Secular Evolution and the Growth of Pseudobulges in Disk Galaxies

Kormendy, John; Cornell, Mark E.

doi:10.1007/978-1-4020-2862-5_24

Cited by 14 publications

(8 citation statements)

References 72 publications

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“…The corresponding median lines suggest that the most massive galaxies are bulge-dominated (e.g., Baldry et al 2004;Wilman & Erwin 2012;Nair & Abraham 2010), while the majority of normal galaxies are disk-dominated (e.g., Fukugita et al 2007;Bamford et al 2009;Nair & Abraham 2010); a behaviour which is consistent with observational studies. The large scatter in (2,1) suggests that in a few galaxies pseudobulges dominate the total stellar mass budget, hence leading to the development of lenticular galaxies (Kormendy & Kennicutt 2004;Kormendy & Cornell 2004;Weinzirl et al 2009;Vaghmare et al 2013). Interestingly, there are a some extreme cases where the pseudo-bulge-to-total stellar mass ratio is as high as 0.9.…”

Section: Stars-mmentioning

confidence: 99%

Morphological evolution and galactic sizes in the L-Galaxies SA model

Irodotou

Thomas

Henriques

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In this work we update the L-Galaxies semi-analytic model (SAM) to better follow the physical processes responsible for the growth of bulges via disk instabilities (leading to pseudo-bulges) and mergers (leading to classical bulges), showing the impact of these processes on the fractional breakdown of our galaxies into different morphological types, and obtaining an excellent fit to the morphology-mass relation. We find that an accurate match to the observed correlation between stellar disk scale length and mass at z ∼ 0.0 requires that the gas loses 20% of its initial specific angular momentum to the corresponding dark matter halo during the formation of the cold gas disk. With this assumption, we reproduce the observed trends between the stellar mass and specific angular momentum for both disk-and bulge-dominated galaxies, with latetype galaxies rotating faster than early-types of the same mass. We include dissipation of energy in gas-rich mergers, thus reducing the merger remnant sizes, which allows us to match the observed mass-size relation for bulge-dominated systems. Finally, we present the baryonic Tully-Fisher relation for gas-and disk-dominated galaxies, and find that our trend agrees well with the present-day observational constraints. ∆ ì J gas = δ ì J gas,cooling + δ ì J gas,SF + δ ì J gas,acc.

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Section: Stars-mmentioning

confidence: 99%

Morphological evolution and galactic sizes in the L-Galaxies SA model

Irodotou

Thomas

Henriques

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…It is important to compare results from different methods for measuring BH masses, because such comparisons can provide insight into potential systematic errors for each method (Siopis et al 2009;Kormendy 2004;Humphrey et al 2009;Greene et al 2010). Comparing optically measured dynamical BH masses with those from the H 2 O megamaser method is especially valuable, since the megamaser galaxies with Keplerian rotation curves provide the most direct and accurate BH mass measurements for external galaxies, These maser BH masses can be used to test the more commonly used BH mass measuring techniques in the optical, such as the stellar or gas dynamical methods.…”

Section: Other Bh Mass Measuring Techniquesmentioning

confidence: 99%

“…Over the past two decades, there has been substantial progress in detecting BHs and constraining their masses, especially in quiescent or mildly active nearby galaxies (Kormendy & Richstone 1995;Kormendy & Gebhardt 2001;Kormendy 2004;Ferrarese & Ford 2005). This rapid progress was mainly facilitated by the high angular resolution provided by the Hubble Space Telescope (HST) and by gradually maturing techniques for modeling stellar dynamics of galaxies.…”

Section: Introductionmentioning

confidence: 99%

The Megamaser Cosmology Project. Iii. Accurate Masses of Seven Supermassive Black Holes in Active Galaxies With Circumnuclear Megamaser Disks

