Quantitative Morphology of Bars in Spiral Galaxies

Martin, Pierre

doi:10.1086/117461

Cited by 196 publications

(311 citation statements)

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“…The ratio of a bar length to a disk scale length or size tends to decrease from early-type to late-type barred galaxies, which is also pointed out by Martin (1995); the ratio is about three times larger in early-type barred galaxies than in late-type barred galaxies. The bar length also correlates with a bulge size (Athanassoula & Martinet 1980).…”

Section: Bar Lengthsupporting

confidence: 55%

Global Photometric Properties of Barred Galaxies

Ohta

1996

International Astronomical Union Colloquium

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Section: Bar Lengthsupporting

confidence: 55%

Global Photometric Properties of Barred Galaxies

Ohta

1996

International Astronomical Union Colloquium

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“…Secular accumulation or satellite accretion of only 1-3% of the total stellar disk mass near the center is su cient to induce dissolution of the bar into a lens or triaxial component and later into a spheroid (Kormendy 1982, Pfenniger & Norman 1990, P93, Friedli 1994, M95, Norman, Sellwood, & Hasan 1996. It is estimated that about two-thirds of disk galaxies currently have a bar, especially as revealed in the infrared (Block & Wainscoat 1991, Zaritzky, Rix & Rieke 1993, Sellwood & Wilkinson 1993, Martin 1995 and that most spirals have probably harbored a self-destructive bar at one time or another during their evolution (Friedli & Benz 1993, hereafter FB93;Friedli et al 1994). Once a bar has formed, thickened and subsequently dissolved, no more thickening of the central dissipationless material is expected unless triggered by starbust activity or stellar accretion.…”

Section: An Overview Of Secular Evolutionmentioning

confidence: 99%

The Bulge/Disk Connection in Late-Type Spirals

Courteau

1996

New Extragalactic Perspectives in the New South Africa

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Abstract.Recent ground-based photometric investigations suggest that central regions of late-type spirals are closely coupled to the inner disk and probably formed via secular evolution. Evidence presented in support of this model includes the predominance of exponential bulges, the correlation of bulge and disk scale lengths, blueness of the bulge and small di erences between bulge and central disk colors, detection of spiral structure into the core, and rapid rotation. Recent HST observations show that our own bulge and that of M31, M32, and M33 probably harbor both an old and intermediateage populations in agreement with models of early collapse of the spheroid plus gas transfer from the disk. Secular evolution provides a mechanism to build-up central regions in late-type spirals; mergers or accretion of small satellites could explain the brighter, kinematically distinct bulges of Sa's and SO's.

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“…Visual inspection of galaxy images (e.g. Martin 1995), ellipse fitting of the isophotes by locating the maximum in the ellipticity profile (e.g. Wozniak & Pierce 1991) or by looking for variations of the position angle (e.g.…”

Section: Introductionmentioning

confidence: 99%

On the morphology of dust lanes in galactic bars

Sánchez-Menguiano¹,

Pérez²,

Zurita³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The aim of our study is to use dynamical simulations to explore the influence of two important dynamical bar parameters, bar strength and bar pattern speed, on the shape of the bar dust lanes. To quantify the shape of the dust lanes we have developed a new systematic method to measure the dust lane curvature. Previous numerical simulations have compared the curvature of bar dust lanes with the bar strength, predicting a relation between both parameters which has been supported by observational studies but with a large spread. We take into account the bar pattern speed to explore, simultaneously, the effect of both parameters on the dust lane shape.To that end, we separate our galactic bars in fast bars (1 < R < 1.4) and slow bars (R > 1.4), obtaining, as previous simulations, an inverse relation between the dust lane curvature and the bar strength for fast bars. For the first time, we extend the study to slow bars, finding a constant curvature as a function of the bar strength. As a result, we conclude that weak bars with straight dust lanes are candidates for slow bars. Finally, we have analysed a pilot sample of ten S 4 G galaxies, obtaining dust lane curvatures lying within the range covered by the simulations.

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Quantitative Morphology of Bars in Spiral Galaxies

Cited by 196 publications

References 0 publications

Global Photometric Properties of Barred Galaxies

Global Photometric Properties of Barred Galaxies

The Bulge/Disk Connection in Late-Type Spirals

On the morphology of dust lanes in galactic bars

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