Morphology of 15 Southern Early?Type Disk Galaxies

Laurikainen, Eija; Salo, H.; Buta, Ronald J.; Knapen, Johan H.; Speltincx, T.; Block, David L.

doi:10.1086/508810

Cited by 102 publications

(139 citation statements)

References 86 publications

(92 reference statements)

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“…Curiously, another observational result compatible with a dry minor merger evolution is the high fraction of pseudobulges found in S0's (Laurikainen et al 2005(Laurikainen et al , 2006(Laurikainen et al , 2007. Note that the S0's resulting from our dry minor mergers have n < ∼ 2 and B/T < 0.4.…”

Section: Discussionsupporting

confidence: 54%

Evolution along the sequence of S0 Hubble types induced by dry minor mergers

Eliche‐Moral

González–García

Aguerri

et al. 2012

A&A

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Context. Recent studies have argued that galaxy mergers are not important drivers for the evolution of S0's, on the basis that mergers cannot preserve the coupling between the bulge and disk scale-lengths observed in these galaxies and the lack of correlation of their ratio with the S0 Hubble type. However, about 70% of present-day S0's reside in groups, an environment where mergers and tidal interactions dominate galaxy evolution. Aims. We investigate whether the remnants resulting from collision-less N-body simulations of intermediate and minor mergers onto S0 galaxies evolve fulfilling global structural relations observed between the bulges and disks of these galaxies. Methods. Different initial bulge-to-disk ratios of the primary S0 have been considered, as well as different satellite densities, mass ratios, and orbits of the encounter. We have analysed the final morphology of the remnants in images simulating the typical observing conditions of S0 surveys. We derive bulge+disk decompositions of the final remnants to compare their global bulge-to-disk structure with observations. Results. We show that all remnants present undisturbed S0 morphologies according to the prescriptions of specialized surveys. The dry intermediate and minor mergers induce noticeable bulge growth (S0c−→S0b and S0b−→S0a), but affect negligibly to the bulge and disk scale-lengths. Therefore, if a coupling between these two components exists prior to the merger, the encounter does not break this coupling. This fact provides a simple explanation for the lack of correlation between the ratio of bulge and disk scale-lengths and the S0 Hubble type reported by observations. Conclusions. These models prove that dry intermediate and minor mergers can induce global structural evolution within the sequence of S0 Hubble types compatible with observations, meaning that these processes should not be discarded from the evolutionary scenarios of S0's just on the basis of the strong coupling observed between the bulge and disk scale-lengths in these galaxies.

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Section: Discussionsupporting

confidence: 54%

Evolution along the sequence of S0 Hubble types induced by dry minor mergers

Eliche‐Moral

González–García

Aguerri

et al. 2012

A&A

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“…Bulges of early-type spirals, however, appear more exponential than previously assumed (Balcells et al 2003;Laurikainen et al 2005). Furthermore, lower values of B/T than in earlier studies have been reported (Laurikainen et al 2005(Laurikainen et al , 2006(Laurikainen et al , 2007Weinzirl et al 2009). The reason for the observed lower mean values of n and B/T is most likely related to the multicomponent decomposition used (Laurikainen et al 2005(Laurikainen et al , 2007: the omission of bars (and ovals/lenses) leads to modifying bulge (mostly) and disk parameters and furthermore to B/T inflation (see also Gadotti 2008;Weinzirl et al 2009).…”

Section: Introductionmentioning

confidence: 53%

Optical multiband surface photometry of a sample of Seyfert galaxies

Slavcheva-Mihova

Mihov

2010

A&A

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Context. Parallel analysis of the large-scale morphology and local environment of matched active and control galaxy samples plays an important role in studies of the fueling of active galactic nuclei. Aims. We carry out a detailed morphological characterization of a sample of 35 Seyfert galaxies and a matched sample of inactive galaxies in order to compare the evidence of non-axisymmetric perturbation of the potential and, in the second part of this paper, to be able to perform a multicomponent photometric decomposition of the Seyfert galaxies. Methods. We constructed contour maps, BVR C I C profiles of the surface brightness, ellipticity, and position angle, as well as colour index profiles. We further used colour index images, residual images, and structure maps, which helped clarify the morphology of the galaxies. We studied the presence of close companions using literature data. Results. By straightening out the morphological status of some of the objects, we derived an improved morphological classification and built a solid basis for a further multicomponent decomposition of the Seyfert sample. We report hitherto undetected (to our knowledge) structural components in some Seyfert galaxies -a bar (Ark 479), an oval/lens (Mrk 595), rings (Ark 120, Mrk 376), a nuclear bar and ring (Mrk 352), and nuclear dust lanes (Mrk 590). We compared the large-scale morphology and local environment of the Seyfert sample to those of the control one and found that (1) the two samples show similar incidences of bars, rings, asymmetries, and close companions; (2) the Seyfert bars are generally weaker than the bars of the control galaxies; (3) the bulk of the two samples shows morphological evidence of non-axisymmetric perturbations of the potential or close companions; (4) the fueling of Seyfert nuclei is not directly related to the large-scale morphology and local environment of their host galaxies.

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“…Most commonly I other describes light from a bar, but could also refer to rings, nuclei, or bright star forming spiral arms. Not taking a bar into account when modeling the light profile leads to systematic effects, such as overestimating the bulge-to-total ratio (B/T ) by as much as a factor of two, and also systematically overestimating the value of the Sérsic index (Gadotti, 2008;Fisher & Drory, 2008;Laurikainen et al, 2006). If the galaxy has a central point source, either AGN or nucleus, this must be accounted for as well or else the returned model will have an artificially large Sérsic index and B/T .…”

Section: Structural Properties Of Bulges: Sérsic Index Scalingmentioning

confidence: 99%

An Observational Guide to Identifying Pseudobulges and Classical Bulges in Disc Galaxies

Fisher¹,

Drory²

2016

Astrophysics and Space Science Library

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In this review our aim is to summarize the observed properties of pseudobulges and classical bulges. We utilize an empirical approach to studying the properties of bulges in disk galaxies, and restrict our analysis to statistical properties. A clear bimodality is observed in a number of properties including morphology, structural properties, star formation, gas content & stellar population, and kinematics. We conclude by summarizing those properties that isolate pseudobulges from classical bulges. Our intention is to describe a practical, easy to use, list of criteria for identifying bulge types.

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Morphology of 15 Southern Early?Type Disk Galaxies

Cited by 102 publications

References 86 publications

Evolution along the sequence of S0 Hubble types induced by dry minor mergers

Evolution along the sequence of S0 Hubble types induced by dry minor mergers

Optical multiband surface photometry of a sample of Seyfert galaxies

An Observational Guide to Identifying Pseudobulges and Classical Bulges in Disc Galaxies

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