The Bulgeless Seyfert/Liner Galaxy NGC 3367: Disk, Bar, Lopsidedness, and Environment

Hernández-Toledo, H. M.; Cano-Díaz, M.; Valenzuela, O.; Puerari, I.; García-Barreto, J. A.; Moreno-Díaz, Edmundo; Bravo-Alfaro, H.

doi:10.1088/0004-6256/142/6/182

Cited by 6 publications

(6 citation statements)

References 85 publications

(118 reference statements)

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“…Our model with a more dominant disk (S.FeMu−Bar) presents a different evolution compared with the S.FeMu. As all the simulated cases, the gas rich-disk fragments generating clumps, but the model also develops relatively soon a large scale bar-like structure, similar to that observed in some barred galaxies with a clumpy stellar distribution (Hernández-Toledo et al 2011). The gas distribution and motion is affected by this bar triggering an inflow, which in turn weakens the large scale bar.…”

Section: Multi-channel Bulge Formationsupporting

confidence: 77%

Clumpy disc and bulge formation

Pérez¹,

Valenzuela²,

Tissera³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We present a set of hydrodynamical/Nbody controlled simulations of isolated gas rich galaxies that self-consistently include SN feedback and a detailed chemical evolution model, both tested in cosmological simulations. The initial conditions are motivated by the observed star forming galaxies at z ∼ 2-3. We find that the presence of a multiphase interstellar media in our models promotes the growth of disc instability favouring the formation of clumps which in general, are not easily disrupted on timescales compared to the migration time. We show that stellar clumps migrate towards the central region and contribute to form a classical-like bulge with a Sersic index, n > 2. Our physicallymotivated Supernova feedback has a mild influence on clump survival and evolution, partially limiting the mass growth of clumps as the energy released per Supernova event is increased, with the consequent flattening of the bulge profile. This regulation does not prevent the building of a classical-like bulge even for the most energetic feedback tested. Our Supernova feedback model is able to establish a self-regulated star formation, producing mass-loaded outflows and stellar age spreads comparable to observations. We find that the bulge formation by clumps may coexit with other channels of bulge assembly such as bar and mergers. Our results suggest that galactic bulges could be interpreted as composite systems with structural components and stellar populations storing archaeological information of the dynamical history of their galaxy.

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Section: Multi-channel Bulge Formationsupporting

confidence: 77%

Clumpy disc and bulge formation

Pérez¹,

Valenzuela²,

Tissera³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…For the Seyfert Sc galaxy NGC 3367 (McAlpine et al 2011), Dong & De Robertis (2006) report a K-band bulge magnitude of −21.6 mag, corresponding to a bulge-tototal flux ratio of 0.08. Hernández-Toledo et al (2011) find that the bulge has a Sérsic index between 1 and 1.8, and after including a bar in their image analysis they report a bulge-to-disc ratio of 0.07 to 0.11. The bulge magnitude from Dong & De Robertis (2006), after brightening it by 0.11 mag for dust (Driver et al 2008), yields an expected black hole mass of log M bh /M ⊙ = 6.2 ± 0.9.…”

Section: Individual Galaxiesmentioning

confidence: 95%

THEM_BH-L_SPHEROIDRELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES

Graham¹,

Scott²

2013

ApJ

257

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From a sample of 72 galaxies with reliable supermassive black hole masses M bh , we derive the M bh -(host spheroid luminosity, L) relation for i) the subsample of 24 core-Sérsic galaxies with partially depleted cores, and ii) the remaining subsample of 48 Sérsic galaxies. Using K s -band Two Micron All Sky Survey data, we find the near-linear relation M bh ∝ L 1.10±0.20 Ks for the core-Sérsic spheroids thought to be built in additive dry merger events, while M bh ∝ L 2.73±0.55 Ks for the Sérsic spheroids built from gas-rich processes. After converting literature B-band disk galaxy magnitudes into inclinationand dust-corrected bulge magnitudes, via a useful new equation presented herein, we obtain a similar result. Unlike with the M bh -(velocity dispersion) diagram, which is also updated here using the same galaxy sample, it remains unknown whether barred and non-barred Sérsic galaxies are offset from each other in the M bh -L diagram.While black hole feedback has typically been invoked to explain what was previously thought to be a nearly constant M bh /M Spheroid mass ratio of ∼0.2%, we advocate that the near-linear M bh -L and M bh -M Spheroid relations observed at high masses may have instead largely arisen from the additive dry merging of galaxies. We argue that feedback results in a dramatically different scaling relation, such that black hole mass scales roughly quadratically with the spheroid mass in Sérsic galaxies. We therefore introduce a revised cold-gas 'quasar' mode feeding equation for semi-analytical models to reflect what we dub the quadratic growth of black holes in Sérsic galaxies built amidst gas-rich processes. Finally, we use our new Sérsic M bh -L equations to predict the masses of candidate intermediate mass black holes in almost 50 low luminosity spheroids containing active galactic nuclei, finding many masses between that of stellar mass black holes and supermassive black holes.