Kuo

Braatz

Condon

et al. 2010

ApJ

279

340

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Observations of H 2 O masers from circumnuclear disks in active galaxies for the Megamaser Cosmology Project allow accurate measurement of the mass of supermassive black holes (BH) in these galaxies. We present the Very Long Baseline Interferometry (VLBI) images and kinematics of water maser emission in six active galaxies: NGC 1194, NGC 2273, NGC 2960 (Mrk 1419), NGC 4388, NGC 6264 and NGC 6323. We use the Keplerian rotation curves of these six megamaser galaxies, plus a seventh previously published, to determine accurate enclosed masses within the central ∼ 0.3 pc of these galaxies, smaller than the radius of the sphere of influence of the central mass in all cases. We also set lower limits to the central mass densities of between 0.12 and 60 ×10 10 M ⊙ pc −3 . For six of the seven disks, the high central densities rule out clusters of stars or stellar remnants as the central objects, and this result further supports our assumption that the enclosed mass can be attributed predominantly to a supermassive black hole. The seven BHs have masses ranging between 0.76 and 6.5×10 7 M ⊙ . The BH mass errors are ≈ 11%, dominated by the uncertainty of the Hubble constant. We compare the megamaser BH mass determination with other BH mass measurement techniques. The BH mass based on virial estimation in four galaxies is consistent with the megamaser BH mass given the latest empirical value of f , but the virial mass uncertainty is much greater. Circumnuclear megamaser disks allow the best mass determination of the central BH mass in external galaxies and significantly improve the observational basis at the low-mass end of the M − σ ⋆ relation. The M − σ ⋆ relation may not be a single, low-scatter power law as originally proposed. MCP observations continue and we expect to obtain more maser BH masses in the future.

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“…Galaxies can evolve via internal processes, such as the formation of bars or spiral arms, as in secular evolution (Courteau et al 1996;Kormendy et al 2004;Kormendy & Ho 2013;Sellwood 2014;Combes 2014;Méndez-Abreu et al 2014), or via cataclysmic external processes, as in interactions with other galaxies (Toomre & Toomre 1972;Barnes & Hernquist 1996). Indeed, interactions between gas rich galaxies is a very efficient way of perturbing a system and introducing more gas into the environment.…”

Section: Introductionmentioning

confidence: 99%

SDSS-FIRST-selected interacting galaxies

Misquitta

Eckart

Yttergren

2023

A&A

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Context. In the hierarchical model of evolution of the Universe, galaxy mergers play an important role, especially at high redshifts. Interactions among galaxies appear to be associated with incidences of radio-loudness in quasars and it is of interest to study the galaxies that are in the process of interacting with each other, where there is at least one nucleus that is active in the radio regime. Aims. In order to understand the various processes taking place within colliding galaxies, it is important to study the radio and optical properties of these sources, as well as any possible correlations that might exist. Methods. To this end, we present optical long-slit spectroscopy data for ten pairs of interacting galaxies selected from SDSS-FIRST at redshifts of ∼0.05, observed using the multi-object double spectrographs at the Large Binocular Telescope. Results. We used line fluxes extracted from the spectra of the nuclear regions of galaxies to plot optical diagnostic diagrams and estimate the masses of the central supermassive black holes, as well as their Eddington ratios. Additionally, we used previously published Effelsberg radio telescope data at 4.85 GHz and FIRST survey data at 1.4 GHz to estimate radio spectral slopes and the radio-loudness parameters for all of the radio-detected sources. We also used WISE data to plot a mid-infrared colour-colour diagram. Conclusions. We see that while the sample of galaxies covers all of the classes on the optical diagnostic diagrams, the sources that are radio-detected fall in the composite or transition region of the diagram. Additionally, we notice a trend of the highest radio-loudness parameter in a pair of interacting galaxies being associated with the galaxy that hosts the more massive central supermassive black hole. We do not see any obvious trends with respect to the radio spectral slope, radio-loudness parameter, and Eddington ratio. With respect to the mid-infrared data of the galaxies detected by WISE, we see that most of them have some type of contribution from star formation, however, two of them seem to have a significant contribution from an AGN as well.

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Secular Evolution and the Growth of Pseudobulges in Disk Galaxies

Cited by 14 publications

References 72 publications

Morphological evolution and galactic sizes in the L-Galaxies SA model

Morphological evolution and galactic sizes in the L-Galaxies SA model

The Megamaser Cosmology Project. Iii. Accurate Masses of Seven Supermassive Black Holes in Active Galaxies With Circumnuclear Megamaser Disks

SDSS-FIRST-selected interacting galaxies

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