Do Bars Trigger Activity in Galactic Nuclei?

Lee, Gwang-Ho; Woo, Jong-Hak; Lee, Myung Gyoon; Hwang, Ho Seong; Lee, Jong Chul; Sohn, Jubee

doi:10.1088/0004-637x/750/2/141

Cited by 59 publications

(56 citation statements)

References 137 publications

(181 reference statements)

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“…This finding may indicate that tidal interactions destroy and/or disfavor bar growth instead of enhancing it as expected from results of numerical simulations. As weak bars are more commonly found in fainter, less-massive galaxies than strong bars (Lee et al 2012b; Cervantes-Sodi et al 2013), the fact that we find the effect of nearby companions at larger scales for the case of weak bars may be not unexpected. Due to the low mass of galaxies hosting weak bars, their gravitational potential is also weaker and they are more fragile to disturbances than their more massive counterparts.…”

Section: Summary and Discussionsupporting

confidence: 63%

“…The large number of strongly barred galaxies in our sample helps to improve the statistics and reduce the statistical errors in our measurements, but even with large error bars, if we look at the result for weakly barred galaxies, we see that the drop of average neighbor counts is noticeable at even larger scales, up to a few hundred kiloparsecs. A possible explanation for this effect at larger scales for the case of weakly barred galaxies might be related with these systems being less massive than those galaxies hosting strong bars (Lee et al 2012b;Cervantes-Sodi et al 2013), which would make them less stable against interactions with massive neighbors even at large separations.…”

Section: Close Neighbor Countsmentioning

confidence: 99%

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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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Section: Summary and Discussionsupporting

confidence: 63%

Section: Close Neighbor Countsmentioning

confidence: 99%

The Environment of Barred Galaxies in the Low-Redshift Universe

Lin

Sodi

et al. 2014

ApJ

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“…Laine et al 2002). However, Lee et al (2012b) found that no significant difference in bar fraction between active and inactive galaxies can be observed if one compares samples of galaxies that are matched in mass, color, etc.…”

Section: Morphologymentioning

confidence: 97%

“…Observations of the remaining 53 galaxies of the LLQSO sample might be useful to ensure the statistical significance. Lee et al (2012b) analyzed a volume-limited sample of SDSS galaxies with 0.01 < z < 0.05, M r < −20.3 and M * > 10 10 M , similar to our sample. They found a bar-fraction of 41.4% at optical wavelengths.…”

Section: Morphologymentioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Zuther

Valencia-S.

et al. 2014

A&A

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Recognizing the properties of the host galaxies of quasi-stellar objects (QSOs) is essential for understanding the suspected coevolution of central supermassive black holes (BHs) and their host galaxies. Low-luminosity type-1 QSOs (LLQSOs) are ideal targets because of their small cosmological distance, which allows for a detailed structural analysis. We selected a subsample of the Hamburg/ESO survey for bright UV-excess QSOs that contains only the 99 nearest QSOs with redshift z ≤ 0.06. From this LLQSO sample, we observed 20 galaxies and performed aperture photometry and bulge-disk-decomposition with BUDDA on near-infrared J-, H-, and K-band images to separate disk, bulge, bar, and nuclear component. From the photometric decomposition of these 20 objects and visual inspection of images of another 26, we find that ∼50% of the hosts are disk galaxies and most of them (86%) are barred. Stellar masses, calculated from parametric models based on inactive galaxy colors, range from 2 × 10 9 M to 2 × 10 11 M with an average mass of 7 × 10 10 M . Black hole masses measured from single-epoch spectroscopy range from 1 × 10 6 M to 5 × 10 8 M with a median mass of 3 × 10 7 M . In comparison with higher-luminosity QSO samples, LLQSOs tend to have lower stellar and BH masses. Moreover, in the effective radius vs. mean surface-brightness projection of the fundamental plane, they lie in the transition area between luminous QSOs and normal galaxies. This can be seen as additional evidence that they populate a region intermediate between the local Seyfert population and luminous QSOs at higher redshift. This region has not been well studied so far. Eleven LLQSOs, for which we have reliable morphological decompositions and BH mass estimations, lie below the published BH mass vs. bulge luminosity relations for inactive galaxies. This can partially be explained if one assumes that the bulges of active galaxies contain much younger stellar populations than the bulges of inactive galaxies. Another possibility would be that their BHs are undermassive. This might indicate that the growth of the host spheroid precedes that of the BH.

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“…These shocks are tracing the channels by which the gas flows towards the galaxy centres where it can contribute to the central mass concentration, for example producing star formation, pseudo-bulges formation or AGN activity (e.g. Shlosman, Frank & Begelman 1989;Oh, Oh & Yi 2012;Wang et al 2012;Lee et al 2012). …”

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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Do Bars Trigger Activity in Galactic Nuclei?

Cited by 59 publications

References 137 publications

The Environment of Barred Galaxies in the Low-Redshift Universe

The Environment of Barred Galaxies in the Low-Redshift Universe

A low-luminosity type-1 QSO sample

On the morphology of dust lanes in galactic bars

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