Numerical simulations of interacting gas-rich barred galaxies: vertical impact of small companions

Berentzen, I.; Athanassoula, E.; Heller, Clayton; Fricke, K. J.

doi:10.1046/j.1365-8711.2003.06417.x

Cited by 60 publications

(64 citation statements)

References 58 publications

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“…In this case the central mass component evolves to an axisymmetric bulge instead of forming a real bar. Some dynamical models (Berentzen et al 2003) also predict that galaxy interactions might accelerate the transition from a strongly barred galaxy to a weakly or nonbarred galaxy.…”

Section: Discussionmentioning

confidence: 99%

Comparison of Bar Strengths and Fractions of Bars in Active and Nonactive Galaxies

Laurikainen

Salo

Buta

2004

ApJ

144

175

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Gravitational perturbation strengths and bar fractions in active and nonactive galaxies are compared using the Ohio State University Bright Galaxy Survey, which forms a statistically well defined sample of 180 disk galaxies. Bar fractions are studied using (1) the optical and near-IR classification of bars made by Eskridge and coworkers in 2002 and (2) our own bar classification based on Fourier decomposition of near-IR images (Fourier bars). The gravitational perturbation strengths are calculated using the bar torque method, taking the maximum ratio Q g of the tangential force to the mean background radial force as a measure of the nonaxisymmetric perturbation. In addition, two-dimensional bulge-disk-bar decomposition is used to study the properties of bulges of the sample galaxies. In the near-IR, Seyfert galaxies, LINERs, and H ii/starburst galaxies were found to have a similar fraction, 72%, of Fourier bars (or SB-type bars), compared to 55% in the nonactive galaxies. However, if SABtype bars are also included, practically all (95%) H ii/starburst galaxies have bars. In addition, a large fraction (34%) of bars in LINERs are obscured by dust in the optical region. We find that bars in early-type galaxies are at the same time long and massive and have weak perturbation strengths. Weak perturbation strengths can be explained by dilution of the nonaxisymmetric forces by the massive bulges: for a bulge-to-disk mass ratio B=D ranging from 0 to 1, the dilution may reduce Q g from as high as 0.6 to as low as 0.1. On the other hand, bar length (relative to disk scale length) is not correlated with B=D, contrary to expectation. Seyfert-or LINER-type nuclear activity is present in most galaxies that have thin and thick planar bar components, whereas nuclear activity does not appear in those late-type galaxies that have extremely massive bars and strong perturbation strengths.

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Section: Discussionmentioning

confidence: 99%

Comparison of Bar Strengths and Fractions of Bars in Active and Nonactive Galaxies

Laurikainen

Salo

Buta

2004

ApJ

144

175

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“…However, there is the possibility that former bars (which are now dissolved) could be responsible for the boxy structure of the TBBs. It is known that bars can be destroyed by large gas inflow and mass accumulation in the center (Hasan et al 1993;Friedli & Benz 1993;Norman et al 1996;Sellwood & Moore 1999;Bournaud & Combes 2002;Berentzen et al 2003) and boxy bulges arise progressively at the end of the bar life-time (Combes 2003). On the other side, recent studies show that bars are more robust against central mass concentration than previously thought (Shen & Sellwood 2003).…”

Section: Discussionmentioning

confidence: 99%

Box- and peanut-shaped bulges

Lütticke

Pohlen

Dettmar

2004

A&A

127

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Abstract. Inspecting all 1224 edge-on disk galaxies larger than 2 in the RC3 on Digitized Sky Survey (DSS) images (Lütticke et al. 2000a) we have found several galaxies with extraordinary bulges meeting two criteria: they are box shaped and large in respect to the diameters of their galaxies. These bulges are often disturbed, show frequently prominent irregularities and asymmetries, and some possess possible merger remnants or merging satellites. For these bulges we have introduced the term "Thick Boxy Bulges" (TBBs). About 2% of all disk galaxies (S0-Sd), respectively 4% of all galaxies with box-and peanut-shaped (b/p) bulges, belong to this class of galaxies. Using multicolour CCD and NIR data we have enlarged and followed up our sample of nearly 20 galaxies with a TBB. The disturbed morphology of a large fraction of these galaxies shows that many of the TBB galaxies are not dynamically settled. For the TBBs the extent of the box shape seems to be too large to result from a normal bar potential. Therefore we conclude that two classes of b/p bulges exist with different origins. While most (∼96%) b/p bulges can be explained by bars alone (Lütticke et al. 2000b), the extended boxy structures of TBBs result most likely from accreted material by infalling satellite companions (soft merging).

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“…Second, in numerical simulations, the vertical impact of small companions can cause asymmetries in gas-rich barred galaxies (Berentzen et al 2003). Walker et al (1996) found that a minor merger can form significant disk asymmetry that is visible for at least 1 Gyr.…”

Section: Minor Merger Event In Ngc 7479mentioning

confidence: 99%

“…In addition, the evolution of stellar bars may relate to minor mergers in numerical simulations (Berentzen et al 2003;Romano-Díaz et al 2008). However, these correlations still need to be studied further.…”

Section: Introductionmentioning

confidence: 99%

Star Formation Properties in Barred Galaxies (Sfb). I. Ultraviolet to Infrared Imaging and Spectroscopic Studies of NGC 7479

Zhang

Cao

Meng

et al. 2011

The Astronomical Journal

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Large-scale bars and minor mergers are important drivers for the secular evolution of galaxies. Based on ground-based optical images and spectra as well as ultraviolet data from the Galaxy Evolution Explorer and infrared data from the Spitzer Space Telescope, we present a multi-wavelength study of star formation properties in the barred galaxy NGC 7479, which also has obvious features of a minor merger. Using various tracers of star formation, we find that under the effects of both a stellar bar and a minor merger, star formation activity mainly takes place along the galactic bar and arms, while the star formation rate changes from the bar to the disk. With the help of spectral synthesis, we find that strong star formation took place in the bar region about 100 Myr ago, and the stellar bar might have been ∼10 Gyr old. By comparing our results with the secular evolutionary scenario from Jogee et al., we suggest that NGC 7479 is possibly in a transitional stage of secular evolution at present, and it may eventually become an earlier type galaxy or a luminous infrared galaxy. We also note that the probable minor merger event happened recently in NGC 7479, and we find two candidates for minor merger remnants.

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Numerical simulations of interacting gas-rich barred galaxies: vertical impact of small companions

Cited by 60 publications

References 58 publications

Comparison of Bar Strengths and Fractions of Bars in Active and Nonactive Galaxies

Comparison of Bar Strengths and Fractions of Bars in Active and Nonactive Galaxies

Box- and peanut-shaped bulges

Star Formation Properties in Barred Galaxies (Sfb). I. Ultraviolet to Infrared Imaging and Spectroscopic Studies of NGC 7479

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