Close encounter between galaxies – II. Tidal deformation of a disc galaxy stabilized by massive halo

Noguchi, Masafumi

doi:10.1093/mnras/228.3.635

Cited by 222 publications

(202 citation statements)

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“…Quantitatively, we find that these interactions are quite weak and, based on numerical simulations, may not be able to trigger bar formation (Salo 1991). On the other hand these systems fit into the scenario proposed by Noguchi (1987) that the interaction of two gaseous systems first leads to bar formation and then to the formation of an amorphous galaxy. Few conclusions can be reached until these data can be compared with more appropriate numerical simulations (i.e.…”

Section: Discussion: the Interactionssupporting

confidence: 61%

“…The major question this raises is whether or not the interactions with these HI clouds are the cause of the barred morphology and kinematics in 128 Wilcots, Lehman, and Miller these galaxies. There is an increasing amount of evidence both observational and numerical that barred structure in galaxies is related to gravitational interactions with their neighbors (Elmegreen et al 1990;Noguchi 1987Noguchi , 1988Gerin et al 1990;Salo 1991;Odewahn 1994). Quantitatively, we find that these interactions are quite weak and, based on numerical simulations, may not be able to trigger bar formation (Salo 1991).…”

Section: Discussion: the Interactionsmentioning

confidence: 61%

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HI Observations of Barred Magellanic Type Galaxies

Wilcots

Lehman

Miller³

1996

International Astronomical Union Colloquium

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Abstract.We present the results of a VLA D-configuration survey of a sample of Barred Magellanic type (SBm/IBm) galaxies. The data show that: (1) the HI is extended well beyond the optical diameter; (2) the HI distribution often has a different position angle than the optical distribution; (3) the bar morphology is typically manifested in the HI kinematics; (4) these galaxies not only tend to have gaseous companions, but they also tend to be strongly interacting systems; and (5) the companions have no obvious optical counterparts.

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Section: Discussion: the Interactionssupporting

confidence: 61%

Section: Discussion: the Interactionsmentioning

confidence: 61%

HI Observations of Barred Magellanic Type Galaxies

Wilcots

Lehman

Miller³

1996

International Astronomical Union Colloquium

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“…NGC 1792 and ESO 362-019 have a bulge-less flocculent appearance, while NGC 1808 has an outer ring-like structure and an extended multiple-arms structure. None of galaxies show unambiguous morphological distorsions due to interaction, while most of them show outer asymmetric structures and bars which are often associated to past interactions events (see simulations of Noguchi 1987).…”

Section: Uv Morphologymentioning

confidence: 87%

Galaxy evolution in Local Group analogs

Marino

Bianchi

Rampazzo

et al. 2010

A&A

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Context. Understanding the astrophysical processes acting within galaxy groups and their effects on the evolution of the galaxy population is one of the crucial topics of modern cosmology, as almost 60% of galaxies in the Local Universe are found in groups. Aims. We aim at learning about galaxy evolution within nearby groups dominated by late-type galaxies, specifically by studying their ultraviolet-emitting stellar population. Methods. We imaged in the far (FUV, λ eff = 1539 Å) and near ultraviolet (NUV, λ eff = 2316 Å) with the Galaxy Evolution Explorer (GALEX) three nearby groups, namely LGG 93, LGG 127 and LGG 225. We obtained the UV galaxy surface photometry and, for LGG 225, the only group covered by the SDSS, the photometry in u, g, r, i, z bands. We discuss galaxy morphologies looking for interaction signatures and we analyze the spectral energy distribution of galaxies to infer their luminosity-weighted ages. The UV and optical photometry was also used to perform a luminosity-weighted kinematical and dynamical analysis of each group and to evaluate the stellar mass. Results. A few member galaxies in LGG 225 show a distorted UV morphology due to ongoing interactions. (FUV − NUV) colors suggest that spirals in LGG 93 and LGG 225 host stellar populations in their outskirts younger than that of M 31 and M 33 in the Local Group or with less extinction. The irregular interacting galaxy NGC 3447A has a significantly younger stellar population (a few Myr old) than the average of the other irregular galaxies in LGG 225 suggesting that the encounter triggered star formation. The early-type members of LGG 225, NGC 3457 and NGC 3522, have masses of the order of a few 10 9 M , comparable to the Local Group ellipticals. For the most massive spiral in LGG 225, we estimate a stellar mass of ≈4 × 10 10 M , comparable to M 33 in the Local Group. Ages of stellar populations range from a few to ≈7 Gyr for the galaxies in LGG 225. The kinematical and dynamical analysis indicates that LGG 127 and LGG 225 are in a pre-virial collapse phase, i.e. still undergoing dynamical relaxation, while LGG 93 is likely virialized. Both the photometric and the dynamical analyses suggest that LGG 225 is in a more active evolution phase than LGG 93 and LGG 127.

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“…Tidal triggering can induce a bar in a galaxy that is stable when isolated (e.g., Noguchi 1987). Such bars would be strongly braked if the target galaxy had been stabilized by a massive halo.…”

Section: General Implicationsmentioning

confidence: 99%

Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

Debattista

Sellwood

2000

ApJ

527

631

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We show that bars in galaxy models having halos of moderate density and a variety of velocity distributions all experience a strong drag from dynamical friction unless the halo has large angular momentum in the same sense as the disk. The frictional drag decreases the bar pattern speed, driving the corotation point out to distances well in excess of those estimated in barred galaxies. The halo angular momentum required to avoid strong braking is unrealistically large, even when rotation is conÐned to the inner halo only. We conclude, therefore, that bars are able to maintain their observed high pattern speeds only if the halo has a central density low enough for the disk to provide most of the central attraction in the inner galaxy. We present evidence that this conclusion holds for all bright galaxies.

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Close encounter between galaxies – II. Tidal deformation of a disc galaxy stabilized by massive halo

Cited by 222 publications

References 0 publications

HI Observations of Barred Magellanic Type Galaxies

HI Observations of Barred Magellanic Type Galaxies

Galaxy evolution in Local Group analogs

Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

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