyse the output of the hi-res cosmological "zoom-in" hydrodynamical simulation ErisBH to study self-consistently the formation of a strong stellar bar in a Milky Way-type galaxy and its effect on the galactic structure as well as on the central gas distribution and star formation. The simulation includes radiative cooling, star formation, SN feedback and a central massive black hole wich is undergoing gas accretion and is heating the surroundings via thermal AGN feedback. A large central region in the ErisBH disk becomes bar-unstable after z ∼ 1.4, but a clear bar-like structure starts to grow significantly only after z ≃ 0.4, possibly triggered by the interaction with a massive satellite. At z ≃ 0.1 the bar stabilizes and reaches its maximum radial extent of l ≈ 2.2 kpc. As the bar grows, it becomes prone to buckling instability, which we quantify based on the anisotropy of the stellar velocity dispersion. The actual buckling event is observable at z ≃ 0.1, resulting in the formation of a boxy-peanut bulge clearly discernible in the edge-on view of the galaxy at z = 0. The bar in ErisBH does not dissolve during the formation of the bulge but it is long-lived and is strongly non-axisymmetric down to the resolution limit of ∼ 100 pc at z = 0. During its early growth, the bar exerts a strong torque on the gas within its extent and drives gas inflows that enhance the nuclear star formation on sub-kpc scales. Later on, as the bar reaches its maximum length and strength, the infalling gas is nearly all consumed into stars and, to a lesser extent, accreted onto the central black hole, leaving behind a gasdepleted region within the central ∼ 2 kpc. Observations would more likely identify a prominent, large-scale bar at the stage when the galactic central region has already been quenched. Bar-driven quenching may play an important role in disk-dominated galaxies at all redshift. AGN feedback is instrumental in this scenario not because it directly leads to quenching, but because it promotes a strong bar by maintaining a flat rotation curve, suppressing the density of baryons within the central kpc in the early stages of the formation of the galaxy.

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Dissecting cosmological filaments at high redshifts: emergence of spaghetti-type flow inside DM haloes

Bi,

Shlosman,

Romano-Díaz

2023

Monthly Notices of the Royal Astronomical Society

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We use high-resolution zoom-in simulations to study the fueling of central galaxies by filamentary and diffuse accretion at redshifts, z ≳ 2. The parent haloes were chosen with similar total masses, log (Mvir/M⊙) ∼ 11.75 ± 0.05, at z = 6, 4, and 2, in high/low overdensity environments. We analyze the kinematic and thermodynamic properties of circumgalactic medium (CGM) within few virial radii, Rvir, and down to the central galaxy. Using a hybrid d-web/entropy method we mapped the gaseous filaments, and separated inflows from outflows. We find that (1) The CGM is multiphase and not in thermodynamic or dynamic equilibrium; (2) filamentary and diffuse accretion rates and densities decrease with lower redshifts, and inflow velocities decrease from 200 − 300 km s−1 by a factor of 2; (3) temperature within the filaments increases inside Rvir, faster at lower redshifts; (4) filaments show a complex structure along their spines: a core radial flow surrounded by a lower density envelope. The cores exhibit elevated densities and lower temperature, with no obvious metallicity gradient in the cross sections. Filaments also tend to separate into different infall velocity regions and split density cores, thus producing a spaghetti-type flow; (6) inside the inner ∼30 h−1 kpc, filaments develop the Kelvin-Helmholtz instability which ablates and dissolves them, and triggers turbulence along the filaments, clearly delineating their spines; (7) finally, the galactic outflows affect mostly the inner ∼0.5Rvir ∼ 100h−1kpc of the CGM.

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Secular Evolution in Disk Galaxies

Cited by 6 publications

References 210 publications

Linking the Spin Evolution of Massive Black Holes to Galaxy Kinematics

Linking the Spin Evolution of Massive Black Holes to Galaxy Kinematics

Bar-driven evolution and quenching of spiral galaxies in cosmological simulations

Dissecting cosmological filaments at high redshifts: emergence of spaghetti-type flow inside DM haloes

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