Dynamical Properties of Tidally Induced Galactic Bars

Miwa, T.; Noguchi, Masafumi

doi:10.1086/305611

Cited by 119 publications

(144 citation statements)

References 44 publications

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“…Although our images are moderately deep, the S/N ratio becomes low at outer isophotes and therefore we terminate the plot at ∼30 arcsec for the two smaller galaxies. become increasingly subtle, passing from stellar shells and ripples to possibly tidal bars (Miwa & Noguchi 1998) or boxy isophotes (see Barnes & Hernquist 1992). If the galaxies we observe as starbursting transition dwarfs formed via near equal mass mergers, then these events were in the distant past or involved a companion with very few stars.…”

Section: Dwarf-galaxy Fine-structure Featuresmentioning

confidence: 92%

Deep Optical Imaging of Starbursting “Transition” Dwarf Galaxies

Dellenbusch

Gallagher

Knezek³

et al. 2007

The Astronomical Journal

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A subgroup of dwarf galaxies have characteristics of a possible evolutionary transition between star-forming systems and dwarf ellipticals. These systems host significant starbursts in combination with smooth, elliptical outer envelopes, and small H i content; they are low on gas and unlikely to sustain high star-formation rates over significant cosmic time spans. We explore possible origins of such starburst "transition" dwarfs using moderately deep optical images. While galaxy-galaxy interactions could produce these galaxies, no optical evidence exists for tidal debris or other outer disturbances, and they also lack nearby giant neighbors which could supply recent perturbations. Colors of the outer regions indicate that star formation ceased >1 Gyr in the past, a longer time span than can be reasonably associated with the current starbursts. We consider mechanisms where the starbursts are tied either to interactions with other dwarfs or to the state of the interstellar medium, and discuss the possibility of episodic star-formation events associated with gas heating and cooling in low specific angular-momentum galaxies.

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Section: Dwarf-galaxy Fine-structure Featuresmentioning

confidence: 92%

Deep Optical Imaging of Starbursting “Transition” Dwarf Galaxies

Dellenbusch

Gallagher

Knezek³

et al. 2007

The Astronomical Journal

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“…Similar results are reported by Byrd & Valtonen (1990) for the case of tidal forces exerted by a cluster potential on simulated disk galaxies. Although the configuration of the interaction changes the final properties of the bar, some groups found that in general, it enhances the formation of the bar (Gerin et al 1990;Miwa & Noguchi 1998), while others report that the opposite is also possible: the bar can loose angular momentum and mass and debilitate after the interaction (Sundin & Sundelius 1991;Sundin et al 1993). There seem to be also controversy about the different effects of prograde and retrograde interactions (Romano-Díaz et al 2008;Aguerri & González-García 2009).…”

Section: Introductionmentioning

confidence: 99%

The Environment of Barred Galaxies in the Low-Redshift Universe

Lin

Sodi

et al. 2014

ApJ

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We present a study of the environment of barred galaxies using a volume-limited sample of over 30,000 galaxies drawn from the Sloan Digital Sky Survey. We use four different statistics to quantify the environment: the projected two-point cross-correlation function, the background-subtracted number count of neighbor galaxies, the overdensity of the local environment, and the membership of our galaxies to galaxy groups to segregate central and satellite systems. For barred galaxies as a whole, we find a very weak difference in all the quantities compared to unbarred galaxies of the control sample. When we split our sample into early-and late-type galaxies, we see a weak but significant trend for early-type galaxies with a bar to be more strongly clustered on scales from a few 100 kpc to 1 Mpc when compared to unbarred early-type galaxies. This indicates that the presence of a bar in early-type galaxies depends on the location within their host dark matter halos. This is confirmed by the group catalog in the sense that for early-types, the fraction of central galaxies is smaller if they have a bar. For late-type galaxies, we find fewer neighbors within ∼50 kpc around the barred galaxies when compared to unbarred galaxies from the control sample, suggesting that tidal forces from close companions suppress the formation/growth of bars. Finally, we find no obvious correlation between overdensity and the bars in our sample, showing that galactic bars are not obviously linked to the large-scale structure of the universe.

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“…The thickness of a stellar disk is an important physical parameter which can help to specify dynamical evolution of the galaxy: interactions with other galaxies such as gravitational tides or merging with smaller satellites, can "heat" the disks (e.g. [1,2]), making them thicker, while smooth, laminar accretion of a large amount of cool gas with subsequent star formation and the development of young stellar systems that are dynamically cool like the gas from which they form, can reduce the thickness of the disk [3].…”

Section: Introductionmentioning

confidence: 99%

The thickness of stellar disks in early-type galaxies

Chudakova¹,

Сильченко

2014

Astron. Rep.

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We suggest and verify a new photometric method enabling derivation of relative thickness of a galactic disk from two-dimensional surface-brightness distribution of the galaxy in the plane of the sky. The method is applied to images of 45 early-type (S0-Sb) galaxies with known radial exponential or doubleexponential (with a flatter outer profile) surface-brightness distributions. The data in the r-band have been retrieved from the SDSS archive. Statistics of the estimated relative thicknesses of the stellar disks of early-type disk galaxies show the following features. The disks of lenticular and early-type spiral galaxies have similar thicknesses. The presence of a bar results in only a slight marginal increase of the thickness. However, we have found a substantial difference between the thicknesses of the disks with a single-scaled exponential brightness profile and the disks that represent the inner segments of the Type III (antitruncated) profiles. The disks are significantly thicker in the former subsample than in the latter one. This may provide evidence for a surface-brightness distribution of a single-scaled exponential disk to be formed due to viscosity effects acting over the entire period of star formation in the disk.

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Dynamical Properties of Tidally Induced Galactic Bars

Cited by 119 publications

References 44 publications

Deep Optical Imaging of Starbursting “Transition” Dwarf Galaxies

Deep Optical Imaging of Starbursting “Transition” Dwarf Galaxies

The Environment of Barred Galaxies in the Low-Redshift Universe

The thickness of stellar disks in early-type galaxies

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