Internal kinematics of modelled interacting disc galaxies

Kronberger, T.; Kapferer, W.; Schindler, S.; Böhm, A.; Kutdemir, Elif; Ziegler, B.

doi:10.1051/0004-6361:20064976

Cited by 29 publications

(47 citation statements)

References 35 publications

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“…Notice that the final remnants are in all cases dominated by random motion. Similar kinematic features have been seen in other simulations of fast galaxy encounters in the literature (see Kronberger et al 2006). The kinematical characteristics of the models with simulated tidal stripping (GST1 and GST2) do not differ much from similar simulations without tidal stripping (TID1 and TID2).…”

Section: Tidally Induced Barssupporting

confidence: 87%

On the origin of dwarf elliptical galaxies: the fundamental plane

Aguerri¹,

González-García

2008

A&A

108

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Context. Early-type dwarf (dE) galaxies are the most common type of galaxies observed in the Universe. Their study has important cosmological implications because according to hierarchical galaxy evolution theories they are the progenitors of brighter galaxies. Nevertheless, the origin of this kind of system is still not well understood. Aims. The aim of the present work is to investigate whether the different locations of dwarf galaxies with respect to ellipticals in the face-on view of the fundamental plane could be due to the transformation of bright disc galaxies in low-mass systems by harassment. Methods. We have run high-resolution N-body numerical simulations to test the tidal stripping scenario of dE galaxies. The present simulations modelled several individual tidal stripping events in initial disc-like galaxy models with different bulge-to-disc mass ratios.Results. The models have shown that tidal stripping is a very efficient mechanism for removing stars and dark matter particles from galaxies, specially from their outer parts. The particles of the disc and halo components were easily stripped, while the bulge particles were not. Thus, the scale length of the discs were 40−50% shorter than the initial ones. Prograde tidal interactions create tidal features like stable bars in the discs of the galaxies. In contrast, bars are inhibited in retrograde encounters. After several tidal interactions the galaxy remnants looks like a dwarf spheroidal system. The final position of the low-mass systems in the face-on view of the fundamental plane (FP) depends on the initial conditions of the simulations. Thus, simulated galaxies with initial large B/D ratios are closer to the face-on view of the fundamental plane defined by bright E and bulges of early-type galaxies. Nevertheless, galaxies with initially small B/D ratio are located, after four fast tidal encounters, at the position of dE galaxies in the face-on view of the fundamental plane.The final position of the remnants in the FP do not depend on the orbital configuration of the encounters. Conclusions. We conclude that fast galaxy-galaxy interactions are efficient mechanisms of transforming bright galaxies into dwarf ones. Indeed, the different location observed between Es and dEs in the face-on view of the fundamental plane can be explained by the formation of dwarf galaxies by harassment of late-type bright ones.

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Section: Tidally Induced Barssupporting

confidence: 87%

On the origin of dwarf elliptical galaxies: the fundamental plane

Aguerri¹,

González-García

2008

A&A

108

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“…In fact, tidal forces perturb the global gas motions and can cause local velocity increases, leading to an over-estimate of the dynamical mass. They also increase the velocity dispersion of the individual clouds (Mihos & Hernquist 1996;Kronberger et al 2006) and the turbulence of the ISM (Elmegreen et al 1993). Last but not least, the rather small widths of the individual HI and CO lines towards VCC 2062, of about 20 km s −1 for the HI component (FWHM) and 15 km s −1 (FWHM) for the CO component, rather indicate that the local gas is not very perturbed or at least has had time to settle down.…”

Section: 22)mentioning

confidence: 99%

VCC 2062: an old tidal dwarf galaxy in the Virgo cluster?

Duc¹,

Braine

Lisenfeld

et al. 2007

A&A

103

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Context. Numerical simulations predict the existence of old Tidal Dwarf Galaxies (TDGs) that would have survived several Gyr after the collision lying at their origin. Such survivors, which would by now have become independent relaxed galaxies, would be ideal laboratories, if nearby enough, to tackle a number of topical issues, including the distribution of Dark Matter in and around galaxies. However finding old dwarf galaxies with a confirmed tidal origin is an observational challenge. Aims. A dwarf galaxy in the nearby Virgo Cluster, VCC 2062, exhibits several unusual properties that are typical of a galaxy made out of recycled material. We discuss whether it may indeed be a TDG. Methods. We analysed multi-wavelength observations of VCC 2062, including a CO map acquired with the IRAM 30 m dish, an optical spectrum of its HII regions, GALEX ultraviolet and archival broad-band and narrow-band optical images as well as a VLA HI datacube, originally obtained as part of the VIVA project. Results. VCC 2062 appears to be the optical, low surface brightness counterpart of a kinematically detached, rotating condensation that formed within an HI tail apparently physically linked to the disturbed galaxy NGC 4694. In contrast to its faint optical luminosity, VCC 2062 is characterised by strong CO emission and a high oxygen abundance more typical of spiral disks. Its dynamical mass however, is that of a dwarf galaxy. Conclusions. VCC 2062 was most likely formed within a pre-enriched gaseous structure expelled from a larger galaxy as a result of a tidal interaction. The natural provider for the gaseous tail is NGC 4694 or rather a former companion which subsequently has been accreted by the massive galaxy. According to that scenario, VCC 2062 has been formed by a past tidal encounter. Since its parent galaxies have most probably already totally merged, it qualifies as an old Tidal Dwarf Galaxy.

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“…with mass ratios > 7:1, see Hernquist 1992;Eliche-Moral et al 2006;Kronberger et al 2006;Sarzi et al 2015). Thus, a possible way to distinguish among these formation processes is by analysing the kinematics of spirals and S0s.…”

Section: Introductionmentioning

confidence: 99%

Formation of S0 galaxies through mergers

Tapia

Eliche‐Moral

Aceves

et al. 2017

A&A

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Context. Lenticular (S0) galaxies are known to derive from spiral galaxies. The fact that S0s nearly obey the Tully-Fisher relation (TFR) at z ∼ 0 (as spirals have done in the last ∼9 Gyr) is considered an argument against their major-merger origin because equal mergers of two disc galaxies produce remnants that are outliers of the TFR. Aims. We explore whether a scenario that combines an origin by mergers at z ∼ 1.8 − 1.5 with a subsequent passive evolution of the resulting S0 remnants since z ∼ 0.8-1 is compatible with observational data of S0s in the TFR both at z ∼ 0.8 and z ∼ 0. Methods. We studied a set of major and minor merger experiments from the GalMer database that generate massive S0 remnants that are dynamically relaxed and have realistic properties. We analysed the location of these remnants in the photometric and stellar TFRs assuming that they correspond to z ∼ 0.8 galaxies. We then estimated their evolution in these planes over the last ∼ 7 Gyr considering that they have evolved passively in isolation. The results were compared with data of real S0s and spirals at different redshifts. We also tested how the use of V circ or V rot,max affects the results. Results. Just after ∼ 1-2 Gyr of coalescence, major mergers generate S0 remnants that are outliers of the local photometric and stellar TFRs (as already stated in previous studies), in good agreement with observations at z ∼ 0.8. After ∼ 4 -7 Gyr of passive evolution in isolation, the S0 remnants move towards the local TFR, although the initial scatter among them persists. This scatter is sensitive to the indicator used for the rotation velocity: V circ values yield a lower scatter than when V rot,max values are considered instead. In the planes involving V rot,max , a clear segregation of the S0 remnants in terms of the spin-orbit coupling of the model is observed, in which the remnants of retrograde encounters overlap with local S0s hosting counter-rotating discs. The location of the S0 remnants at z ∼ 0 agrees well with the observed distribution of local S0 galaxies in the σ 0 -M K , V circ -σ 0 , and V rot,max -σ 0 planes. Conclusions. Massive S0 galaxies may have been formed through major mergers that occurred at high redshift and have later evolved towards the local TFR through passive evolution in relative isolation, a mechanism that would also contribute to the scatter observed in this relation.

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Internal kinematics of modelled interacting disc galaxies

Cited by 29 publications

References 35 publications

On the origin of dwarf elliptical galaxies: the fundamental plane

On the origin of dwarf elliptical galaxies: the fundamental plane

VCC 2062: an old tidal dwarf galaxy in the Virgo cluster?

Formation of S0 galaxies through mergers

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