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“…The UNAM-KIAS not only adds a significant number of new isolated galaxies at v < 10,000 km s −1 vindicating some previously presumed non-isolated cases lacking radial velocity information (e.g., Hernández-Toledo et al 2010), but becomes a natural extension of the CIG for v > 10,000 km s −1 up to a bit more than 20,000 km s −1 . It is therefore hoped that any joint study of the properties of these isolated galaxies will necessarily add more statistical significance and deeper insight to the origin of such galaxies.…”

Section: Selection Criteriamentioning

confidence: 79%

The Unam-Kias Catalog of Isolated Galaxies

Hernández-Toledo¹,

Vázquez-Mata²,

Martínez-Vázquez³

et al. 2010

The Astronomical Journal

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A new catalog of isolated galaxies from the Sloan Digital Sky Survey Data Release 5 (SDSS DR5) is presented. A total of 1520 isolated galaxies were found in 1.4 sr of sky. The selection criteria in this UNAM-KIAS catalog are a variation on the criteria developed by Karachentseva, including full redshift information. Through an image processing pipeline that takes advantage of the high-resolution (∼0. 4 pixel −1 ) and high dynamic range of the SDSS images, a uniform g-band morphological classification for all these galaxies is presented. We identify 80% (Sa-Sm) spirals (50% later than Sbc types) on one hand, and a scarce population of early-type E (6.5%) and S0 (8%) galaxies amounting to 14.5% on the other hand. This magnitude-limited catalog is ∼80% complete at 16.5, 15.6, 15.2, 14.6, and 14.4 mag in the ugriz bands, respectively. Some representative physical properties including SDSS magnitudes and color distributions, color-color diagrams, absolute magnitude-color, and concentration-color diagrams as a function of morphological type are presented. The UNAM-KIAS Morphological Atlas is also released along with this paper. For each galaxy of a type later than Sa, a mosaic is presented that includes (1) a g-band logarithmic image, (2) a g-band filtered-enhanced image where a Gaussian kernel of various sizes was applied, and (3) a red giant branch color image from the SDSS database. For E/S0/Sa galaxies, in addition to the images in (1), (2), and (3), plots of r-band surface brightness and geometric profiles (ellipticity , position angle PA, and A 4 /B 4 coefficients of the Fourier series expansions of deviations of a pure ellipse) are provided. The size of the sample, the redshift completeness, the availability of high-quality multicolor photometric data and detailed morphological and spectroscopic information make the UNAM-KIAS catalog of isolated galaxies a suitable sample to address important issues such as (1) comparative studies of environmental effects, (2) constraining the currently competing scenarios of galaxy formation and evolution, (3) the nature and evolution of elliptical and spiral galaxies in the field, (4) the spectral properties of a statistically significant number of isolated galaxies and their evolution as a function of redshift, and (5) the fraction of active galactic nuclei in isolated environments, among other important topics. The optimization and estimation of new structural parameters as well as important information to complement existing ones in other wavelengths is being carried out.

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The Bulgeless Seyfert/Liner Galaxy NGC 3367: Disk, Bar, Lopsidedness, and Environment

Cited by 6 publications

References 85 publications

Clumpy disc and bulge formation

Clumpy disc and bulge formation

THEM_BH-L_SPHEROIDRELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES

The Unam-Kias Catalog of Isolated Galaxies

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The Bulgeless Seyfert/Liner Galaxy NGC 3367: Disk, Bar, Lopsidedness, and Environment

Cited by 6 publications

References 85 publications

Clumpy disc and bulge formation

Clumpy disc and bulge formation

THEMBH-LSPHEROIDRELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES

The Unam-Kias Catalog of Isolated Galaxies

Contact Info

Product

Resources

About

THEM_BH-L_SPHEROIDRELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES