Galaxy transmutations: The double ringed galaxy ESO 474-G26

Решетников, В. П.; Bournaud, F.; Combes, F.; Faúndez-Abans, M.; Oliveira-Abans, M. de; Driel, W. van; Schneider, S. E.

doi:10.1051/0004-6361:20041756

Cited by 11 publications

(27 citation statements)

References 25 publications

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“…Another possible driver is merging, as suggested by the existence of many ICs exhibiting strong misalignments or distorted morphologies and/or kinematics with respect to the host disc (see, e.g., Okumura et al 1994;Arnaboldi et al 1995b;Buta & Combes 1996;Barnes & Hernquist 1996;Knapen et al 2004;Reshetnikov et al 2005;Mazzuca et al 2006;Sil'Chenko & Moiseev 2006;Chilingarian et al 2009;Faúndez-Abans et al 2009;Moiseev & Bizyaev 2009;Brosch et al 2010). This scenario is supported by numerical simulations, which have proven that major mergers can drive the formation of kinematicallydecoupled ICs analogous to the ones found in E-S0 galaxies (Hernquist & Barnes 1991;Balcells & González 1998;Bendo & Barnes 2000;Barnes 2001;Jesseit et al 2007;Di Matteo et al 2008).…”

Section: Introductionmentioning

confidence: 99%

A minor merger origin for stellar inner discs and rings in spiral galaxies

Eliche‐Moral

González-García

Balcells

et al. 2011

A&A

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Context. Observations have shown that inner discs and rings (IDs and IRs) are not preferably found in barred galaxies, which indicates that their formation may differ from that described by the traditional bar-origin scenario in many cases. In contrast, the role of minor mergers in producing these inner components (ICs), while often invoked, is still poorly understood. Aims. We investigate the capability of minor mergers to trigger the formation of IDs and IRs in spiral galaxies through collisionless N-body simulations. Methods. We run a battery of minor merger simulations in which both primary and secondary galaxies are modelled as disc-bulgehalo galaxies with realistic density ratios. Different orbits and mass ratios are considered, as well as two different models for the primary galaxy (a Sab or Sc). We then perform a detailed analysis of the morphology, structure, and kinematics of the ICs resulting from the minor merger. Results. All the simulated minor mergers develop thin ICs out of satellite material, supported by rotation. A wide morphological zoo of ICs are obtained (including IDs, IRs, pseudo-rings, nested IDs, spiral patterns, and combinations of them), but all have structural and kinematical properties similar to those observed. The sizes of the resulting ICs are comparable to those observed in real galaxies with the adequate scaling. The existence of the resulting ICs can be deduced from the features that they imprint in the isophotal profiles and kinemetric maps of the final remnant, as in many real galaxies. Weak transitory oval distortions appear in the remnant centre in many cases, but none of them develops a noticeable bar. The realistic density ratios used in the present models ensure that the satellites experience more efficient orbital circularization and disruption than in previous studies. Combined with the disc resonances induced by the encounter, these processes produce highly aligned co-and counter-rotating ICs at the remnant centre. Conclusions. Minor mergers are an efficient mechanism for forming rotationally-supported stellar ICs in spiral galaxies, without requiring either strong dissipation or the development of noticeable bars. The present models indicate that minor mergers can account for the existence of pure-stellar old ICs in unbarred galaxies, and suggest that their role must have been crucial in the formation of ICs and much more complex than just bar triggering.

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Section: Introductionmentioning

confidence: 99%

A minor merger origin for stellar inner discs and rings in spiral galaxies

Eliche‐Moral

González-García

Balcells

et al. 2011

A&A

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“…This is a mass ratio for which Bournaud et al 2005 found stable and long‐lived polar or high‐inclined rings of gas, returning to the galaxy along tidal tails, and equatorial rings, that appears as ‘dust lanes’ when they are seen edge‐on. Such unequal‐mass merger has been proven to be the most likely scenario for another peculiar galaxy: the double‐ring ESO 474‐G26 (Reshetnikov et al 2005).…”

Section: Discussionmentioning

confidence: 99%

“…However, other types of interactions, such as smooth accretion and stripping, seem to be equally important in the growth of galaxies and the relative weights of the various processes depend on the environment, which drive many morphological features observed in galaxies, such as bars, shells (see Malin & Carter 1980) and highly inclined or even counter‐rotating rings/discs (see Galletta 1996 for a review). Concerning the latter morphology, different degrees of evolution of these peculiar rings/discs are seen: in some cases, the decoupled matter is composed by stars and gas, and regions of recent star formation are also observed (Iodice et al 2002a,b; Reshetnikov et al 2005); other cases show rings with a particularly smooth structure (Iodice et al 2004), or formed only by gas (Bettoni et al 2001). In general, these peculiar galaxies have very large amount of gas (Richter, Sackett & Sparke 1994; Galletta, Sage & Sparke 1997) and dust which lies in the same plane of the decoupled ring/disc (e.g.…”

Section: Introductionmentioning

confidence: 99%

Revisiting the formation history of the minor-axis dust lane galaxy NGC 1947

Spavone

Iodice

Calvi

et al. 2009

Monthly Notices of the Royal Astronomical Society

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In this paper, we present a detailed study of the peculiar early‐type galaxy NGC 1947. The main goal of this work is to constrain the dynamical status and the formation history of NGC 1947 by comparing the observed properties with the predictions derived from different galaxy formation scenarios. To this aim, we derived the photometric and kinematical properties of NGC 1947. Due to the presence of an extended dust lane, which crosses the galaxy centre along the photometric minor axis, we used near‐infrared (NIR) images (J and K bands) to derive an accurate analysis of the stellar light distribution. Optical images (in the V and R bands) are used to derive the colour profiles and colour maps to study the structure of the dust lane. The observed kinematics confirm the presence of two components with decoupled angular momentum: gas and dust rotate along the minor axis, while the rotation velocities of the stars are observed along the major axis. The complex structure observed in NGC 1947 supports the hypothesis that some kind of interactions happened in the evolution of this object. We analysed two alternatives: a merging process and an accretion event. We discussed how the observed properties strongly suggest that the decoupled ring of gas and dust has been accreted from outside.

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“…This galaxy has two perpendicular and almost irregular rings, one in the equatorial and one in the polar plane, surrounding a central nearly spherical galaxy. Reshetnikov et al () found very blue optical colours for the rings, typical of late‐type spirals. Moreover, since both rings rotate around the central galaxy (Whitmore et al ; Reshetnikov et al ), they conclude that ESO 474−G26 can be classified as a kinematically confirmed PRG.…”

Section: Introductionmentioning

confidence: 98%

“…Reshetnikov et al (), analysing the luminosity profiles of ESO 474−G26 in the optical bands, were able to distinguish three components: (i) the main central body with almost round isophotes ( b / a ∼ 0.94), (ii) a narrow ring with a diameter of ≃37 arcsec = 37 kpc in the equatorial plane and (iii) a second (larger) polar ring with a diameter of ≃58 arcsec = 58 kpc in the polar plane. Both rings are very irregular.…”

Section: Introductionmentioning

confidence: 99%

A new photometric investigation of the double-ringed galaxy ESO 474−G26: unveiling the formation scenario

Spavone¹,

Iodice

Bettoni

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present a detailed photometric study of the peculiar double-ringed galaxy ESO 474-G26. Near-infrared (NIR) and optical data have been used, with the main goal of constraining the formation history of ESO 474-G26. NIR photometry is fundamental in this kind of study, because it gives better constraints on the spectral energy distribution (SED) and traces the older stellar population of the galaxy well. This galaxy presents a very complex structure with two almost orthogonal rings, one in the equatorial and another in the polar plane, around an elliptical-like object. Due to the peculiar morphology of ESO 474-G26, we used both NIR images (J and K bands) to derive accurate analysis of the stellar light distribution and optical images (in the B, V and R bands) to derive colour profiles and colour maps to study the structure of the rings. The observational characteristics of ESO 474-G26 are typical of galaxies that have experienced some kind of interaction during their evolution. We investigated two alternatives: a merging process and an accretion event

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Galaxy transmutations: The double ringed galaxy ESO 474-G26

Cited by 11 publications

References 25 publications

A minor merger origin for stellar inner discs and rings in spiral galaxies

A minor merger origin for stellar inner discs and rings in spiral galaxies

Revisiting the formation history of the minor-axis dust lane galaxy NGC 1947

A new photometric investigation of the double-ringed galaxy ESO 474−G26: unveiling the formation scenario

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